investigated the sizes of particles smaller than 10 μm that impacted the aluminum foils of the Stardust probe. The distribution peaks at about 175 nm, but if we assume that the particles areagglomerates of smaller subunits, as indicated by their common polymineralic nature, then the subunit size distribution would peak at sizes below 100 nm


while the models with higher He core masses are compatible with the typical kicks of young pulsars


A more realistic shock process, on the other hand, is most likely accompanied by radiative cooling to some degree in which the post-shock plasma temperature may stay comparatively as cool as that of the upstream one, as in the isothermal shocks (e.g.,


It has been pointed out that the widely used approximation for the vertical component of gravity, GMz/R3, is only valid for the thin disk with H/R ≪ 1, and a more accurate expression of vertical gravity should be adopted for a slim disk


Because they are detected in a wide variety of interstellar sources – in hot cores


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


The points mark detections from previous studies in the literature. References:


All relevant numerical routines were extracted from the LLMODELS stellar model atmosphere code


Nevertheless, the ‘combined’ bar fraction in Fig. 6 is not constant over (g −r) colour and agrees well with


for redder colours [(g −r) colour > 0.5]


The flux variability of the source rules out an X-ray supernova remnant and confirms that it is powered by accretion onto a compact object


we employed the RAM36 (rho-axis-method for 3- and 6-fold barriers) code that uses the RAM approach for the molecules with the C3v top attached to a molecular frame of Cs or C2v symmetry and having 3- or 6-fold barriers to internal rotation, respectively


Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S ii]/H α > 0.4–0.5


In some galaxies, the depletion time in the centres appear shorter


In 2018, a new technique combining a Terahertz radiometer (41–49) GHz and a vacuum chamber was developed to observe the generation of cold plasma and UV photochemistry in the gas phase under low pressure as described by


However, in the context of the experiment described here, it is important to note that the spectrometer developments were not coupled to a system where the gas-phase molecules originated from the solid state.


Pebble accretion is a mechanism able to speed up significantly the giant planet formation process (i.e.,


A whole host of ions, atoms, and molecules have been detected through a variety of, often complementary, techniques, such as differential spectrophotometry using low-to-mid resolution spectroscopy (e.g.


Historically, models reproducing the evolution of stellar populations and dust emission have been developed separately,


and a thorough comprehension of dust grains physics on the other


Velocity dispersions in dwarf galaxies can be on the order of the rotational velocity, ∼10–15 km s−1 (e.g.,


Orbiting SMBHBs produce a stochastic GW background (GWB


On the numerical side, van Wassenhove et al. (2010) consider different scenarios for formation of a black hole in Milky Way satellites and place the likelihood of one of them having a black hole around the size found here to be below 1%, but this result also depends on the initial seed mass (see also


In particular, an instrumental line (Cu Kα) is known to affect pn at a rest-frame energy of ~8 keV


Despite our efforts to carefully estimate the background, that line might interfere with the Ni-K line in several observations, making a proper modelling of the Ni-K line impossible, and hence, boosting the Ni absolute abundance in pn.


Since then, these two methods have been widely used to explore the cosmic anisotropy


by investigating observational data of, for instance, the Union2.1 sample


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


The blue bump appears mainly due to the presence of late-type WN (WNL) and early-type WC (WCE) stars


The M-type sample consists of the non-Mira stars from the General Catalog of Variable Stars (GCVS;


with quality flag 3 in the IRAS 12, 25, and 60 μm bands and 60 μm flux ≳3 Jy


This model features a self-consistent treatment of the thermal, Compton scattering and the reflection component: ${\tt {\rm kerrbb2}}$ describes the thermal component and supplies the seed photons for ${\tt{\rm simplr}}$ (a modified version of ${\tt{\rm simpl}}$,


while the post-shock temperature in the hot halo near Rv may only be ∼0.5Tv


It is worth noting that the original samples from


and Bernard-Salas et al. (2009) have spectra solely covering the central region of the galaxies.


The center-to-limb variations ofintensity I(μij) and polarization P(μij) were found through trilinear interpolation using the look-up tables from Kostogryz & Berdyugina (2015) and


, according to the selected wavelength, surface gravity, and temperature of a star.


will be a 3-km-long underground interferometer in Japan capable of detecting the gravitational radiation emanating from collisions involving black holes with masses up to 200 M⊙


We then attempted to unify the data for each filter to a consistent zero point by using ensemble photometry


This essentially uses all measured stars on the frame to determine magnitude offsets resulting from differences in exposure time, airmass, atmospheric transparency, and the like. Our implementation iteratively fits for position-dependent corrections that result from variations from point-spread function across the frame.


Aa is itself composed of two spectroscopic components (Aa1+Aa2) in an eclipsing orbit with a5.7325 d period, while Ab is two magnitudes fainter than the two Aa components and located 0.′′ 267 away in 1993 and moving away from the primary


We also plot the SFR in the outer regions of spiral galaxies


This unprecedented relation is likely the result of the observed link found between SF indicators such as radio, far-infrared, optical or line luminosities, and galaxy mass


Such shadows reveal that angular distortions are common in inner disks. This is consistent with the existence of a class of self-shadowed disks in which the inner disk scale height is higher than that of the outer disk, leading to a general shadowing and related cooling of the outer disk


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.


These measurements are within the range predicted by the magnetohydrodynamic jet launching models


On larger scales or for measurements invoking substantial temporal and/or spatial averaging, the distributions become gyrotropic but can still remain anisotropic, since isotropization may be slow. The corresponding RH should take into account this anisotropy


For example, shown in Figure 1 are the values of symmetry energy at 2ρ0, that is, Esym(2ρ0), from


analyses of NS radii, tidal deformability, and maximum mass within an extended Skyrme Hartree–Fock approach (eSHF)


Despite the rather different assumptions and methods used in analyzing the different types of laboratory and observational data, it is very interesting to see that they all together are consistent with a fiducial value of Esym(2ρ0) = 47 MeV within the still relatively large error bars of the individual analyses.


