At the wavelength around 4.6 μm for Perseus 1 and 3, RNO 91, and AFGL 7009S, there is a hint for another ice component overlapping with the CO absorption feature at 4.67 μm. Many near-infrared observations have revealed the same feature on the blue wing part of the CO absorption feature


which was suggested as an absorption feature of XCN ice.


Despite the observational evidence, and to keep alive the inherited model,


proposed to decrease the theoretical 60Fe abundance in molecular clouds by assuming that stars more massive than 30 M⊙ do not explode as SNe. These stars would not contribute to the 60Fe inventory, bringing the theoretical ISM 60Fe/26Al ratio closer to that of the solar system. Because stars more massive than 30 M⊙ contribute to less than 50% of the 60Fe production2, this proposition cannot resolve the two orders of magnitude discrepancy between the model and observations.


The orbital phase is calculated using the TEMPO2 package


Although a cavity of 55 astronomical units (au) in radius has been inferred from dust millimeter emission


infrared polarized intensity observations have found no clear evidence for a cavity in scattered light


For the other lines in the 10 − 36 μm interval,


did not report a detection, and we used the data presented in Bernard-Salas et al. (2009) for a total of 15 objects.


can inject strong energy inputs in the primeval universe (e.g.,


covering a wide metallicity range were re-reduced and analysed with our code to ensure that our EWs measurements are on the same scale as the template clusters used to define the metallicity calibration.


These processes have been studied both by investigating normal modes of the inhomogeneous structure


One striking problem is the ${\rm ^{14}N}/{\rm ^{15}N}$ isotopic ratio of nitrogen in comets. Its average value, 144 ± 3


, is three times lower than the bulk ratio of 441 ± 6 in the protosun as inferred from solar wind measurements


The reasons for these different ratios remain elusive, casting doubts on our understanding of the origin of the composition of comets and more generally of the origin of nitrogen in the Solar system.


Over the entire mission, the deceleration of the solar wind using the mean speed of the particles is much more limited than the deceleration shown by the norm of the bulk velocity


: there is more kinetic energy in the solar wind than the bulk velocity vector would let us think.


At small scales (a few tens of kpc), there is substantial evidence from observations and simulations for a decrement of metallicity and an enhancement of star-formation activity in galaxy close pairs, merging, and interacting systems compared to isolated, field galaxies, mostly attributed to the interaction-induced inflow of metal-poor gas from the periphery of interacting galaxies to the center, diluting their metal content, and increasing their gas fuel for star-formation


at the center is blocked by the thick dusty torus acting as the “coronograph”


this makes HzRGs true obscured type-2 quasars, allowing us to probe their host galaxies and CGM without strong AGN contamination (e.g.


This is in contrast with previous studies


where the backward modeling approach is employed to constrain the probability of mass for a given richness,


These studies are based on the hypothesis that magnetic fields are passively transported by the plasma flow and provide a characterisation of advection and diffusion processes in the quiet photosphere from granular to supergranular scales (see, e.g


These studies reveal an anomalous scaling of magnetic field transport with a superdiffusive character consistent with a Levy walk inside supergranules and a more Brownian-like motion in their boundary.


These studies pointed out the large magnetic temporal variability and the critical effect of stellar rotation and mass on magnetic field generation through dynamo mechanism, leading in some parameter regimes to configurations with cyclic activity


The Hβ BEL is considered to be rotating gas in a flat “pancake-like” region in which the normal to the BEL disk is parallel to the jet axis


Thus, the FWHM that appears in Equation (4) depends on the LOS.


This method has since identified a large number across the extragalactic sky, i.e., more than 100 lensed candidates at z > 1


have shown H2O emission to be ubiquitous with intensities as bright as CO lines.


Such high-precision RV surveys include those being undertaken currently with


We estimated the precession period using the theory from Terquem et al. (1999) and the binary parameters taken from


– Mh = 0.8M⊙ (the mass of the hot WD companion), Mp∕Mh = 1.65 (where Mp is the mass of the primary companion), D = 15.5 AU (the mean semi-major axis of the system), and e = 0.25 (eccentricity).


Driven by dynamical friction and global torques from this disc, the pair of MBHs decays very efficiently down to separations of the order of ∼1–0.1 pc, where it forms a gravitationally bound binary


and the kilonova AT 2017gfo in the ultraviolet–optical–infrared band


as well as the combination of the H2O-K2 index with pEWs to derive [Fe/H]


These have revealed a surprising diversity in the orbital alignments (for example


which is in contrast to the Laplacian ideals of planets forming inside a flat disk, coplanar with the stellar equator and staying there


The tilt angle compared to a completely edge-on orientation was suggested to be 3° in the model of Hogerheijde et al. (1995) and


A tilt angle of 3° is equivalent to an enhancement factor of 20 for the measured column densities.


The Largest Linear Sizes (LLS) and radio powers of relics are correlated, as well as the integrated spectral index and the radio power


An alternative and attractive pathway for seed BH formation is via the so-called direct collapse


where a supermassive star (SMS) with ${\sim } 10^{5}\, \mathrm{M}_{\odot }$ collapses into a BH with a similar mass by general relativistic instability


Both kinds of event are too common to be entirely explained with PPI+CC progenitors, and it is likely that both classes contain events with a diversity of physical mechanisms (e.g.,


The task of estimating stellar ages has been addressed by several authors and lots of different methods are found in the literature. For instance, there are (i) empirical methods, which use a deterministic relation between a given parameter and the age of a star (first proposed by Skumanich 1972). This is the case of


Adopting an expansion velocity equal to half the velocity interval where the structure is observed, Vexp = 7.0 ± 1.3 km s− 1 , the molecular mass given in Table 1 and the atomic and ionized masses estimated by


1450 and 3000 M⊙, respectively, we obtain Ekin = (2.5 ± 1.0) × 1049 erg, assuming a 40 per cent error for the masses.


performed SPH (smoothed particle hydrodynamics) simulations and studied water loss in planetary embryos and water retained in significant fragments after a collision. They concluded that the impact velocity and the impact angle play a key role in the water loss of a planetary embryo after a collision.


We leave a more detailed investigation of this change to future work. Here, we simply mention two possible explanations: The change in slope may be a reflection of the differences in the dynamical state (e.g. mass-to-light ratio; M/L) at the outskirts of BCGs


Among the four s-process elements mentioned above, GES provides the abundances of Y II (the first s-process peak element) and Ba II (the second s-process peak element) for all our sample stars. Their abundances behave differently in the Galactic thick and thin discs


In the presence of molecular clouds surrounding the SNR, escaping CRs can illuminate the clouds through pp interactions, producing gamma-ray emission with a flux depending on the amount of nuclear CRs released by an SNR and the diffusion coefficient in the interstellar medium (ISM;


By default, these techniques are applicable only to single-frequency sky images: even for multiwavelength observatories such as the Herschel Space Observatory


the standard detection pipelines have produced individual source catalogs for each frequency band (see e.g.,


The next logical step is to boost the signal of faint sources by combining the different bands into a single detection, that is, “multifrequency detection”.


The derived N(H i) is an order of magnitude less than a typical value through a disk of a spiral galaxy with stellar mass >1010 M⊙, measured by The H i Nearby Galaxy Survey (THINGS


Open clusters are a valuable alternative, being on average younger


and therefore a better tracer of the gradients in the disc out of which the most recent stars formed.


While tides on the progenitor of the second-born black hole can spin up the progenitor star


this effect can be counteracted by mass loss in stellar winds, and more detailed simulations find only low or moderate spin increases due to tides


It is particularly important to understand if cluster mergers


or, alternatively, if they have no direct effect (e.g.


The possible presence of dust in the habitable zones of nearby main-sequence stars is considered a major threat for the direct imaging and characterization of Earth-like extrasolar planets (exo-Earths) with future dedicated space-based telescopes. Several independent studies have addressed this issue and concluded that visible to mid-infrared direct detection of exo-Earths would be seriously hampered in the presence of dust disks 10 to 20Â times brighter than the solar zodiacal cloud assuming a smooth brightness distribution (e.g.,


so it could be a universal model for NS-LMXBs.


The overall incidence rate of magnetic upper main sequence stars in close binaries is less than 2 per cent


although this fraction is significantly higher if one includes wide long-period systems


The patchy beam scenario is one of the common beam models that has been used to explain the emission properties of pulsars (see


Previous studies showed that WL masses obtained from the tangential shear fitting were biased low up to 10 per cent with a scatter of ∼25 per cent


The main source of the bias are due to substructures and triaxiality. When a cluster whose major axis is perpendicular to the line of sight, i.e elongated in the sky-plane, a mass obtained with the spherical NFW profile is typically underestimated.


Observations indicate that the abundance of SiO does not differ significantly between envelopes around M-, S-, and C-type stars, although in all them the SiO abundance decreases with increasing mass-loss rate


IRAS 16293-2422 (hereafter IRAS 16293) was chosen for this work as the quintessential example of such an object. IRAS 16293 is adequate for this role because formaldehyde has previously been detected with notable variations in abundances in three differentiated regions of its protodisk


Being associated with old stellar populations, they represent the basis of an alternative Population II distance scale


more suitable to calibrate secondary distance indicators that are not specifically associated with spiral galaxies (e.g. the globular cluster luminosity function, see


The difference between the Saro et al. (2013) and


galaxy scaling relations depends on the details of the semi-analytic and hydrodynamical implementations used in Saro et al. (2013) and


Still several schemes have been developed to define groups within galaxy catalogues. They mainly invoke Friends of Friends (FoF) like algorithms based on projected separation, radial velocities and even luminosities to identify what are called ‘groups’ of galaxies (e.g.


Possibly the material is accelerated by radiation pressure


but alternatively the high-speed cool gas may be due rapid radiative cooling in some situations.


In addition, it also shows evidence of relativistic jets


Although a supermassive BH can be modeled by adding a Keplerian potential, it is much simpler to model the BH as this small Gaussian


This mechanism would lead to tori that are a few tens of parsec wide and are dynamic, evolving structures as proposed to interpret several recent observational studies and compilations (e.g.,


ROSINA observations provided evidence that this comet is formed from pristine material that has not been significantly altered after its formation in the first Myr of the solar nebula stage. The high abundance of


all indicate that comet 67P formed at low temperature and did not experience any substantial global-scale heating after its formation.


However, laboratory and theorectical studies showed that quantum tunnelling does not contribute much to the mobility of H atoms on silicate, carbonaceous or solid amorphous water (ASW) surfaces


Previous infrared spectroscopy failed to clearly detect the signatures of ongoing active star formation at the central few arcsec region of the NGC 1068 nucleus due to the lack of polycyclic aromatic hydrocarbon (PAH) emission features


which are a good probe of star formation activity


However, the proposed astrophysical pathways to mergers remain highly debated. Possible compact-object merger pathways include isolated binary evolution


individual periodic signals or continuous waves (CWs


Combining different samples from various instruments at different redshifts therefore inevitably introduces ENLR size–luminosity relations with different slopes α depending on the details of target selection and analysis approaches. Slopes ranging from


Growing indirect observational evidence suggests that magnetars could act as the central engines of both LGRBs and short-duration GRBs


Different approaches of subgrid models were explored


to mechanical feedback where the momentum boost during the unresolved adiabatic phase is calibrated through small-scale ISM simulations and injected into the ISM


Simulations of dwarf galaxies in recent years have often adopted one of these approaches for SN feedback. Although many are considered successful in reproducing observations, few attempts have been made to compare these models in full cosmological simulations. It is therefore important to gauge how the evolution of simulated dwarf galaxies (especially at the low mass end) is dependent on feedback models, in order to provide a more robust model with realistic uncertainties for future observations.


Both observations and simulations have suggested that there may be a positive trend between the mean black hole accretion rate and star-formation rate (SFR; e.g.,


However, recent observations of the pickup helium focusing cone using the Plasma and Suprathermal Ion Composition (PLASTIC


on board the Solar and Terrestrial Relations Observatory Ahead (STEREO A) spacecraft measured the peak density and determined the inflow longitude to be


After first being reported in the Earth’s magnetosheath


Therefore, GRB afterglows are good probes of burst environment and the interstellar dust and gas in distant, star-forming galaxies


The determination of the magnetic configuration is also based on a method proposed by Chen et al. (2014), i.e., those filaments that follow Martin's Rule


are of the inverse-polarity type, and those that disobey Martin's Rule are of the normal-polarity type.


Complementing these observations, the spectroscopic confirmation


of over a dozen sources has seen impressive advances with ground-based spectroscopy (e.g., probing the rest-frame UV and FIR with Keck/MOSFIRE, VLT/X-Shooter, and ALMA), particularly for the brightest and rarest objects.


and $\mathcal {G}(z) = g(z)/g_0$, with g(z) as the growth factor at redshift z and g0 = g(z = 0) (e.g.


found a positive correlation between flux and spectral slope for a sample of bright RXTE AGN in the 2–10 keV band. This could affect the relative fluxes seen in our sample which are plotted in Fig. B.1. We have attempted to quantify this for the different detectors used in the creation of our light curves.


In response, shock acceleration transport models were developed in recent years based on the numerical solutions of the focused transport equation


to take advantage of the fact that focused transport is not restricted to small pitch-angle anisotropies.


The fit also provided a low value of electron temperature (kT) consistent with the high value of β obtained


The variability within the GRMHD models was found to be an important limitation for constraining black hole parameters, as attested by, for example, the small difference in recovered parameters between the EHT2021 and EHT2021+ arrays. The analysis pipeline may be extended to include a characterization of the source variability as part of the model selection process (e.g.,


which could improve the constraining power beyond the averaging method introduced here.


Many other authors, in an attempt to contribute to the solution of the cuspy-core problem, performed the RC decomposition considering a constant M/L


Investigations show the layered accretion in the inner disk, where the midplane region is “dead” due to low ionization while the surface layer is “active” due to sufficient ionization


The traditional habitable zone concept assumes a planet with a functioning silicate-weathering feedback and a positive CO2 greenhouse effect


Global glaciation may be triggered on such a planet through a rapid drawdown of atmospheric CO2 that reduces q below the thresholds at which the non-Snowball states disappear.


For σ0 ≳ 2.45, the spread of η for the observed galaxies (e.g.


broadens and spans both positive and negative η values. In fact, majority of the galaxies tend to have positive ηs. This change in behaviour is well known.


Nowadays, global simulations of convective dynamos are able to reproduce cyclic magnetic fields and dynamo solutions resembling many features of the solar magnetic field evolution


Several groups have been devoted to searching for new CL-AGNs, and tens of candidates have been discovered based on large optical and X-ray surveys, such as the Sloan Digital Sky Survey (e.g.,


Note that even in longer time spans, such as from cycle 1 to 24, the sunspot number seems to vary periodically in different periods, like the often-discussed Gleissberg cycle


Radial migration of stars via cold torquing, also known as “churning,” by a bar and spiral waves


then allows for the populations to spatially overlap in the solar neighborhood.


In Fig. 11 (upper panels) we show the evolution of the spectral break measured through the DB definition


as well as the relative strength (the ratio) between the two (lower left panel).


We use the Mishima et al. (1983) formulation (see Appendix of


Examples of relics in this category are those in


A few CTTSs binaries are thought to potentially be accreting through accretion streams. These include DQ Tau


None of these stars shows the type of Hα variations seen in PTFO 8-8695 where the accretion-related emission appears to move from one side of the line profile to the other as it spirals onto one or both of the stars.


The colored rectangles represent the errors of the DEM curve, which are calculated from 100 Monte Carlo (MC) realizations of the observational data


Finally, a number density ratio (rd = n0/ne) of ∼0.02 between outside and inside of the flaring loop is determined, which is very close to the density contrast from recent observations


Quasars’ lifetimes are not long ( 0.1 Gyr,


Conventional parametric techniques correct for this effect by dividing the measured flux by a polynomial function of the coordinates of the photometric centroid; some variants may include time-dependence (e.g.,


There is another possibility of the FB formation due to the tidal disruption of stars


and the acceleration of individual particles by the arising shock waves.


At Io, the total neutral volcanic content (SO2, SO, NaCl, KCl, Cl, and dissociation products) ejected to space (Section 4.2.1) by the incident plasma is estimated to be, on average, ∼1000 kg s−1 (e.g.,


Later, numerical algorithms based on Monte Carlo techniques were developed to solve radiative transfer for more general cases. Now theoretical studies mostly rely on them (e.g.,


Allowing for the maximum value of this interval (which would imply a significant foreground galaxy halo), we recover a minimum host contribution of ${\rm DM}_{\rm host, min} \approx 60~\rm pc~cm^{-3}$. This is consistent with estimates for host galaxy contributions from theoretical and empirical treatments


Since Eggen et al. (1962) showed a model of the MW’s formation process from the kinematic analysis of halo stars in the solar neighborhood, many studies of this Galactic fossil component have been carried out using a large number of newly available halo samples, with their assembly requiring considerable observational efforts over the past decades. These include, for example,


Above the turnover, the GMC mass function has a power-law form with β ∼ 1.9, close to the observed range of β ∈ [1.6, 1.8] for clouds in the Milky Way


The rotational period of RX J1856 is P = 7 s and the X-ray pulsed fraction is the lowest among the XDINSs, ∼1.3 per cent


This anticorrelation between stellar mass and λeff is qualitatively consistent


as well as other observational evidence (e.g.


Moreover, the GR analyses with lensing and internal kinematics of both clusters indicate that the total mass profile is well fitted by the NFW model


We test in Section 2 two available one-dimensional (1D) codes:


and a modified version of the Eulerian, 1D hydrodynamic flash4.0 code with thermonuclear burning


We show that with resolutions that are typical for multidimensional full-star simulations, the V1D and the flash results are not satisfactory (up to $50{{\ \rm per\ cent}}$ error in V1D and up to $20{{\ \rm per\ cent}}$ error in flash).


This progress has led to a general consensus about the main physical ingredients required to describe the evolution of the galaxy population (e.g.


In the past, various limits on LIV have been obtained from the spectral time lags of individual GRBs or a large sample of GRBs (e.g.,


Indeed, variability between the yields of different mergers is required to explain observed abundances in metal-poor stars


Measurements from Muller et al. (1980), Danjo et al. (1984), Mueller et al. (1985), and


demonstrated onsets below the ionization threshold.


The rate at which water vapour will be released is da/dt ∼ 1.5 × 10−3 μm yr−1 (scaled to the distance of the ring, from the result of


), where a is the vertical thickness of the layer.


Due to the complicated physical processes involved in spectral line formation in a 3D atmosphere (e.g.


it is difficult to quantify higher order effects beyond the linear relation between $\mathfrak {v}$ and Wλ; that is, the systematic uncertainty of the linear fitting.


Dense cores, where stars form, are located along or at the intersections of some of these fine substructures (e.g.


Theoretical models explain this inefficiency through a combination of mechanisms that provide support against gravitational collapse, including turbulence, magnetic fields, stellar feedback, and dynamical stabilization


Currently, a limited number of observations


are available to explore the environment dependence of the metallicity


Although most galaxies have an implied SFR that scatters within a factor two around the MS, some do show a significantly higher SFR. Those objects also exhibit a higher gas content, shorter gas depletion times (e.g.,


The predictions are based on experimental data from


It has also been generally believed accordingly that most activity (namely active galactic nuclei—AGNs) of supermassive black holes (BHs) at the centers of galaxies at low redshifts


appear to be fueled by the random accretion of gas via internal, secular processes working close to the BH (say, within a few hundred parsec,


Additionally, glycolaldehyde (C2 H4O2), the simplest form of sugar and one of the first intermediates in the formose reaction


, has also been detected in this object for the first time in space in 2012


On the other hand, the super-Chandrasekhar WDs were often explained by incorporating different physics, such as a


show that parameters of the differential rotation and convection, e.g. the typical size and turnover time of convective flows, depend on the general stellar parameters, such as mass, age, the spectral class and the rotation rate.


They were discovered as dark silhouettes against the galactic background at 8 and 15 μm with the Midcourse Space Experiment (MSX,


The comparison sample is compiled from the literature up to z ∼ 3


Such a Comptonisation mechanism accounts for the power-law-like shape of the X-ray primary continuum emission and the high-energy roll-over observed in various nearby AGNs (e.g.


while similar works were performed on INTEGRAL data (e.g.