A second, fast path involves a downward transition in the mass–size plane, at approximately constant redshift


This process requires a substantial “compaction” of the formally extended star-forming galaxies.


In LTE, a linear dependence of the core/wing ratio is expected (e.g.,


but such dependence is probably less obvious for the Mg ii h and k line, whose cores form in NLTE conditions.


Weaker solar cycles and advanced imaging and modeling capabilities have raised the profile of pseudostreamers and their boundaries as contributors to the outflows within this slow wind layer


Plin represents the real-space, linear matter power spectrum for which we use the CLASS Boltzmann solver


When random pairing is used (i.e., binary companions are randomly chosen from a given IMF), we find similar mass segregation results to those for star clusters containing only single stars. However, random pairing is ruled out observationally, and there is also a lack of theoretical backing for a random pairing function


It has a (energy-dependent) angular size of ∼0.1° and its distance has been estimated to be ≈2.2 kpc, corresponding to a physical size of ≈3.8 pc


At large galactocentric radii (>10 kpc) this includes, among others,


and streams of stars kicked up from the disk that undergo phase mixing, sometimes referred to as “feathers” (e.g.,


with a sample of 322 giants, including 10 planet-hosts, did not find any metallicity offset.


Bars in spiral galaxies may drive gas inflows, which enhance central star formation (bar-driven evolution;


found that CIR boundaries can be well defined when the total pressure exceeds 50 pPa (indicated by the horizontal dashed line in Fig. 2), which is slightly higher than that in the background solar wind, which typically is 20−30 pPa, according to Jian et al. (2006).


Within the classical MOND framework, the Newtonian gravitational acceleration gN is replaced in the spherically symmetric case by $g=\sqrt{g_{\rm {N}} a_0}$ when the gravitational acceleration is far smaller than the critical acceleration a0 = 1.2 × 10−10 m s−2


Different types of software, such as lenstronomy


can handle the inference of lensing quantities from mass maps using fast Fourier transform convolution.


As mentioned in Sect. 5.7, the 13CO/C18O abundance ratio increases in regions of enhanced UV field


This category is similar to the ‘uncertain’ (UNC) class introduced in


that, based on the results of the 3DBarolo fits, contains sources they are unable to classify because of the low S/N and/or spectral resolution, or contrasting evidence in their classification criteria.


An additional goal of high-resolution observations for L1451-mm and the remaining youngest candidates should be to investigate the temperature and density profiles of the envelope at scales from few au to 100 au. This is because simulations show that the temperature remains lower than ∼30 K even at several tens of au up to 100 au from the centre


The quality and breadth of these experiments are limited by the availability of computational resources and the fidelity of models for galaxy physics such as


It has only recently become widespread to model the formation of galaxies ab initio


It was the first source identified as a hot corino


based on the detection of Complex Organic Molecules (COMs) in the source, which was later supported by follow-up studies


revealed that the excitation is probably due to the κ − γ mechanism, acting mainly in the zone of the second partial ionization of He, with a weaker contribution from the region of the first partial ionization of He and the partial ionization of H.


Surprisingly, we observe that this data reduction change was only applied to the Balmer β, γ, and δ lines but not applied to the Balmer α line. For the latter one, the original iterative spline interpolation scheme has been used all along. As a result, an absorption-like feature at the location of Balmer α is found in SDSS data releases 9 up to now, i.e. the latest data release 14


It is more similar to the extremely low values of [14N/15N] found in primitive solar system material, like cometary CN and HCN


More importantly, we showed that, as long as the archives are consistent with each other, for example, they are centred at the same wavelength and employing the same bandwidth for the observations, the method can be used to derive accurate information on the evolution of plage areas without the need of any adjustments in the processing of the various archives


The energetic plasma in the vicinity of RFs plays a key role in connecting the magnetotail with the inner magnetosphere because they carry a large amount of energy and can be injected into the inner magnetosphere to affect the ring current and radiation belt


The most well-known stellar stream in this region is the Monoceros Ring (e.g.


while the baryon content is revealed by emission lines ranging from H and He lines in the optical through to highly ionized Fe lines in the X-rays


These values are consistent with the current observed SFR in the Milky Way


The tidal disruption probability of NSBH mergers and the brightness of NSBH EM signals are determined by the BH mass, BH spin, NS mass, and NS equation of state (EoS; e.g.


This UV-soft SED is regarded as more realistic for radio-quiet quasars than the other available SEDs provided by Cloudy (see the detailed discussion in Section 4.2 of


Usually, we see a decay in magnetic field strength as solar-type stars evolve, as their activity decreases along with their rotation


However, this subgiant star seems to have a relatively strong large-scale magnetic field compared to the Sun. The exact process through which this star would reach this stage in its evolution with such a magnetic field is yet unknown.


showed that, in order to have a significant feedback impact in the environment surrounding an AGN, it is required a minimum ratio between the mechanical power of the outflow and the bolometric luminosity of ${\sim}0.5{{\ \rm per\ cent}}$.


Instead, the lower limits are below the minimum value required to generate at least a weak feedback. Considering only the values derived from the lower limits on the distance, i.e. the situation in which the X-ray winds are cospatial, we would be in a scenario in which the source loses much luminosity due to advection inside the disc, resulting in a much lower efficiency for wind production as most of the radiation remains trapped inside the disc.