Physically, it is the rotation that develops a toroidal magnetic field and a poloidal electric field in the lab frame (or the inertial frame), which seems to imply that Φ would not be chosen arbitrarily and would be self-consistently determined by the MHD equations, given the Ψ and Ω specified (e.g.,


Based on its SED, MWC 758 has been classified as a pre-transition disk


The distribution of number density, core radius, and concentration parameter remains the same, indicating that the population of clusters in the point source catalog is more compact than the extent-selected sample. The extent-selected sample does not show a clear bias toward cool-core clusters or clusters with a central AGN, but contains the fraction of cool-cores is similar to that of SZ surveys


In this sample, we observe the opposite trend.


and have coupled the code to SN ejecta models


The large mass and solid angle covered by highly concentrated galaxy clusters make them ideal gravitational lenses, which can be used as ‘cosmic telescopes’ to observe very distant galaxies (e.g.


For example, the well-known density–morphology relation reveals that the ellipticals are preferably found inside the dense groups and clusters, whereas the spirals are intermittently distributed in the fields


More recently, indications of radial anisotropy in the outer regions of DM haloes have been obtained from numerical simulations (e.g.


We have performed the first detailed dissection of the stellar populations of the Milky Way disc in age, [Fe/H] and $\mathrm{[ \alpha \mathrm{/Fe]}}$ space, bridging the gap between the detailed observational understanding of MAPs (e.g.


In 2007, it displayed a complex symmetric dimming pattern of up to ~ 3 magnitudes during a 56 day eclipse. This has been attributed to the transit of a substellar companion (called “J1407 b”) with a mass of 60–100 MJup


Interestingly, the D2 and D3 glide terms for these variants were found to vary by several tens of microarcseconds in the comparison to ICRF2, in line with the level of the systematics observed for those terms. Such findings are not unexpected since Galactic acceleration manifests itself as a dipolar deformation in the source coordinates (e.g.,


Nuclear optical line emission has been reported from spectroscopy


There is some tentative evidences for alignment with respect to the magnetic field


in, e.g., the IRAS 4A system at cm wavelengths


For the case of ρIA = 1.3 (magenta), a decrease of the amplitude of the primary can hardly be observed, as expected for low-amplitude wave


Similar rapid changes in the optical-UV flux are typically seen in other BLS1s, especially those at low Lbol/LEdd (e.g.


The mechanism by which a nascent millisecond magnetar might power a GRB jet has been studied in detail over the past decade


Other authors observed different systems and likewise saw chro-mospheric excess emissions


In fact, the X-ray continuum in AGNs is well modelled by a power law with a high energy roll-over (e.g.


The fraction of clumpy galaxies was studied from z = 0 up to the most distant galaxies identified today at z ~ 10


Another major coolant of the ISM is [O i]63 μm


For V593 Cen, we updated the orbital parameters using more complete light curves. The orbital inclination of 83°.18 is similar to the result (82°.6) obtained by


Using the critical intensity advocated by recent studies


In addition to these clean-based approaches, recent developments in the field of compressive sensing (CS) applied for astronomical imaging have given birth to many imaging algorithms, particularly for RI


Leveraging optimization frameworks, these methods aim to solve the underlying image recovery problem by enforcing sparsity of the image of interest in some suitable domain.


Unprecedented flux and spectral variability during these episodes have been observed


These IGM transmissions are estimated from Monte Carlo simulations (


) which generate 10 000 sightlines for redshifts consistent with the H i cloud distribution defined analytically by Inoue et al. (2014).


The problem of accretion on to an SMBH has been studied via hydrodynamical simulations (e.g.


Although such fundamental physics is well known, it has not been well studied in SNR shocks. In fact, it is usually assumed that the Ly β photons are at the limits of either completely optically thick or optically thin at SNR shocks, i.e. they are completely converted to H α photons or not at all (e.g.


Similar energy dependent pulse arrival time behavior can also be found in


Prominences are generally believed to be supported by the magnetic tension force of the dips in sheared arcades


For grains consisting of two or three materials, we first derive effective optical constants following the Maxwell Garnett mixing rule


The dynamics of stars can be related to the gravitational potential that they inhabit via the collisionless Boltzmann equation. For systems in a steady state with certain symmetry properties (typically spherical or axisymmetric) it is possible to find solutions to the phase-space distribution of a stellar tracer population, either through distribution function modelling or via the moments of the Boltzmann equation


A good example of this effect is the Virgo cluster, the closest rich galaxy cluster, considered a ram pressure stripping laboratory since a number of clearly ram pressure stripped galaxies have been observed (e.g.,


are indicated by the turquoise shaded region in panels c and d.


and a similar distribution function analysis using 5D phase-space data from Gaia


This was done using the complex dielectric function for the sample obtained by heating boehmite at 1173 K from


assuming a spheroid with depolarization parameters of (0.35, 0.035).


While the importance of including GR gravity in simulations of core-collapse supernovae has always persisted in the literature and is in use in many current and state-of-the-art multidimensional, core-collapse supernova calculations


many modern simulations have used a purely Newtonian approximation for gravity


Large numbers of works have extensively studied the binary-disk system in the Newtonian regime with


If we considered the AIA 304 Å observations alone, the on-disk condensation, and hence coronal rain events we report here would resemble those occurring in magnetically closed field lines


which are generally interpreted as a manifestation of the heating-condensation cycles due to thermal nonequilibrium


However, combining the observations of SDO and STEREO A and B at different viewing angles, we find that the on-disk coronal rain in this study corresponds to the downflows of condensations facilitated by reconnection between open and closed structures.


More specifically, fast- and slow-mode magnetoacoustic waves in coronal plasma structures are well-known to be subject to a frequency-dependent damping by e.g. resonant absorption and thermal conduction (e.g.


Here we additionally make the assumption that stellar mass comprises 50% of the baryonic content of galaxies by mass at these redshifts, a value broadly consistent with the few measurements made at or near these redshifts (e.g.,


Moreover, the disk formation process has been revealed to be much more complicated for binary and multiple cases, both in observations


In spite of its huge infrared luminosity, the host galaxy is classified from the optical morphology as an ordinary Sa-type galaxy ([R’]SAB[s]a;


Typical values are close to D2 = 1.4–1.5


which are consistent with the fractal dimension as derived for the young stellar structures.


and Li etal. (2016) both found that the rotation measure predicted from the ADAF is roughly consistent with the observational values.


The majority of past applications of this method constrained the IGM thermal state by fitting the low-b-$N_{\rm H\, {\small I}}$ cutoff of the $b-N_{{{{\rm H\, {\small I}}}}{}}$ distribution


Furthermore, statistical variations in the observed magnetic field direction near the SWTS were included as a time series to model time variations in the injection and DSA of pickup ions to simulate the highly volatile nature of actual DSA at the SWTS


we used a custom filter centred on the deep 1.45 µm feature present in YPMOs to distinguish between them and background sources. In the 2–5 µm range covered by NIX, such water features are far less dominant, and there are strong telluric features across some of this range that would make a similar ‘water’ technique difficult to use. Instead, we use the differing spectral shape in K-band of very low mass brown dwarfs when compared to earlier spectral type stars.


Clarke et al. (2019) and Buck (2020) suggest that bimodality should be common in disc galaxies, whereas


For our disk model, we are using the power-law profile for the scattering surface height H and the separation r found by


for the disk around HD 97048. This profile describes the flaring discovered in this source reasonably well up to a separation of ~270 au.


These PESs have also been able to account for even subtle effects such as the GP


This is likely to need to be considered for different possible exterior disc models and in addition the planets may have built up their masses as they went (see e.g.


These considerations are beyond the scope of this paper.


However, there is no theoretical argument (or pathology) against GWs propagating faster than light (see


In past years, several alternatives have been proposed to constrain the redshift of BL Lac objects, including


or from the neutral hydrogen in the intergalactic medium (e.g.


While this approach initially appeared to work remarkably well in the case of starburst galaxies


there is now ample evidence that there is no tight universal relation between the UV slope and the


Such an approach, also known as floating chunk offset method (FCO;


has proven extremely reliable even in the presence of complex activity signals, as shown by Malavolta et al. (2018).


The initial condition is the Orszag–Tang vortex (OTV) (e.g.,


In the case of GRBs, approximately 1/6 of examples are consistent with a galaxy nucleus


showed that the annual Ursid shower was related to comet 8P/Tuttle, a Jupiter family comet with a period of 13.6yr (JPL-HORIZONS, ssd.jpl.nasa.gov) and a perihelion distance slightly greater than 1au.


High-resolution CO observations are critical for evaluating where high-redshift galaxies fall on the true surface density version of the Schmidt–Kennicutt relation, where ΣSFR and Σgas can be compared on a pixel-by-pixel basis within individual galaxies (as done for local galaxies; e.g.,


Studies have shown that heating mainly escapes through the outflow cavity in deeply embedded sources


Secondly, in practice, determining the location of the cutoff is vulnerable to systematic effects, such as contamination from the narrow metal lines


where the formation of a stellar bulge stabilizes the disk against further star-formation, is also improbable.


The production of elements in the region of Sr, Y, and Zr is more efficient for slightly neutron-rich conditions, corresponding to RLn = 1.35


We observe a very similar behavior and dependency of abundances on the Ye distribution for all exploding models of the 15 M⊙ progenitor.


Atiras or Interior Earth Objects (IEOs) have aphelion distances 0.983 au and can only be observed at low solar elongations (often 70○); Vatiras have aphelia 0.718 au, are observed at very low solar elongations (typically 40○–45○), and just one such object is currently known


The distances of the nebulae from the illuminating star are about 1 pc, assuming that they are located near the plane of the sky occupied by γ Cas


NLs have high accretion rates (∼10−8 M⊙ yr−1), so are in a persistent high state, and they gather above the period gap in the period distribution of CVs


In particular, the SPS approach has been applied to observations of various Galactic and extragalactic environments (e.g.,


showing power spectral slopes β roughly ranging from −2.7 to −3.7 depending on the tracers used (e.g., H i, carbon monoxide (CO), and dust).


Since the halo concentration cannot be reliably measured for haloes with fewer than about ∼400 particles, we use the method presented by Ramakrishnan, Paranjape & Sheth (2021) to assign concentrations cvir (assuming


NFW profiles) conditioned on the mass and local tidal environment of individual haloes.


Finally, the MFD internal shock (IS) model for GRBs also suffers some criticisms, such as


and inconsistency with some empirical (Amati/Yonetoku) relations


their projected axis is oriented perpendicular to the disk midplane whose inclination with respect to the line-of-sight was estimated to be less than 30° (namely, the disk is seen approximately edge-on;


data release as well as calibration vectors for the MaNGA survey


In the upper panel, we show small-scale features in calibration vectors from the same plate (number 3647) processed by the DR9 (blue), DR12 (green), and DR14 (red) pipelines. The spectra are obtained by normalizing the large-scale features in calibration vectors with a cubic b-spline with break points separated by 50 Å. The three spectra are mostly identical while the smooth curving features at the wavelengths of Balmer series in DR9 disappear in DR12 and DR14. From DR12, the pipeline corrects the features with linear interpolation across wavelength regions with Balmer β, γ, and δ lines


One can also observe the change in the median residual spectra of DR9 and DR12 in Fig. 1. However, the Hα feature remains uncorrected from DR9 to DR14.


Given our very limited knowledge of the ternary C/O/Ne phase diagram


this effect cannot be quantitatively implemented in our evolution models.


However, we note that our current understanding of 22Ne phase separation is remarkably consistent with the missing cooling delay.


Interestingly, we found that, four HSPs did not show any IDV


is based on similar ideas, but makes use of the optical Hα surface brightness and a wide set of various calibrators.


It is worthwhile noting that laboratory experiments on the coagulation growth of water-ice particles have a long history outside astronomy and planetary science, since coagulation is observed in daily life and is a plausible route to the formation of snowflakes (e.g.


Indeed, the first molecular searches of PNe turned up negative (e.g.,


Treatment of errors for combining distance moduli across methods or across measurements is suggested by


and Tully et al. (2016) to be based on weighted estimates such as the uncertainty of the weighted mean, albeit with caution partly due to the heterogeneous origin of the compiled data and partly due to Malmquist bias.


Further, the higher contrast of the acoustic features in EE power spectrum compared to astrophysical foregrounds


will ultimately provide independent and tighter constraints on the standard cosmological parameters, such as the scalar spectral index ns, than those from the temperature data alone.


The role of twisted magnetic field in the MHD waves has been studied in many theoretical works (e.g.


However, a hot region with radius 3–4 times smaller than R can still produce a pulsed fraction below current limits of 20–40 per cent in the spin period range 0.1–0.4 s of known CCOs (see Section 1; for pulsed fraction dependence on spot size, see, e.g.


Indeed, the ultraviolet and X-ray variability detected for many of these LINERs


is in favour of a direct view of the AGNs (i.e. perpendicular to the disc under the UM). This is consistent with the fact that most of the [O III] morphologies found for LINERs are spheroids, if we assume that the [O III] traces the NLR.


showed that the main differences between the migration recipes from Jiménez & Masset (2017) and Paardekooper et al. (2011) lie in the computation on the corotation torque.


According to this framework, HERGs are powered by accretion of cold gas, provided by e.g., a recent merger with a gas-rich galaxy, while LERGs accrete hot intergalactic gas from dense environments at a low rate


with fuelling from major mergers strongly disfavoured by recent observations (e.g.,


he protoplanetary embryos masses scale as M ≈ r3(2 − x)/2Δ3/2


where Δ is the mutual Hill radii separations between embryos orbits.


The flux ratio ϕ(α)/ϕ(0) can be derived by using the dust phase function


Several SNe surveys have set strong constraints on cosmological models from the distance–redshift relation (e.g.


However the measured apparent magnitudes, have a residual scatter arising from its intrinsic scatter and effects due to line-of-sight (LOS) structures.


In systems with very large super-Eddington mass-transfer rates, matter presumably piles up around the NS and forms a growing, bloated cloud engulfing a large fraction of the accretion disc. A system will only avoid a CE if it manages to evaporate the bulk of the transferred matter via the liberated accretion energy at a distance from the NS larger than the trapping radius. Otherwise, the incoming material has too much negative binding energy to be ejected. At the same time, this trapping radius must be located inside the Roche lobe of the NS in order to avoid a CE


An LBV star provides an adequate explanation for the transient time-scale, the isolation (e.g.


the lack of a host H ii region (Fig. 2 and 3; see below, however), and the transient/main source offset (d ≈ 0.3 kpc, for D ≃ 8 Mpc; Table 1; see below, however).


As a result of the analysis of 3 min oscillations detected in observations from the Atmospheric Imaging Assembly instrument


on-board the Solar Dynamic Observatory (SDO;


These studies all used an invariant quantity (the Reynolds stress or thewave action for rotating or magnetic flows) as a diagnostic tool to interpret the role of the critical level in terms of energy transmission and to quantify exchanges between the wave and the mean flow


Only a few hot corinos have been identified so far either with single dish or interferometric observations:


Sparse and/or irregular sampling is a very common issue in SF analysis


Active suppression of these speckles requires measurement of the electric field associated with the speckles directly from a coronagraphic image using a focal plane wavefront sensor (FPWFS). Several FPWFSs have been proposed such as phase diversity


Observations of such ‘low-luminosity’ ULXs


have revealed changes in the disc emission that may imply the creation of a radiation pressure supported, larger scaleheight flow in the inner regions


Whether the core collapses or the deflagration disrupts the core depends sensitively on the ignition density


This is consistent with other results (e.g.


which have shown that galaxies having higher current SFR relative to their past averaged SFR are likely to deviate above the IRX–β relation, i.e. have larger AFUV(IRX) for a given AFUV(β).


Despite this qualitative agreement, the Kong et al. mean numerical relation for their UV-selected sample of 50 local starbursts is not a good fit to the FIR-selected SFRS data as shown in Fig. 9.


We excluded stars with saturated photometry


by limiting the magnitudes of the detected VISTA/VVV sources to 13.8, 12.8, and 12.8, for the J, H, and KS bands, respectively.


While this is an important difference between the two line lists, generally speaking, it is suggested that using very strong lines often introduces complications such as non-LTE effects into a chemical abundance analysis (e.g.,


For example, using Gaia Data Release 2 (DR2)


Kounkel et al. (2018) and Zari et al. (2019) demonstrated that the Orion star-forming region is composed of a variety of populations with different spatial and kinematic properties each that are all likely generated in multiple events instead of in a progressive star formation history (see also


discussing three bursts of star formation in the Orion Nebula cluster).


Many systems have not been taken into account due to several issues. For instance, the system PG1115+080


from the CASTLES survey has been discarded because the lens mass model is steeper than isothermal.


Theoretical predictions are now available


but they have not yet been thoroughly tested against observations, because only very few stripped stars with sufficiently strong wind mass-loss have been identified and studied in detail so far (e.g.,


More generally, a body of work in various domains,


has tried to understand the properties of wave propagation and dissipation around co-rotation and, more generally, at all special locations in fluids that correspond to singularities in the linear wave propagation equation.


Here, we report on Large Binocular Telescope (LBT) observations of an isolated pulsar, PSR J2043+2740


The grain-surface network has been further updated to include all studied routes to water formation under interstellar and circumstellar conditions


We estimated the projected spatial wavelength λproj of the “wiggling” wave according to λ = λproj∕sin i, where i is the angle between the jet symmetry axis and the line of sight, and T = λ∕υ, where υ is the jet velocity, from


State-of-the-art PT has proven successful in predicting the large-scale behaviour of the velocity PDF and the correspondent monopole and quadrupole of the redshift-space correlation function (e.g


, at least for massive haloes, M ∼ 1013 M⊙.


However, the addition of weak bars in low-mass blue galaxies is insufficient to resolve the apparent disagreement between Erwin (2018) and many SDSS-based studies


which instead seems likely to be due to the very different sample selection of the S4G and SDSS galaxy samples.


We recalculated the lifetimes of molecules assuming AV = 3 mag, and with (1) standard dust properties (i.e. with composition and size distribution as of interstellar dust) or (2) with larger and less opaque grains, at the gas-to-dust mass ratio of 124 (see


for more details on the assumed dust properties).


The 10.0–70.0 keV flux of the source is found to be (2.26 ± 0.01) × 10−9 erg cm-2s-1, much lower than the value (5.6 ± 0.3) × 10−9 erg cm-2s-1, previously reported from SUZAKU data


To speed them up, we used the Modified Random Walk method implemented in RADMC-3D


that the local overdensity correlates with the group-centric distance (e.g.,


One should note that during studies of the isolated Abell groups


only a rudimentary alignment was found and related only to the brightest cluster members.


We also manually perform the absolute wavelength calibration using a relatively strong neutral line, O I 1355.60 Å (see


The extended star formation history and the broad range of metallicity (−1.5 ≲ [Fe/H] ≲ 0.2) discovered in the stream fields can be explained by a disk galaxy progenitor


In the case of NGC 7213, the photometric data included in the analysis are:


However, such a degeneracy can be broken when the inner edge of the disk is very close to the compact object


Asteroid 469219 librates around $\omega _{\rm r}=-90{^\circ }$ for Venus, the Earth, and Jupiter. This behaviour corresponds to domain III in


horseshoe-retrograde satellite orbit transitions and librations (around $\omega _{\rm r}=-90{^\circ }$ or 90°). For a given cycle, the lower part corresponds to the horseshoe phase and the upper part to the quasi-satellite or retrograde satellite phase.


Indeed, constraints from explosion parameters have shown the majority of CCSNe to be consistent with lower mass progenitors, as opposed to more massive Wolf–Rayet stars


GRBs likely represent a population with rather larger initial masses


It is thought that the early pre-solar nebula was hot (>1500 K), such that both volatiles and refractories (Tsub ≳ 1400 K) are in the gas phase out to larger distances


Such lens model has found widespread astrophysical applications in the literature


In particular, detailed analysis of the radial column density profiles indicates that, at least in the nearby clouds of the Gould Belt, molecular filaments are characterized by a narrow distribution of crest-averaged inner widths with a typical full width at half maximum (FWHM) value Wfil ∼ 0.1 pc and a dispersion of less than a factor of ∼2


The different cosmologies used in the Millenium simulation (in particular, σ8 = 0.9; Springel et al. 2005) by Saro et al. (2013) and the simulations by


To perform the fitting to the data, we adopted the Python package emcee


, a pure-Python implementation of Goodman & Weare’s Affine Invariant Markov chain Monte Carlo (MCMC) Ensemble sampler.


SN 2006jd was observed at 1638 days, an epoch very similar to that of SN 2014C, with Spitzer/IRAC and WISE


In all three cases, the photometry and spectra from 1 to 10 μm are well fitted by purely carbonaceous dust models, which we overplot in Figure 6 using dust parameters from the literature.