For a sanity check, we estimate the bulge mass of NGC 3504 using our H-band MGE model and adapting the effective radius of the bulge derived from the bulge-disk-bar decomposition model


However, previous results show that fast CME would decelerate during their propagation in interplanetary space (e.g.,


Moreover, several molecules were detected and resolved toward NGC 1068 with interferometers in the past few years


The Fκ-test is preferred when the magnitude difference between the object and comparison stars is large


The corresponding range is depicted in Fig. 6 by the horizontal bar shaded in blue. As thevolume filling factor is known, the laboratory measurements can be used to determine the most likely material of the surface.


are at the levels of >4σ for the analysis of


Multiple feedback mechanisms influence disc evolution. In sufficiently dense environments, star–disc encounters can truncate the disc and induce increased accretion rates


Accordingly, numerous studies were focused on peak fluxes of SEPs and corresponding acceleration and transport processes (e.g.,


A process that constrains the outcoming radiation field to narrower angles may leave some room for the accretion process to continue in some directions. This seems to be the case for the outflows driven by young stars from a very broad mass range, as previous reported by several authors


VLA observations of the NH3 inversion lines (1, 1) and (2, 2) seen in absorption (1\hbox{$\farcs$}.̋1 beamsize) revealed radial infall on scales larger than 5000 AU toward the W51e2 core


The RXTE observed another outburst in 2002 and re-established its cyclotron resonance feature corresponding to a centroid energy at 30.7 ± 1.8 keV (as established earlier by Ginga), which did not show a significant dependence on X-ray luminosity, although the continuum became harder with increasing source luminosity


QSO flux measurements that reach to z ∼ 7.5


the absorbed doses used in our fixed energy experiments change from ~ 2 to ~ 15 MGy, whichis quite similar to the absorbed doses in


In the linear perturbation theory limit of the MHD equations, δB2 includes contributions from shear Alfvén, fast and slow magnetosonic compressive eigenmodes (e.g.


We do detect starburst-like behaviors in galaxies on the main sequence


likely linked to the existence of transitional objects


to limit the references to recent works based on submillimeter observations


However, implementation of these models is complex and a large library is needed to model all galaxies properties. Instead, numerous studies have used simple analytical forms to model galaxies SFH (e.g.,


This limit is referred to as the quasi-static approximation to MHD


although recent numerical studies on its turbulent properties and anisotropy have been done as well


Reconstruction techniques are divided into two classes, although this distinction is by no means unique or even consistent in some cases. Parametric techniques (e.g.


assume a parametric form of the underlying mass density distribution for the lens and typically make the assumption that light traces mass in the positioning of these parametric forms.


In particular, the Magnetospheric Multiscale (MMS) mission has contributed greatly to the kinetic physics of magnetopause reconnection


With the remarkable progress in scientific computing, their rotating magnetosphere has captured designers of numerical methods that integrate FFE and magnetohydrodynamics (MHD) with ever-improving accuracy (e.g.


Presently, although we still know little about rotation velocities of massive stars and their variation with environment, observations seem to favor fast rotators at low Z (e.g.


The possible change of macroscopic magnetic moment of pulsars at the moment of a glitch occurring was discussed by Link and Epstein


where time, radius and velocity are normalized to the outer radius a, the resistive diffusion time τR = a2/μ0η, and the Alfvén velocity $V_{\rm A} = B_0/\sqrt{\mu _0 \rho _0}$, respectively.


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


Unfortunately, the previous work does not cover all the phase angles of the images we investigated, but the spectral slope variation between 35–54° (Fig. 3 of


is small so that we can make this comparison. However, if we follow the linear trend of the phase reddening, for the image taken in 70.45° phase angle (image #4), the spectral slopes would vary from 15%/100 nm to 18%/100 nm in the observations we used.


Most of the known metal-poor stars have been found in dedicated surveys, such as objective prism surveys (the HK survey and Hamburg-ESO survey


These motivated an effort to measure the neutron star radius using the burst continuum spectrum, where the normalization of the burst blackbody is expected to be proportional to the square of the stellar radius (e.g.,


(ii) the disruption of a monolithic object due to excessive spin-up resulting from non-gravitational forces or YORP5 effect followed by a reaccretion


If the pairs are produced via TeV–eV collisions (i.e., via the second path) outside the gap outer boundary, they have outward ultrarelativistic momenta to easily “climb up the hill” of the potential k0


see also Figure 2 of HP16) and propagate to large distances without turning back.


Considering that the relation between the gas temperature and the para-H2CO line ratio may vary at different spatial densities (see Fig. 2 in


we modeled it at spatial densities 104, 105, and 106 cm−3 in Fig. 5.


Moreover, the Te problem can also be originated due to the use of an unappropriate calculation of the ionization correction factor (ICF) for oxygen in AGNs


The models for galaxy formation include physical processes such as gas heating by a spatially uniform and time-dependent UV background, primordial and metal-line gas cooling, a subgrid model for star formation, and the unresolved structure of the interstellar medium


The blue squares are data from the GAMA galaxy survey


We probed four orientations for the simulated outflows


For a few very nearby (100 Mpc) quiescent galaxies, including our Galaxy, SMBH masses can be measured through the stellar or gaseous dynamics method (e.g.


Because it is difficult to determine the cut-off energy from our data, we fix it at 300 keV, which is a typical value measured in nearby AGNs


For example, the enhanced close binary fraction of metal-poor solar-type stars substantially strengthens the conclusion that the shaping of PN morphologies is the result of binary interactions


When the magnetic field lines are parallel it is not easy to have reconnection


Hereafter, we adopt natural units c = ℏ = 1. have been reported (see, e.g.,


There remains much debate in the literature on the origin of such axisymmetric substructure in protoplanetary disks including


and toroidal dust traps created by hydrodynamic or magnetohydrodynamic effects (see, e.g.,


The existence of an early ocean is supported by


and from records of the oxygen isotope composition of seawater


also saw highly structured material most probably originating from a prominence in 63% of CMEs associated with eruptive prominences at the limb observed in visible light using the broadband filter (λλ 5000−5350 Å).


Although such observations are called as white light in literature, it would be better to consider them as observations in visible light, because naturally integral intensities in the visible spectral range are observed including both continuum and absorption lines, while white light is just a continuum caused by Thomson scattering on free electrons without the lines.


This cluster has about solar metallicity ([Fe/H] in the range −0.04 to +0.03, e.g.


Nevertheless, it still faces numerous challenges on galaxy scales. Among these, the most important ones are


or the unexpected diversity of rotation curve shapes at a given mass scale


While the PHIBSS project estimated molecular gas masses by measuring the CO(3–2) line emission


Scoville et al. (2016, 2017) used the flux on the Rayleigh–Jeans tail of the dust continuum emission to estimate the total gas masses.


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.


This is quite a difficult measurement to do in observations as light profile fitting is required, which can be robustly done in very disc- and bulge-dominated galaxies, but when both components contribute similarly, the measurement is less robust


Set II: we now focus on the observational constraints on the model parameters after the inclusion of the local measurement of H0 by


with the previous data sets (CMB, Pantheon, and CC) in order to see how the parameters could be improved with the inclusion of this data point.


When the relative fraction of RC stars is taken into account (27%; see Section 4), the difference in [Na/Fe] between the genuine RC stars would correspond to Δ[Na/Fe] ∼ 0.20 dex, which is comparable to that expected from our chemical evolution model for the bulge stars (Δ[Na/Fe] = 0.2 ∼ 0.3 dex;


As an example, it has been known for several decades that the Galactic disc contains large-scale non-axisymmetric features, including


In low radio states, it has also displayed evidence of a high-ionization X-ray-absorbing wind


estimated with NEXAFS spectroscopy (at the C K-edge) that X-ray irradiation at 150 eV of pure methanol ice at 20 K leads to a survival rate of 50% for methanol after an absorbed dose of 1.1 MGy.


However, the complexity of such simulations obscures the physical mechanisms through which these processes affect the dark matter distribution. These mechanisms normally invoke ‘heating’ of the cold central density cusp through an irreversible process, such as dynamical friction from infalling clumps


In the jet model, such a p can also reasonably account for the very late flux decline of


While this parameter space is inhabited by Uranus and Neptune in the Solar system, which should thus readily supply objects to the Oort Cloud (even accounting for the possibility that these planets may have started closer to the Sun;


it could be that Oort Clouds are relatively rare.


The first possible scenario is that all FRBs are generated from magnetars, the population of non-repeating FRBs are from magnetars born in the delay formation channels


This result strengthens the notion that metallicity may not play an important role in deciding theresulting SN type, in agreement with other works based on SN environments


Absorption band shifts of CO ice in the UV and IR ranges only occurred at deposition temperatures above 20 K


suggesting that CO ice grown at lower temperatures is amorphous below 20 K in our experiments, and therefore, the decreasing photodesorption yield is not related to a transition from amorphous to crystalline ice, instead it might be associated to a different degree of molecular disorder in CO ice samples, depending on their deposition temperature.


One is evaluated from the best-fit model, and one weights all models allowed by the parametric grid, with the best-fit model having the heaviest weight


the nuclear masses for the outer crust were provided by an early semi-empirical mass table.


The corresponding EoS is seen to display a similar pattern with the BCPM, FRDM, and BSk21 results in Fig. 2.


These soft residuals are known to be a common feature in the spectra of ULXs and bright X-ray binaries


and found in other ULXs to be a combination of emission and absorption features related to powerful outflowing winds (including in NGC 6946 ULX-3;


Modelling of DLAs observations suggests that DLAs resemble rotating disc galaxies with circular velocities typically of the order of $100\!-\!200\, {\rm km\, s}^{-1}$


, on the other hand, show that the (nh + ns)/nc ratio remains roughly constant with heliocentric distance in the slow wind, suggesting a lack of interchange between the thermal and suprathermal populations.


These three protostars are all embedded in dense cores with masses ≳0.5 M⊙


Therefore, they are excellent targets by which to study the gas motions on a 100 au scale at an early evolutionary stage.


In observed spectra, recurrent frequency spacings that may correspond to the large separation or half its value have been found in some stars


Comparisons of the two methods show quite good agreement and reasonable agreement with the full quantum calculations is found, particularly for the most important processes with the largest rates


However, our result is consistent with other NLFFF results


The composite SED was reddened according to the new family of optical and near-infrared extinction laws for O-type stars provided by Maíz Apellániz et al. (2014), which constitute an improvement of the widely used extinction laws by


For instance, thioformic acid (HC(O)SH) was very recently detected in G+0.693–0.027. Its trans-isomer has an abundance of ~1 × 10–10


Studies showed that the majority of the optically visible Galactic post-AGB stars could be classified based on their spectral energy distributions (SEDs) into two groups: shell-sources and disc-sources


Studies suggest that this valley likely marks the transition from the smaller rocky planets: ‘super-Earths’, to planets with significant H/He envelopes typically containing a few per cent of the planet’s total mass: ‘sub-Neptunes’ (e.g.


Spacecraft observations show that wave potential structures of Gaussian form are common in space and astrophysical plasmas


We assume this potential well to have Gaussian form


Super-Earths can be found with either high-precision RV observations or space-based transit searches. Such high-precision RV surveys include those being undertaken currently with HARPS (e.g.,


The signature of flare QPPs can be detected in flare light curves across a broad band of the electromagnetic spectrum, i.e., radio/microwave emissions


For cometary nuclei, the primary cause for spin-up is torques caused by outgassing, therefore it is possible that 8P/Tuttle formed as a monolithic body and became a contact binary after its injection into the inner Solar System as a result of excessive spin-up resulting from non-gravitational forces. This scenario has been proposed for comet 67P/Churyumov-Gerasimenko by


Such transition might well imply an imminent increase of the SFR, driving the object in the realm of starbursts


or its cessation, bringing the system back onto or even below the main sequence


with the CO properties potentially able to distinguish between these two scenarios.