The motion of the photospheric footpoints of the coronal magnetic field may also trigger the forced magnetic reconnection, which may be caused by the explosive solar coronal events (e.g.,


The presence of the substructure has been confirmed by


as well as by more recent SZE measurements


By using these techniques, some studies show a correlation between both 12 + log (O/H) and log (N/O)


Studies of clusters and groups at $z$ ∼ 0 have evidently shown that outskirts of groups and clusters


are favourable sites for galaxy transformations.


Still, some correction residuals persist and render the AO PSF shape complex to model. Consequently, standard parametric models that reliably reproduce the seeing-limited PSFs, such as a Moffat function


become inefficient at describing the AO PSF.


One of the methods based on the synergy between UV and WL observations is the Doppler dimming technique


This result is in broad agreement with models of jet launching from ADAFs (e.g.,


which predict the formation of a thin and mildly-relativistic outer layer.


Both clusters host two kinematically distinct populations


More details can be found in our previous papers


A bright X-ray background source such as


can be used to detect the WHIM by producing absorption features in its energy spectra


References for the observational data are as follows: RX J0852.0−4622:


With the obtained abundances [C/Fe] = +2.2 dex and [C/N] = +1.15, HD 112869 occupies the region of CEMP-s stars on the plots [C/Fe] versus [Fe/H] and [C/N] versus [Fe/H] (see Figures 5 and 6 in


Another possible effect of the AGN activity on the molecular gas is through outflows. This possibility is supported by observations of individual objects: For example, Carniani et al. (2017),


and Loiacono et al. (2019) find low gas fractions in powerful AGN at cosmic noon hosting high-velocity molecular and ionized outflows


During the transition from the subcritical to the supercritical regime, sources show two different branches in their hardness–intensity diagram (HID) which are known as horizontal branch (HB) and diagonal branch (DB)


This correlation, hereafter referred to as the R–σv relation, is usually interpreted as the result of turbulent motions in the interstellar medium on all scales


Observation of magnetic fluctuations in the SW indicates that omnidirectional power spectra approach a k−1 wavenumber dependence and that low-frequency turbulence exhibits some sunspot cycle variability


For a circular polarized wave, the dispersion relation in the laboratory frame is given by (e.g.,


We measured 164 ± 13 background-subtracted counts between 0.2 and 2.0 keV, as determined using calc_data_sum in Sherpa


The cluster then forms a dense core of high-mass stars and once it starts to collapse, binaries form in the centre. These perturb their neighbours, and we begin to observe massive stars escaping from the mass segregated core


then yields Lbol ~ 1.7–2.8 L⊙, depending on whether the NIR flux is neglected (which may be the case) or extrapolated from γ = −2.


They are, however, computationally much more expensive and their complexity makes it more difficult to test underlying modelling assumptions compared to GCMs with simplified thermal forcing. The latter are thus better suited to run simulations for various scenarios, to understand large-scale flow and circulation properties in 3D climate models under different conditions


In addition, recent observational and theoretical studies on RSGs and SNe II indicate that RSG wind mass-loss rates may be independent from metallicity


It is also possible to build embedded void lens models with non-spherically symmetric density profiles given that the lowest-order embedded lens theory is applicable to any distributed lens


The first kind of current-sheet formation is associated with the MHD instabilities (e.g., resistive tearing mode and ideal kink mode) known as spontaneous magnetic reconnection (e.g.,


he SFR reported in Table C.1 refers to a stellar mass range from Mlow = 0.1M⊙ to Mup = 100M⊙, is averaged over the past Δt = 100 Myr, and was calculated using the standard SFR(LIR) relationship from


here scaled to a Chabrier 2003, IMF) (1)\begin{equation} \label{eq:sfr} \textit{SFR}=10^{-10}\times L_{\rm IR}[{L}_{\sun}]\, {M}_{\sun}~{\rm yr}^{-1}. \end{equation}SFR=10-10×LIR[L⊙] M⊙yr-1.


Recent advances in understanding the properties of magnetohydrodynamic (MHD) turbulence


stimulate a renewed investigation on density statistics


which provide important insight into key physical processes such as star formation in the turbulent and magnetized ISM


The surface temperatures of such hydrostatic, strongly inflated models computed with plane parallel grey atmospheres are then compared with the fictitious effective temperatures at τ = 20 of the atmosphere calculations performed by


Moreover, Draine’s formulation is accounted to determine the lunar surface’s photoelectric efficiency (


) – its spectral dependence can be represented as ${\chi _{\nu r}} = {\chi _o}[1 - ({\phi _r}/{E_\nu })]$.


Since the source emission has been stable for more than 15 years


we performed the joint fit with the longest, burst-free NuSTAR observations (ObsID = 30001025012) and XMM-Newton observations that were performed ∼11 years earlier.


However, LC II/LFIR is not constant, but declines with increasing LFIR, known as the ‘[C ii] deficit’


Despite the considerable scatter in both colors and color gradients


the tight correlation between color and stellar mass of the host galaxies holds true in both the region identified as intermediate and outer in Sect. 7.


Including baryon physics introduces some distortions in the scaling relations between the mass and other physical quantities such as temperature, X-ray, or optical luminosity


As happens within Earth’s clouds, exoplanet clouds are likely gravitationally stratified, meaning that smaller, lighter grains become concentrated at the top of the clouds, while larger, heavier grains remain at lower elevation


The source is a known source that appears in many sky survey catalogues, including Gaia, where its G-band magnitude is listed as 14.1 and its inferred temperature is ~5000 K (see


for how the listed temperature we extract from the Gaia catalogue is inferred from the Gaia data).


More complex and fragmented mixing structures are generated in the higher resolution simulation, which indicates that the process producing these structures is not completely resolved at the current resolution (see, e.g.,


These often-called starburst galaxies, with an IR luminosity LIR ∼ (0.1–5) × 1012 L⊙ (e.g.,


become increasingly more common at high z.


Although spin misalignments may be introduced by natal supernova kicks, episodes of mass transfer and tidal torques serve to realign component spins before the formation of the final black hole binary


However, from spectro-polarimetric observations of a γ-ray emitting NLSy1 galaxy, PKS 2004 − 447


and accretion disc modelling of a sample of 23 radio-detected NLSy1 galaxies


indicate that they have masses similar to the blazar class of AGNs.


The GP effect, while not significant at temperatures relevant to astrophysics, is important below 1 K as illustrated in a series of calculations on H + HD (v, j) collisions for vibrational levels v = 4 − 9


Indriolo & McCall (2012) find a mean ζH of 1.8 × 10−16 s−1 in their sample of diffuse molecular sight lines, and values as large as ∼1 × 10−15 s−1 have been reported in the literature


It should be noted that only a handful of studies so far have looked at the correlation between α and global galaxy properties:


However, the stellar number densities required for tidal truncation are high, and in practice few observed regions satisfy this condition


Since long cosmologists have felt motivated to look for alternative explanations for the DE beyond a rigid cosmological constant Λ. The scalar field paradigm was then profusely used also to make the cosmic vacuum dynamical: Λ = Λ(ϕ). In the old days, the main aim was to adjust the large value of Λ typically predicted in QFT to be zero. There were many early proposals (see e.g.


Second, while the predicted shadow feature is nearly independent of the spin or orientation of the black hole to within 10%


the emission region surrounding the black hole depends on the details of the underlying accretion process and is intrinsically time variable primarily due to the stochastic nature of magnetorotational-instability-driven turbulence and magnetic reconnection in the accretion flow.


We adopt a different perspective in proceeding from the basic guiding center kinetic equation (e.g.,


instead of the transformed Vlasov equation (Skilling 1975) used by Zank etÂ al. (2014).


It has already been tested with real data collected by the LIGO and Virgo detectors


though the constraints obtained so far with this ‘statistical’ method are not competitive with the ones derived from GW170817 and its EM counterpart, mainly because of the poor spatial resolution of the current network of ground-based interferometers.


In fact, this concept pre-dates the large-scale use of IFU with works dealing with, for instance, photometric disc/bulge decompositions of surface brightness profiles (e.g. see


However, resolving individual spots may be imprecise with poor instrumentations, and a new series, based only on sunspot groups, was proposed, called the group sunspot number, GSN


We note that a similar result was found in observations of the Seyfert 1.2 ICÂ 4329a and the narrow-line Seyfert 1 SWIFT J2127.4+5654 with NuSTAR


the Helios proton data radial gradients of the GCR flux were found to be 6.6 ± 4% above 50 MeV and 2 ± 2.5% between 250 and 700 MeV between 0.4 and 1 AU. These results are in agreement with those from Pamela/Ulysses (within the statistical and systematic errors).


The collision velocity dependence of the coefficient of restitution between particles was observed in experiments


Assuming a set of stellar population models


to generate spectral energy distributions for galaxies at the emission-line redshift, and fitting them to the available photometry, can give estimates of physical quantities of the galaxies like total stellar mass (the normalization between the observed flux and best-fit model), the star formation rate, metallicity, and the age of the stellar populations, i.e., the galaxy (e.g.,


Generally, during the hopping process, the acceleration first shows a gradual increase, and then decreases rapidly at the end of control torque, during which the reaction force is highly fluctuating due to intermittent transmissions of acoustic energy along force-chain-like networks


Most recently, Rodriguez-Almeida reported the first unambiguous detection of ethanethiol in the ISM, toward the G+0.603-0.027 molecular cloud


On galactic scales massive molecular winds are common in local Seyfert galaxies (e.g.


Unfortunately, measurements of UV radiation are strongly hampered by the interstellar medium absorption (up to 70%–90%), which is significant even for relatively close stars, so that estimates of stellar UV radiation strongly rely on modeling (see


The standard model of such a turbulent dynamo producing a large-scale magnetic field involves the amplification of seed magnetic fields due to the usual α effect, where α is a measure of the net kinetic helicity in the flow (see, e.g.,


Our results are consistent with this idea and provide additional evidence for IGM gas feeding into galaxies through streams from the cosmic web (e.g.,


In the literature there are several theoretical works on the evolution of [Ba/Fe] and [Y/Fe] in the Galactic thin disc (e.g.


The main and novel aspect of our work is the analysis of the diffuse radio emission resulting from radio haloes in galaxy clusters


In cosmological hydrodynamical simulations, the O vi absorbing gas lies behind the halo accretion shock and is maximal in L* galaxies because their virial temperature is close to the temperature T ≈ 105.5 K where the O+5 ionization fraction peaks


Red novae are recognized as manifestations of on-going mergers of non-compact stars such as main-sequence dwarfs, sub-giants, or red giants


have been used to estimate the angular power spectrum of the diffused galactic foreground


These works propagate the uncertainties in each visibility estimate and combine that with the sample variance error in measuring the power spectrum to quote uncertainties in the power spectrum estimates.