The complex dielectric functions of the samples obtained by heating bayerite and boehmite to various temperatures


were derived by modeling the reflectance spectra of pellets obtained by pressing powders of these materials under great pressure


The avoidance of its going into CE evolution is – as we will argue – a consequence of the donor star having a radiative envelope


In such a case, when the emission beam is confined by dipolar open field lines, we would expect a P− 1 / 2 dependence, which has indeed been observed when correcting for geometrical effects by transforming the pulse width into a beam radius measurement (see


This effect has been considered in numerical models of GCR modulation to study the long-term modulation mechanism (e.g.,


Over the past decades, much effort has been devoted toward constructing such global NLTE, steady-state model atmospheres of hot stars with winds; several numerical computer codes meanwhile exist on the market, for example


This is not an ideal approach: the momentum imparted on the SMBH from the swallowed gas particle may artificially dislodge it from its position, particularly without instantaneous repositioning (as also discussed by


However, even in ellipticals, large differences prevail. Recent observations of elliptical galaxies with Spitzer and Herschel


have revealed that the far-infrared (FIR) luminosity LFIR from these galaxies can vary by ∼100 among galaxies with similar optical luminosity.


Some of these bursts are still not well understood. This is a case of the slowly positively drifting bursts (SPDBs). They appear in groups or as single bursts, with a duration of an individual burst from 1 to several seconds and their frequency drift is lower than about 100 MHz s−1


Such a distribution is believed to be related to the mass of the hydrogen envelope maintained by the progenitor stars, as evidenced by the results that SNe having larger envelope masses produce light curves with shallower plateau slopes and longer plateau durations


Several explanations about their origin have been put forth. Among these theories, interchange reconnection is the most focused upon


In this scenario, switchbacks are generated in the solar corona, and form at the reconnection sites between open and closed magnetic fluxes.


have revealed small non-mass-dependent variations in Fe isotopes.


This relation has been further extended to high redshifts, using deep near-infrared (IR) spectroscopy facilitated by large ground-based and space-based telescopes


The early X-ray afterglows are usually dominated by erratic X-ray flares and the tail emission of prompt gamma-rays are due to the arrival time delay of photons in the high latitude of the radiating fireball


Toward this goal, conventionally, new summary statistics that can only be measured with imaging have been proposed. These include


The [C ii]158 μm line is typically the brightest in star-forming galaxies, arising from ionized, and even neutral gas where it is the main coolant


In addition, an intermediate-mass black hole (IMBH) in a cluster core will act as a strong central energy source able to delay, or even prevent, core collapse (e.g.


Moreover, it was found that the highest dust temperature at which H2 can be formed efficiently is less than 17 K


Recently, magnetic fields have been unambiguously detected via Zeeman signatures in a large sample of single G-K giants observed with the spectropolatimeters TBL/Narval and CFHT/ESPaDOnS


Gravitational lensing allows for constraints to be placed on the dark matter substructure content of external galaxies, as orbiting sub-haloes will result in anomalies in strong gravitational lenses


Whilst this higher total disc mass is still consistent with the dust mass measurements of protoplanetary discs


high debris disc masses, i.e. those in the range of $100\!-\!1000\, M_{\oplus }$, become problematic since these would require a very high efficiency of primordial dust being incorporated into these larger planetesimals (an example of the so-called ‘disc mass problem’, see


The (CH2OH)2/CH2OHCHO abundance ratio of ~0.3–0.5 previously derived in IRAS 16293 by


Some studies find weak statistical links among AGN activity and the presence of bars (e.g.,


An exponential rise/decay model can appropriately fit the blazar light curve, which generally consists of superpositions of a steady background flux density and a number of flare components caused by events in the jet or the accretion disc/corona region (e.g.


BALQSOs are classified into three sub-classes based on the ionization state of the absorbing gas: (a) high-ionization BALQSOs (HiBALs) consist of absorption from high-ionization lines such as C iv, Si iv, and N v


The sample used in this paper is primarily drawn from Sloan Lens ACS Survey (SLACS)


The combined sample includes 91 lenses from SLACS


Using Ks-band (2.15 μm) direct imaging andH-band (1.65 μm) polarimetric imaging with the High-Contrast Instrument with Adaptive Optics (HiCIAO) at the Subaru Telescope,


detected two spiral arms and polarized light down to 0.′′ 1 (15 au) from the star.


Second, the mass distributions of single and binary sdB stars are indistinguishable (


The choice of SED is very important in the BLR modeling, as different lines respond to the continuum variations on different time scales


Previous sub-arcsecond angular resolution N-band (∼8–13 μm) ground-based spectroscopic studies investigated the 11.3 μm PAH feature in the nuclear and circumnuclear regions of AGN (e.g.,


However, these works were unable to provide definitive details regarding the effect of the AGN on the PAH molecules due to limited wavelength coverage and sensitivity.


we estimated several dynamical properties of the clusters in the point source sample and compared them with the extent-selected sample presented in


Between the end of inflation at t = te ∼ 10−33 s; (e.g.


and t = teq = 2.37 × 1012 s, the Universe was radiation-dominated since at the latter instant a radiation-matter equality is reached (Table 1).


Furthermore, discoveries of atmospheric chemical species allow us to better understand various thermodynamical processes and chemistry, winds in the upper atmosphere


The observations of NGC 1333 IRAS4A and IRAS16293 are presented in Girart et al. (2006) and


Together, these properties lead to the result that an ANN can be trained to provide accurate and practical solutions to Newton’s laws of motion, resulting in major improvements in computational economy


There are various observations of flux ropes in the


At 8.7 GHz we find a PA of 25° ± 5° at about 5 mas from the core, consistent with the archival VLBA monitoring results at 15 GHz, showing a persistent jet orientation at a PA of about 30° in the epochs from 1995 to 2013 at angular scales ∼5 mas


Magnetic field fluctuations have been characterized with great detail at magnetohydrodynamic and kinetic scales, for example, through spectral and high-order moments analysis


Besides the GRB 170817A/AT 2017gfo event, searches for possible kilonova emission have already been carried out in the afterglows of many SGRBs since 2013


The large scale outflow is observed in CO emission at millimeter wavelengths, with both the red and blue lobes being about 100″ in extent


In this very region, the analysis of heliospheric imaging (HI;


has described a transition from striated images that appear to be highly collimated due to a structured magnetic field and lower plasma beta to higher altitude images that appeared to be more disordered and isotropic, a condition described as “flocculation.”


Such a massive secondary black hole would require the Milky Way to have experienced a major merger relatively recently, which is excluded by observations (see


Those cavities have been suggested to exist at ∼pc scales at least for XTE J1550–564 and H1743–322


Compared with other short GRBs, the luminosity of GRB 170817A was extremely weak, thus suggesting that the jet was off-axis to the line of sight


There are a variety of theoretical works related to the damping of the coronal loop oscillations based on the theory of resonant absorption of MHD waves (e.g.,


Alternatively, small dense structures can be temporary density fluctuations frequently created and destroyed by supersonic turbulence (e.g.,


We note that some of our data fits the observational findings of


represented by diamonds over-plotted on the power spectra


The agreement of the theory with the observational data indicates that the results can be used to determine the background structure of the solar atmosphere and confirms that wave generation by the solar granulation in the partially ionized plasma dominates the behavior of the waves.


In the absence of QED vacuum polarization effects, this would produce a drastic depolarization of the radiation collected at infinity


This could stem from the fact that the galaxies studied by Holt et al. (2011),


are local luminous or ultra-luminous infrared galaxies (U/LIRGs), and those of Villar Martín et al. (2014, 2015) are highly obscured Seyfert 2, thus sampling sources that are more gas and dust rich compared to our sample.


We do detect starburst-like behaviors in galaxies on the main sequence


likely linked to the existence of transitional objects


Eventually Philippov & Spitkovsky (2014) computed the first two-dimensional axisymmetric pulsar magnetosphere for an aligned rotator by permanently injecting particle supposed to be released from the surface, avoiding to end to an electrosphere configuration


This chemical scheme was implemented in a chemical model by


to explain the abundance of cyanoallene in TMC-1.


The soft X-ray region of the reflection spectrum is also the most sensitive to modelling assumptions such as vertical disc structure


The in situ formation of the compact blobs is further supported by their metallicity. In fact, while the disc properties are consistent with the stellar mass–metallicity relation of z ∼ 2 star-forming galaxies (e.g.


compact blobs instead show metallicities inconsistent with the mass–metallicity relation (Fig. 7, bottom right panel).


However, the mean length for QS network jets is smaller (3.53 Mm;


Because of the potential diffuse nature of the excited states, their wavefunctions were calculated using a large basis set composed by the aug-cc-pVQZ quality, which is augmented by 3s and 2p diffuse Gaussian-type orbitals (GTOs;


Figure 5 shows the comparison between our EWs measurements and the line strengths measured by


(in both cases the sum of the two strongest lines) for the five calibration clusters.


The observed scatter is consistent with the internal errors of the EW measurements,


Note that any changes in the nearly flat potential will eventually lead to certain features in the spectrum. Local glitches in the potential including rapid change of its amplitude, or the break in its first or second derivatives


all lead to local and non-local oscillations in the spectrum.


Locally, less than 5% of the galaxy population has a star formation rate (SFR) that is significantly higher than the empirical main sequence for star-forming galaxies, i.e., the tight correlation (∼0.3 dex) between the SFR and stellar mass, M⋆


In a shearing disc, if the cells adapt in a truly Lagrangian manner, then they are inevitably deformed into a highly sheared/irregular shape


Several strong processes have been proposed and observed, such as harassment (e.g.


Both giant HII regions are projected on the contour of a giant bubble-shaped structure, outlined in the distribution of HI and CO emission as first noted by


noted the presence of O and early B stars in the area and proposed that they were part of a massive star population responsible for having caused the bubble, but a review of their properties shows them to be generally too bright to be at the distance of the bubble and the giant HII regions, and instead are more likely members of a foreground population.


If the cirrus ISM component heated by the more general galactic UV radiation field contributes to LIR, then the


We then remove the cosmic rays using the LACosmic algorithm


However, sensitivity and resolution limitations severely reduce the effectiveness of the past and present generations of radio and X-ray searches for SNRs in galaxies beyond the Small and Large Magellanic Clouds (MCs)


These slopes essentially provide information on the relative amount of structure as a function of spatial scale and can be compared with theoretical models of turbulence (mainly numerical simulations) to characterize turbulence cascade (e.g.,


Two orange peaks represent the cool lines of O I 1354.60 Å and C I 1354.84 Å


which are far away from the flaring line of Fe XXI 1354.08 Å.


A CO spectroscopic redshift of 3.26 was first suggested by Z-spec


observations, then subsequently confirmed by observations


The most stringent and precise constraints on the self-interaction cross-section have been put on the scales of galaxy clusters (e.g.


where observations require that $\sigma _T/m_chi \lesssim 1\, {\rm cm^2g^{-1}}$.


This form of joint analysis is already being explored within the framework of WMAP


in combination with Planck Low Frequency Instrument data


Moreover, in recent years evidence has grown supporting the statement that GCs are generally composed of two or three chemically distinct populations. These subpopulations are separated by a few tens to hundreds of Myr in age and show vastly varying abundances of light elements such as C, N, O, Na, Mg, and Al (see, e.g.,


Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S ii]/H α > 0.4–0.5


We adopt a four-level AR classification scheme based on the maximum GOES-level flare an AR ever yields


Al i lines at 6696 and 6698 are used for deriving the Al abundance and these lines have negligible contributions from NLTE effects


we found clear evidences of pulsation phase variability with a maximum change of 2 × 10-3 c/d. In other words, as an example after one year time a phase-constant model would appear to have the correct shape with respect to the pulsation pattern of the star, but shifted several minutes in time.