However, the theoretical works that describe the fundamental properties of the low angular momentum accretion and that usually treat the steady solution of the equations have so far been carried out only for nonmagnetized and usually also nonviscous flows


The spatial density measured with para-H2CO (303–202) and C18O (2–1) in N113 and N159W is n(H2) ~ 105 cm−3 on a size of ~30″


We perform this emissivity calculation separately for the main sample of spectroscopically confirmed LBGs and LAEs from M13 (using the UV luminosity functions from


We note that Capak et al. (2011) found that AzTEC3 belongs to a spectroscopically confirmed protocluster containing eight galaxies within a 1 arcmin2 area, and therefore the environment might also play a role in the galaxy size evolution (see also


However, it is currently unclear whether the environmental effects in a galaxy overdensity will lead to a more compact or more extended radio-emitting size than field galaxies.


Among the main proposed formation channels for merging binary COs, we find:


The gas-phase chemical network from Röllig et al. (2007) (mainly based on the UMIST99 ratefile;


allows us to reproduce the C+, CO, and HCO+ abundances in PDRs


so we use this network together with the ionization of the atomic species and corresponding recombinations in the H ii regions.


Another element of the realistic phenomenological hadronic EoS corresponds to the short-range repulsive interaction of the hard core nature between particles


Although the production of HCOOH has also been investigated experimentally


its formation process and chemical link to nitrogen-bearing species are puzzling.


So far, the biggest efforts were focused into two, somewhat complementary approaches. The first is represented by simulations like


These follow structure formation in a large cosmological volume at the expense of having a medium or a low-mass resolution. Such simulations provide the formation histories for a very large number of medium- and high-mass DM haloes, but do not necessary resolve all the details relevant for galaxy formation.


To accurately describe the shape and internal structure of Jupiter, various interior models with new ingredients, such as two-layer and three-layer structure models, have been established by several groups


A potentially powerful tool that was suggested in the literature is the measurement of deuteration fractions, which may be translated into time-scales via chemical models


Such carbonaceous mantles are efficiently processed by UV photons


but can stay H-rich as long as the radiation field is attenuated


was based on only one line of the gGg′ conformer of ethylene glycol about 200 cm-1


above the lowest-energy aGg′ conformer – and thus tentative.


In this work, we will provide the ζ(T, f) function calculated under the assumption of ionization equilibrium using the CHIANTI spectral code


as detailed below. In this framework it is straightforward to users to replace the CHIANTI values for the equilibrium ion fractions by their own values calculated under nonequilibrium conditions, depending on the physical process they model.


Observations have shown that the IRX-β relation varies with


In addition, several observational studies have suggested that the star formation rate (SFR) of the clouds appears to increase over their lifetimes. For example, studies of young clusters embedded in moderate-mass MCs (∼104M⊙) (e.g.


have shown that their age histograms contain a large majority of young (1–2 Myr) objects, but also a tail of older (up to several Myr) ones suggesting an accelerating star formation activity, sometimes followed by a subsequent decline


It is likely that some of these products are also formed in our experiments, but except for CO2, HNCO, and NCO−, they cannot be unequivocally identified with IR spectroscopy alone. Some of them have the same functional groups as urea and their IR spectra present absorptions in the same spectral regions, albeit with different band shapes and intensities. They could contribute somehow to the changes, both in shape and intensity, observed in the absorption bands during processing and thus introduce uncertainty, but by analogy with the literature results just mentioned


we expect that the prevalent dissociation channels will lead to small molecules that will not interfere much with the absorptions of urea.


IRIS observations show that Fe XXI 1354.08 Å is a hot (∼11 MK) and broad emission line and is always blended with many narrow chromospheric lines at the flaring ribbons


The most common way to derive galaxy sizes is by performing light-profile fitting assuming a given shape of the surface brightness profile using a χ2 minimization


\label{number5} \end{eqnarray}kα=κα/hα, kβ=κβ/hβ.Equations (2) and (5) give a direct and elegant expression for the perpendicular wave vector as (7)\begin{eqnarray} \vec{k}_\perp \approx -(\bdel \omega_{\rm c}) t, \label{number6} \end{eqnarray}k⊥≈−(∇ωc)t,which is a generalisation to three dimensions of the results of Mann et al. (1995),


for lower dimensional systems, which developed phase mixing in only one perpendicular coordinate.


The observed optical light curves are smoother than expected and an insufficient fraction of the X-ray emission hits the disc to power the optical variability (e.g.


Moreover, due to their low density, voids are naturally sensitive to dark energy and thus the interest to use them as probe of alternative Dark Energy models and modified gravity scenarios is increasing


The 16th and 84th percentile of the resulting peak flux density distributions, together with the systematic flux scale density uncertainty of 5%


for the FIRST and LoTSS survey, respectively, are used to determine the error on the spectral index.


Significant progress has been made in recent times through detailed full-quantum scattering calculations, based on quantum chemical data, for the cases of simple atoms such as Li, Na, Mg and Ca


Bound galaxies (subhaloes) were identified within the simulations using the subfind algorithm


in the same manner as in the EAGLE simulations


As a result, recent studies have shifted to using dark-matter halo masses as large as 1011 M⊙


based on halo abundance matching arguments.


show strong offsets in the kinematics of the gas from the host galaxy (≈100 km s−1;


whereas the COS-AGN sightlines do not (bottom panel of Fig. 6)


Recently, three unusual TDE candidates have been discovered by Swift, i.e., Swift J164449.3+573451, Swift J2058.4+0516, and Swift J1112.2-8238 (hereafter Sw J1644+57, Sw J2058+05, and Sw J1112-82 for short, respectively), which have very bright nonthermal hard X-ray and radio emissions


In analyses of the resolved star formation properties of nearby disks, a near-unity index for the Schmidt–Kennicutt relation is also found in regimes where the molecular gas dominates the total gas mass surface density (Σgas >9 M⊙ pc−2; e.g.,


and Abbott et al. (2022), a natural consequence from having a (approximate) Gaussian distribution is a reasonable concordance among the three different error measurements, that is, ⟨σα⟩∼σ68 ∼ σstd.


Direct observational evidence for AGN feedback on galactic scales in such environments remains sparse. More specifically, while outflows have been observationally detected in a number of instances around AGN in various gas phases, most of these detections have been made in ultra-luminous infrared galaxies or some of the closest quasar–host galaxies


with only a few examples where the AGN have been shown to couple with kpc-scale outflows that are capable of impacting star-formation on galactic scales (for a review


Thus, it is still unclear to what extent the general AGN population could drive kpc-scale galactic outflows capable of possibly limiting or quenching star-formation in the local Universe.


Lupus 3 MMS is a Class 0 protostar with a bolometric luminosity (Lbol) of 0.41 L⊙ and a bolometric temperature (Tbol) of 39 K in the Lupus 3 cloud at a distance of 200 pc


The parameter m play crucial role in the launching of Blandford–Payne type wind from the accretion disc


While He lines are often removed due to substantial differences between magnetometry results obtained from He versus metallic lines (e.g.


in this case He lines were left in the mask since the majority of the Stokes V line flux comes from these lines, and the Stokes V profiles extracted using a line mask with He lines excluded did not result in detectable Zeeman signatures.


Thanks to large spectroscopic surveys, the search for these chemically peculiar stars is becoming more efficient. Using high spectral resolution surveys, multiple elements, like C, N, O, Na, Mg, and Al, can be measured, depending on the wavelength range and signal-to-noise ratio. Toward this,


and Gaia-ESO survey have led to the discovery of a large group of N-rich field stars


The residence time can be calculated as the time it takes to deflect the accelerated electron by an angle ~1/Γsh


In addition, there is evidence demonstrating that bars can enhance star formation in the central regions of galaxies (e.g.


This connection between radio emission and star formation is strongly supported by the close infrared (IR)-radio correlation observed in galaxies (e.g.


We use the quadratic limb-darkening coefficients reported by


to establish the stellar center-to-limb intensity profile,


However, to date only the FIRE collaboration has implemented the two moment method (capable of dealing with CR streaming) in such simulations, and – in contrast to, for instance, van de Voort et al. (2021) – the plasma β in their winds is too high for the acoustic instability to develop


Ohmic dissipation operates in high-density regions with weak field, AD dominates in highly ionized and low-density regions, and the Hall effect lies in between


The spectral properties of LAEs are usually interpreted as coming from young (≲50 Myr) and low-mass (M*   1010 M⊙) galaxies


which are actively star forming (SFR ∼ 1 − 100 M⊙ yr−1) and dust poor (dust attenuation AV   0.2, see e.g.


Using deep LOFAR 150 MHz observations in the 7 deg2 Boötes field


studied the FIRC at 150 MHz from z ∼ 0.05 out to z ∼ 2.5. They found fairly mild redshift evolution in the logarithmic IR to radio luminosity ratio in the form of qIR ∼ (1 + z)−0.22 ± 0.05.


However, if the FIRC is non-linear (i.e. the logarithmic slope is different from one), then it implies that the qIR parameter would depend on luminosity.


The interplanetary manifestations of CMEs


can be measured by a spacecraft at about 1 AU and exhibit the following characteristics:


counterstreaming suprathermal electron (CSE) strahls and declining speed


In particular, if the field line angular velocity is set much less than the horizon angular velocity by distant plasma and a very tenuous plasma exists in the event horizon magnetosphere, then radiation resistance will determine the flow dynamics of accretion as well as the rotational energy extraction by a putative jet


Therefore, here, we first consider whether Eddington-limited accretion in such a neutron star LMXB might explain the observed radio behaviour in Sw J1858. The neutron star LMXBs with the highest mass accretion rates are the Z-sources, which are thought to accrete near or at the Eddington luminosity, tracing out Z-shaped tracks in their X-ray colour–colour diagrams


Also, in this scenario, Sw J1858 should not have resided in the much more radio bright Horizontal Branch during any of the observations, which is unlikely given the time-scales and commonness of transitions between the branches


A possible explanation for these low braking indices may be through the emission of a relativistic particle wind


For example, Sirko et al. (2004), Kafle et al. (2012),


Kafle et al. (2014) and King et al. (2015) fit an ellipsoidal distribution of velocities


Taking into account all these effects, the HPR of the overall RASS PSF is 84″


However, this method leads to systematic errors as creation of 1D light profile by either averaging over the galaxy image or by taking a single cut along the major axis do not properly take into account non-axisymmetric features like a bar or isophotal twist (for more details see


As of today, many more mass ejection channels have been discussed:


The course of the outburst was monitored in


It has been demonstrated that the statistical predictions of the ‘bubble model’ and the 21cmFAST agree fairly well with radiative–hydrodynamic simulations


at least when recombination, feedback, etc. are ignored.


these two sequences are associated with the thick disc (high-alpha) and thin disc (low-alpha), respectively.