The dust radiative transfer and photosionisation code mocassin


was used produce the temperature parametrization. The atomic data base of the mocassin code included opacity data from Verner et al. (1993) and Verner & Yakovlev (1995), energy levels, collision strengths and transition probabilities from Version 5.2 of the CHIANTI data base (Landi et al. 2006, and references therein) and hydrogen and helium free–bound continuous emission data of Ercolano & Storey (2006).


and the X-ray spectrum can be well described by a multicolour blackbody spectrum (e.g.


Equilibrium tides become then effective (e.g.,


and references therein) and the tidal evolution may occur on a longer timescale.


For instance, for the Lyman α radiation χνr = 0.042 for optimum efficiency χo = 0.1


In particular, there are currently five main competing models.


(2) Empty Asteroid Belt: embryos and planetesimals in the protoplanetary disk formed concentrated within a narrow belt at ∼0.7–1 au


In what is called the “frozen-screen” hypothesis


these pockets, or turbulent eddies, are assumed to be fixed in the atmospheric layer that advects over an interferometric array


The dark and light shaded areas in Fig. 10 correspond to the 1σ and 2σ constraints on the redshift of reionization from the cosmic microwave background measurements of the Planck mission


with a reionization midpoint zre = 7.67 ± 0.73.


Previous sub-arcsecond angular resolution N-band (∼8–13 μm) ground-based spectroscopic studies investigated the 11.3 μm PAH feature in the nuclear and circumnuclear regions of AGN


However, these works were unable to provide definitive details regarding the effect of the AGN on the PAH molecules due to limited wavelength coverage and sensitivity.


In particular, the asymmetric Lyα line profile has enabled redshift confirmations of large samples of sources at both 2  z  6 (e.g.,


The faster solar wind tends to be more imbalanced with greater wave energy flux antisunward than sunward


In addition, another classification scheme uses a scatter plot of flux and duration fitted with two-dimensional Gaussian functions


Since NS He-atmosphere models have harder spectra than H-atmosphere models, using the incorrect composition for the observed thermal emission can result in biases of the inferred radii


The main sequence is a relationship between SFR and stellar mass followed by the majority of star-forming galaxies, apart from some outliers located above the average SFR at given stellar mass


As a result, direct imaging studies cannot decisively determine whether the clumps are different in nature from star-forming regions in our local universe or if the larger apparent size is merely an artifact of insufficient resolution


Prior to complete gas removal, moderate values of ram pressure have also been shown to increase the star formation rate in galaxies both observed


However, close encounters with the planets proved not to be enough for creation of the current population of binary systems


Choosing values of these parameters that are consistent with simulations (e.g. those of


Magnetic reconnection rapidly converts magnetic energy to particle energy, causing emission flare in multiple wave bands and even triggering coronal mass ejections


So, the mean length for QS network jets from the present work is in good agreement with


We note that a hotter disk during maximum was predicted by a simpler study in the past


The most evident effect driven by galaxy encounters is probably the triggering of new episodes of star formation, which can occur both in the pre-merger regime between first pericentre and coalescence (e.g.


In Fig. 10, we show the relation between the size and star formation rate of clumps, including samples across different redshifts


despite being at z ∼ 2–6, have sizes comparable to local H ii regions and GCs


However, a study of non-convex shape models for fast two to four hour rotators in


indicated that such asteroids have rather minimal levels of global-scale concavities, and the ~ 2.7 h rotation period of Cuyo implies that its shape could be similar.


An alternative explanation that we propose here goes back to the nature of the optically thick 12CO emission and to the approximately linear relation between 12CO luminosity and virial mass found for GMCs (see e.g.


Similar signatures were also reported in observations (e.g.,


For reference, the dark red crosses also show the equivalent satellite/central red galaxy wg + correlations from KiDS×GAMA here (c.f.


On large scales at least, our illustristng red sample is consistent with their measurements.


There are a few interesting features here to note, however.


Although the general trends match the real data,


with ss and to a lesser extent cs exhibiting strong scale-dependent IAs in this regime, the magnitude is somewhat higher in our sample.


This is particularly interesting, given that our sample characteristics are similar (〈L〉/L0 = 0.91 and 0.34 for our red and blue samples, respectively, compared with their ∼0.99 and 0.50).


It is now well established that the weak lensing of distant galaxies by foreground mass provides a relatively clear window on to the large-scale structure of the Universe. This is true whether that foreground mass is in the form


or the continuous large-scale matter distribution (cosmic shear;


The [C ii] deficit persists when including high-z galaxies (e.g.


This problem is also known as the Cosmological Lithium problem


Over that time they have been assigned different terms, such as


For comparison, we show published observations in the same redshift range from the literature in the right panel of Figure 5


IMF the expected range for the observed M/OB number ratio.


Minkowski functionals, which are also closely related to the crossing statistics


and have been utilized for cosmological random fields


This phase motion has been seen in magnetospheric data of Alfvén waves


and the simulations of coronal oscillations by


These studies note that the direction of motion is related to the spatial variation of ωc.


Energetic electrons are unstable to Langmuir waves, thus they are converted into radio emission at the local plasma frequency and its harmonic (see


have shown that the effects of a merger are visible for approximately 0.25 Gyr after the merger event while the pre-merger stage is much longer. However, we chose to have the pre and post merger period approximately equal as tests conducted with longer pre-merger times showed no improvement, see discussion in Sect. 4.2.


which is considered as the most critically analysed data base.


and with the NIST values shows that the present ab initio values are not fully converged to experimental values.