This is in agreement with the finding that the thick disc has a shorter scale length than the thin disc


In the case of collimated relativistic jets, magnetic fields must play an important role


A periodogram of these RVs showed a clear signal at 35.57 days, but the TESS photometry and the RHK index


indicate a stellar rotation period of around 35 days, calling for caution.


The accretion rate then reaches the standard value predicted for MYSOs of $10^{-3}\, \rm M_{\odot }\, \rm yr^{-1}$


up to the onset of the disc formation happening at ${\approx } 12\, \rm kyr$.


Since the planet is synchronized within a timescale of a few thousand years, the stellar tide drives the secular orbital evolution


to assume an effective medium theory, such that a pellet is a mixture of one of their samples with a matrix of air.


The slow rising afterglow light curves also rejected a uniform top-hat jet


We have not included in our models the effects of ‘kicks’ caused by asymmetric emission of gravitational waves, which have been proposed to be possibly responsible for ejecting BHs from haloes with shallow potential wells, thus halting or reducing the growth of high-redshift BHs hosted in small haloes (e.g.


This effect, however, seems to affect less than 10 per cent of binaries


Whether or not any theoretical mechanism presently exists to explain the formation of giant planets in binary systems, the fact remains that at least a few binary systems, such as γ Cephei


do harbor planets. Therefore, some formation mechanism does in fact exist.


and nearly edge-on orientation, the Bar provides an ideal laboratory for testing PDR models


and a primary target for observational studies of physical and chemical structures of PDRs (e.g.,


At high nb the density profile inside the WS cell extends towards the edge of the cell, pointing out that the WS approximation may be close to its limits of validity


Moreover, higher SFRs could be induced by an increased efficiency of star formation due to the enhanced fragmentation in gas-rich, turbulent, and gravitationally unstable high-redshift disks


Regarding its distance, there are currently two different methodologies based on parallaxes from Hipparcos


Traditionally, bulges were thought to invariably form early-on via


with the disk gradually building up around them.


Whereas this inside-out galaxy formation scenario appears consistent with important integral characteristics of CBs (e.g., their red colors), it does not offer a plausible explanation for the presence of PBs in present-day LTGs.


No fits of these sizedistributions are available, but the figures in


and Price et al. (2010) indicate that the differential sizes may follow a log-normal distribution.


These stellar absorption lines are intrinsically weak in star-forming galaxies, with EW0 typically well bellow 1 Å (e.g.


The general morphologies and the locations of the high-twist fields are also in agreement with many previous studies


discovered that the distributions of X-ray photon spectral indices between RLAGNs and their radio-quiet counterpart are very similar


The location of the star (Teff ≃ 45 000 K, log g ≃ 4.5;


is consistent with a current mass of M∼0.55 M⊙ which implies an initial mass in the main sequence of ∼1 M⊙.


By taking into account the results of the initial qualitative classification by Le Fèvre et al. (2020) and of the more recent quantitative analysis of a subsample of the ALPINE targets by


we proceed with a more in-depth characterization of the [CII]-detected galaxies aimed at obtaining a robust merger fraction at z ∼ 5.


Because they are detected in a wide variety of interstellar sources


it is of prime importance to understand well how these precursor molecules form.


However, it is worth noting that since GRB relativistic blast waves generate synchrotron radiation as they expand into the circumstellar (wind generated) medium


we expect the forward-shock of the afterglow to peak more brightly at 15.7 GHz and at earlier times than the peaks recorded by Chandra & Frail (2012).


We therefore require a higher monitoring cadence at early times (within 5 d post-burst) to detect similar radio peaks.


The high-twist region in our result is also in agreement with


The flexibility in ESPRESSO’s operations has been tackled by adopting a new DFS deployment plan described in


that is exceptional under various aspects because it has to cope with various telescope and instrument configurations while remaining operationally simple.


have shown that the macro model cannot explain the flux ratios in this lens, which suggested the presence of microlensing or dark matter substructures. Thus, to avoid possible biases caused by flux ratios, we only use the lensed quasar positions and the extended arc to constrain the mass model, which is also the standard procedure for H0 measurements in TDCOSMO Collaboration. Ignoring the fluxes of the lensed quasar images will not affect the constraining power of the imaging data, since the lensed arc emission is much more constraining than the lensed quasar fluxes.


The mechanism of gamma-ray emission may be predominantly due to hadronic processes, where relativistic protons interact with gas and subsequently produce gamma rays through neutral pion decay


The initial mass function of first stars is thought to be more or less top-heavy


Theoretical considerations and simulations of MHD turbulence in the presence of a significant background/guide magnetic field suggest that solar wind turbulence can to lowest order be modeled in terms of a combination of a dominant quasi-2D turbulence component of coherent structures (small-scale magnetic islands) perpendicular to the background/guide field and a minor parallel-propagating Alfvén wave turbulence component


a view that is consistent with analysis of solar wind observations


and with the finding that quasi-2D turbulence alone is not sufficient to explain observed solar wind turbulence


Due to different emission zone locations, standard pulsar radiation models include the


By averaging over 222 976 supergranular cells and applying time-distant helioseismic inversions,


found a symmetrical flow in supergranules, which is directed radially away from the centre of the cells to its periphery, with horizontal velocities in the range of 0.3–0.6 km s−1. Their velocity profile is found to increase with increasing distances to the supergranule centre up to a maximum value from where on a continuous decrease for larger distances starts.


Scudder & Olbert (1979) also predict that the halo Ebp/kBTc ratio remains constant with heliocentric distance, whereas


find that the halo Ebp/kBTc ratio decreases with heliocentric distance.


This is crucial since, although space weather forecasting often focuses on estimating the onset and intensity of geomagnetic storms


Previous works in the literature have shown an increase of [C/O] ratios as [O/H] increases (e.g.


but our ratios present a quite large dispersion that together with the shorter range in [O/H] prevents us from seeing a clear behaviour.


Additional followup observations in the optical, near-IR, submm and other wavelengths were targeted at the lensed z = 3.26 source and the foreground objects responsible for the lensing, resulting in detailed analyses of this lensing system by


Theoretical models explain this inefficiency through a combination of mechanisms that provide support against gravitational collapse, including turbulence, magnetic fields, stellar feedback, and dynamical stabilization


In FigureÂ 2, we compare our determination of the stellar surface density fraction to a simple theoretical model and to the best fit of a sample of lens galaxies by


or through dynamical feedback driven by starbursts or active galactic nuclei (AGNs;


The linear separation of the V and 37 GHz emission region can be estimated using the relation


Secondly, the chemical abundance of SF galaxies at z ∼ 2 is lower by 0.1–0.3 dex for a given stellar mass compared to those at low-z


When also considering the central band in rare cases it is plausible to witness multiple-peaked or otherwise complex spectral line profiles (e.g. see the discussions by


This also stresses the need for systemic tracers beyond  Lyα to distinguish IGM signatures and pinpoint the origins of various spectral features.


More recently, unified EoSs for NS have been derived by the Brussels-Montreal group


has also mentioned the well known problem of the “anomalous ions”, that is, the observed high intensities of the Li- and Na-like (as Si iv) ions


Additional searches in the infrared (IR) regime have yielded a few more candidates (e.g.


Several studies show that one can distinguish at least classes of channels, such as isolated binaries and dynamically induced mergers,


as well as the orbital eccentricity at some reference GW frequency


In the sub-Keplerian flow, shocks are formed when the Rankine–Hugoniot conditions are satisfied


This is the most intense emission detected so far from a Galactic GC, again suggesting the presence of a large number of MSPs. However, no direct radio detection of these objects has been obtained so far in this system


Unlike common chemical peculiarities seen in Am and Ap stars, λ Boötis stars are not constrained to slow rotation


Since the PG108.3 cloud consists of three evolved H ii regions, one can thus speculate that the formation of young sources in the region might have been triggered by the expanding bubble. However, our observations largely do not favor such a process because in such a scenario one would expect the distribution of young YSOs or star-forming cores at the outskirts of the H ii regions (see, e.g.,


In contrast, we find that no young Class I sources around S147 and most of Class I sources around S148 are cospatial with the Class II sources located near the center of the ionized gas.


exhibit low-frequency GW emission due to the standing accretion shock instability (SASI


This condition corresponds for CG X-1 to the requirement MBH ≳ 1.5 vw, 10004δ2 M⊙, where MBH is the BH mass, vw, 1000 is the wind velocity in units of 1000 km s−1, and δ ≈ 1 is a dimensionless parameter


In some cases, twisted magnetic flux tubes appear close enough to flow vortices, leading to magnetic and kinetic vortex structures closely coexisting in regions with high plasma-β


Hence, if we assume that FRBs produced by magnetars are created in the magnetosphere close to the polar cap, we can expect them to be significantly beamed


The recent discovery of peculiar highly overluminous SNeIa,


indicates a huge Ni-mass and confirms the highly super-Chandrasekhar white dwarfs, having mass 2.1–2.8 M⊙, as a suitable progenitors


Predicting the amplitude of a solar cycle can be done using solar polar magnetic fields from the previous cycle as “precursors” of the next cycle


Although the chemical retrievals follow different strategies (equilibriumversus free-chemistry), both indicate that a depletion of TiO relative to VO is needed to explain the observed emission spectrum, supporting the earlier findings by


Further support for this interpretation was provided by the findings of stronger impact of large-scale tides on the galaxy spin orientation in denser filaments


using filament density as a proxy for the thickness of filaments


Furthermore, the more clearly an event is identified as a starting track, the more probable it is to be an astrophysical rather than atmospheric background. Down-going atmospheric neutrino events at high energy are likely to be accompanied by muons produced in the same cosmic-ray shower that triggers the veto and reduces the atmospheric neutrino background


However, if this fraction is very low, as required if GW170817 leaves behind a black hole


the fast magnetar model may fail to explain the small fraction of LGRB/SLSN-like hosts in FRB samples.


The general morphologies and the locations of the high-twist fields are also in agreement with many previous studies


Later versions of the model used a more moderately top-heavy IMF in starbursts, triggered by disc instabilities rather than mergers, and found similarly good agreement with the number counts


In particular, we have also used the ML1 (α = 1,a = 1 / 8,b = 1 / 2,c = 24,


tracks, as recommended by Bruzual & Charlot (2003)


propose a scenario where it is the high temperature that is responsible for the HCN enhancement, whereby neutral-neutral reactions with high reaction barriers are enhanced


thus leading to the possible enhancement of HCN and the depletion of HCO+ via newly available formation and destruction paths, respectively.


However, while of course higher gas temperatures are expected in AGN-dominated regions, these are not unique to these environments, as starburst regions and/or regions where outflows dominate can also harbour high enough temperatures for such enhancement to occur. Additionally, the higher temperatures could increase HCN excitation, relative to HCO+ and CS, without necessarily changing their relative abundances


Finally, infrared radiative pumping is also a possible explanation of the HCN intensity enhancement relative to HCO+ and CS. Infrared pumping is a result of the emission of 14 μm infrared photons due to the presence of hot dust around AGN. These photons vibrationally excite HCN to the ν2 = 1 state. Upon de-exciting from this state back to the vibrational ground state, ν = 0, the HCN line intensities are thus pumped to higher fluxes


However, we note that it is also not unlikely that the 12 μm infrared photons can similarly vibrationally excite HCO+, thus nullifying the extent of this effect


Using this method, surveys of star-forming regions with (sub)mm facilities such as SMA and ALMA have determined that protoplanetary disks have typical masses of 0.1%–0.5% of that of their host star (e.g.,


Alternatively, mass transfer rate-related events such as X-ray state changes and disc instability can also cause long-term modulations


Our target locations are not on a major maria and near sites repeatedly observed in previous Earthshine photometry because they were expected to have roughly comparable albedos


The WD companions to Be stars proved unexpectedly elusive


suggest that a baryon-poor outflow can explain the high-energy afterglow emission of GRB 200415A, while a baryon-rich outflow is also viable if the dissipation happens below the photosphere via internal shocks. Therefore, in this paper, we calculate two situations that the ejecta is dominated by electron–positron pairs or protons, respectively.


The density can be expressed in number density of hydrogen atoms (mH = 1.6727 × 10-27 kg), which follows roughly (2)\begin{equation} \label{density} n_{\rm H} = 2.0 \; {\rm e}^{-\frac{|z|}{100\,{\rm pc}}}, \end{equation}nH=2.0e−|z|100 pc,where z is the galactic height


However, as all results show that EII product ion fractions decrease as the complexity of the molecules increases


The analysis, described in detail in Field et al. (2013), is remarkably successful in describing important characteristics of spontelectrics, such as the deposition temperature dependence of the surface polarization charge, including the counterintuitive behavior of solid methyl formate


The disk-wind model suggests that the BLR gas comes from winds produced by the accretion disk


Pioneering work with integral field unit (IFU) observations of four GPs


reveals that two are rotationally supported, with seemingly undisturbed morphology, and two are dispersion-dominated, leading the authors to conclude that mergers may not be a necessary driver of their star formation properties, and by extension, for their LyC emission.


This region exhibits a steeper density gradient in its outer envelope, with qout ≃ −2.5, also illustrated by the cloud structure studied with probability density function


Interesting enough, these two portions of the stream are separated by a very narrow region across which Alfvénicity changes abruptly, from high to low


During the occurrence of X-class flares, the complex AR had shown δ-sunspots, which are identified with a complex distribution of sunspot groups in which the umbrae of positive and negative polarities share a common penumbra


This scenario is strengthened by the recent observations of warm Neptunes at the border of the desert, on the verge of


Instead we believe it to trace the metal-poor gas that acts as a replenishment mechanism of galaxies throughout the universe. It has indeed been suggested that GRB hosts in general are fuelled by recent metal-poor gas inflow


The general dynamics of this process have been studied extensively in purely hydrodynamical simulations


For a warped disc, the binary separation and the mass ratio suggest that M81 X-6 lies in the intermediate instability zone for radiation-driven warping in X-ray binaries (see fig. 1 of


Furthermore, the hard radiation fields in star-forming dwarf galaxies, along with their lower dust abundance, result in extended ionized gas regions prominent on global galaxy scales


In some cases, double relics have been detected on opposite sides of the cluster centre (e.g.,


In these clusters it is possible to constrain the merger history, providing important information about the formation processes of relics.


The mass accretion and loss rates for Class 0/I low-mass protostars span the range of 10−6–10−8 M⊙ yr−1, and the derived jet efficiencies (ratio between mass ejection and accretion rates) range between ∼1 per cent and 10 per cent (e.g.


On the other hand, FRB 20180916B has a nominal RM and has shown a gradual variation in RM value over the two year timescale


Modified Two Stream Instability (MTSI) due to relative drift between reflected ions and incoming solar wind electrons (fast drift), and incoming solar wind ions and electrons (slow drift) has been frequently considered


At low energies they assumed the ENA energy spectra provided by Fuselier et al. (2012). They derived a total pressure of 2.5 pdyn cm−2 in all three plasma regions in the nose of the heliotail


Pressure contributions from the slowed solar wind, magnetic pressure, and the pressure exerted from pickup ions and anomalous cosmic rays all had to be taken into account to obtain this total pressure.


However, it is tempting to speculate that environmental effects from such a rich field could be playing a role in the production of this wind nebula (e.g., triggering of pair cascade by external gamma rays from a nearby source


It is unquestionable that such a unique sample of Cepheids – likely all members of the cluster and at the same distance, chemical composition and age – would constitute a milestone in our understanding of the Cepheid pulsational scenario. Indeed, it offers an unprecedented opportunity to investigate both empirical and theoretical estimates of the luminosity and colour of the pulsating structures and their relation with the observed periods. For this reason, many authors have studied the NGC 1866 Cepheids


in both the optical and near-infrared bands, and have tested different methods to calibrate the PL relations in different filters.


The abundance of real-world applications of ANNs is largely a consequence of two properties: (i) an ANN is capable of closely approximating any continuous function that describes the relationship between an outcome and a set of covariates, known as the universal approximation theorem


Mechanisms suggested to produce these small-scale magnetic helicity fluxes are: advection of magnetic fields by an outflow from the disk through the galactic fountain or wind


Similar results are obtained in studies of individual galaxies at z ∼ 6–8


However, given the low angular resolution of these data, they can not rule out the possibility that one or more merging [C II]-bright satellites are mimicking the smooth gradient observed in the velocity maps


Massive YSO outflows mapped in high-velocity CO lines have collimation factors R = length/width ∼2.05 ± 0.96 as compared to R ∼ 2.81 ± 2.16 for low-mass stars


indicating a weak tendency that outflows associated with massive stars are less collimated than those from low-mass stars as previously thought


The combined detector and telescope PSFs are described in detail in


and the snow line is located at a greater distance from the central star


As a consequence, these planets are most likely formed at greater orbital distances and, due to the shorter disk timescale, inward migration is halted; they thus reach their final position at a relatively large distance from the parent star.


Specifically, we create mock data cubes that mimic ALFALFA observations


Recent work also finds that transient spiral structure


may lead to the formation of moving groups,


Thus, in order to discover all planets in a system, one either needs to image old stars – which seems currently impossible given the already low detection rate around young stars probed by large DI surveys (e.g.,


– or try to minimize the impact of the stellar activity of young stars.


Furthermore, even spherical grains can produce polarized emission by self-scattering of large grains in an anisotropic radiation field


FSRQs have high luminosity and a thin and radiatively efficient black hole accretion disk


Besides RAVE, other surveys have published successive DRs that are available for public use. At the time of writing, there is open access to the DR16 of the Apache Point Observatory Galactic Evolution Experiment (APOGEE;


The user defined heating is therefore highly stratified, spatially smooth and steady (e.g.


is interesting because of the presence of a Saturn mass planet in a similar orbit to 55 Cancri.


The innermost planet lies just outside a pair of secular resonances at 3.0 d (eccentricity) and 3.4 d (inclination) and so is consistent with a lack of inclination excitation. If we allow for the existence of a 1 M⊕ planet interior to this, eccentricity resonances are found at 0.9 and 2.1 d (and a mean motion resonance at 1.9 d) and inclination resonances at 1.2 and 2.1 d. Thus, a planet that has tidally migrated to orbital periods 2 d in this system could have had its inclination pumped up and have avoided transit.


We expect to detect the GWB first, followed by detection of individual SMBHBs


In particular, the damping behavior of a large plate or surface is expected to differ from that of a same-sized particle, so that the velocity dependence of the coefficient of restitution might be an effect of the experimental setup in


Strong non-potential field arcades have been observed in hot X-ray sigmoids on scales of hundreds of arseconds


This range of lengths over a range of temperatures and magnetic field topologies points directly to self-similar mechanisms influencing plasma and magnetic field dynamics at a range of scales.


Absorption coefficients for pure water ice (kH2O) at sub-mm-to-cm wavelengths are discussed extensively by


who also provides several analytic formulations to estimate them as a function of frequency and temperature along with illustrative plots.


This trend is in agreement with the metallicity dependent yields from


which provide higher carbon as [Fe/H] increases from massive stars (i.e. also increasing the O production) but lower carbon from low and intermediate mass stars as [Fe/H] increases (i.e. less production of C).


show that the retention of BHs in dense stellar clusters of wide mass range, beginning from low-/medium-mass young and open clusters


comprise environments where BHs can pair up through close dynamical interactions, which, furthermore, lead to general-relativistic (hereafter GR) coalescences of these BBHs.


We note that in our calculations, we assume a source size that is 1.8 times larger than the FWHM, following the approach of Readhead (1994) and


We followed the second approach since there are natural thermal instabilities in the plasma, such as instability caused by X-ray irradiation


The abundances of these rare but massive subhaloes has important implications for, among others, the statistics of massive satellite galaxies (e.g.


The prior mean functions that we discussed are the following: zero mean function, the theoretical function of angular size calculated from the angular diameter distance under the assumption of three cosmological models: flat ΛCDM with Ωm = 0.27, so-called Rh = ct universe


A cross-correlation method was applied to derive continuous 2D speed maps of a CME from coronagraphic images by