The hybrid source XTE J1701–462 occupies a special place among NS LMXBs and is considered to be a remarkable source, as it displays all the characteristics exhibited by both Z and atoll sources


and May & Stevenson (2020) favour a larger phase offset (21 ± 2 °E) than Mendonça et al. (2018) and Morello et al. (2019) (12 ± 3 °E and 11 ± 2 °E).


There are at least three reasons why radiative feedback is an essential ingredient of the galaxy formation process.


Thirdly, it is difficult to explain the large gas turbulence values observed in star-forming regions without including the momentum input by radiation


Furthermore, most of these HFF clusters are in a state of collision, enhancing their value for assessing the collisionality of dark matter (DM), a basic assumption of the standard particle interpretation of DM


The features observed in most CL AGNs, e.g., the complex multiband spectral variabilities, and strong changes seen in the infrared or low level of polarization, strongly argue against the scattering (or obscuration) scenario (e.g.,


noted that heating bayerite at 500°C eliminates the XRD pattern of bayerite, and they note that at 700°C, the infrared reflectance spectrum of the boehmite sample no longer shows OH− stretching bands.


As can be seen in this table, the WHISPER survey allowed the detection of some organic molecules in the Horsehead nebula, such as formaldehyde (H2CO) and methanol (CH3OH), which constitute key species in the likely synthesis of more complex organic molecules such as some prebiotic molecules


In these objects, the total number of OB associations is significantly larger than the number of HII regions under formation and of OB stars reaching the final stage of their evolution, thus their total Hα luminosity is fairly constant with time. This might not be the case in strongly perturbed systems or in dwarf galaxies, where the total star formation activity can be dominated by individual giant HII regions


Early attempts of low-resolution three-dimensional numerical simulations on overshooting were made by


also showed that the MMF can be generalized for the case where the SED of the sources is not known.


This generalization outperforms the single-frequency MF in terms of S/N and can be used to infer the spectral index of synchrotron-dominated radio sources, as shown in Lanz et al. (2013).


The detrending performances of pixel-ICA method have been compared with division by a polynomial function of the centroid, in this paper PCD method, and PLD method


This result is inline with the number density estimate of the order of ∼10−10 Mpc−3 by


Our preliminary analysis shows that the self-gravitating response is a linear superposition of two terms: (i) a continuum of modes given in Equation (12), dressed by self-gravity, that undergo phase mixing and give rise to the phase spiral; and (ii) a discrete set of modes called point modes or normal modes (see


One warm and compact component at 200 K and a size of 0.35″ (that of the continuum compact emission obtained by ALMA Band 7 observations,


this mass is significantly diminished via stellar winds already during core hydrogen (H) burning


has opened up new ways of studying galaxies in the radio, and a number of studies have used LOFAR’s capabilities to investigate this relationship between star formation and radio luminosity in the low-frequency regime – for example


Read et al. (2018), Smith et al. (2021), and Wang et al. (2019a).


The chemical contamination of barium stars is believed to be due to accretion of chemically enriched material from an evolved binary companion, likely through wind


Then a separation of the HC top from that of the prominence was observed during the eruption initiated by the ideal kink instability


Therefore, this observation offered further important support for the idea that an HC is an MFR


The overall excesses within 805 and 1186 h of HESS exposures


Most of the radiative models for Sgr A*, which are based on post-processing GRMHD simulations, assume that electrons have a thermal, relativistic (Maxwell–Jüttner) distribution function, and that the proton-to-electron temperature ratio is constant across the simulation domain


There are indeed indications that the buildup of the ice in cold environments results in the formation of pores as shown b


These two studies, based on Monte Carlo simulations, suggest a significant level of porosity at the surface/subsurface, in particular in cold and dense environments.


This geometric advantage is shared with the related analysis technique of spherical Fourier-Bessel (SFB) decomposition


which, in addtion to spherical harmonic decomposition, involves a further Fourier-Bessel transform and data-compression along the line-of-sight.


However, SFB does not share another important feature of SHT, which is its ability to capture redshift-dependent change over cosmological time in deep surveys.


While Sn can also be formed from pure H2S ice by photo processing


the fact that S3 is clearly related to dust and is not found in the normal nucleus ice, where H2S is quite abundant, indicates that S3 is a product of radiolysis of the ammonium salt.


However, for heavily accreting massive YSOs the onset of the H II region could be delayed via stellar bloating


where the effective temperature of the star is much cooler than it would be considering a main sequence star of the same luminosity. In these models, a halt or considerable reduction in accretion (≪10−3 M⊙ yr−1), or growth beyond ~30−40 M⊙, will result in the YSO contracting to a “main-sequence” configuration, heating significantly, and being able to create an H II region.


When we change the magnitude of two tides, the final location of the planets can be adjusted


Concerning the other far-IR PACS band (100 μm) and the mid-IR 24-μm band, we use the association available in the DR1 release and based on the maximum likelihood technique


The time for GJ 1148 b to reach asymptotic rotation is inversely proportional to the initial Prot, as long as the initial Prot is much less than 27.5 d, and it depends on the other parameters of GJ 1148 b according to Eq. (3) of


At higher Eddington ratios of Lbol/LEdd ≳ 10−2, single-epoch X-ray and UV observations of large samples of AGN have previously revealed a hardening of αOX as Lbol/LEdd drops from ∼1 to ∼10−2 (e.g.,


We note that we can discount variations in the seed photon population as the driver for changes in the power spectrum, as the UV emission from the disc is established to be considerably less variable than the corona in NLS1s


We find here that about two free-fall times (as defined for cylindrical systems, see


are sufficient to reach core deuteration fractions of ≳0.1.


Within conventional leptonic scenarios, this component is produced when the synchrotron-emitting electrons inverse Compton up scatter the photons of internal (synchrotron self-Compton, SSC;


Adding on AGN feedback would significantly impact on the distribution, kinematics and physical status of the gas, specifically for the close environment of the black hole


In last few decades, the understanding of CMEs improved significantly because of space and ground-based observational data with the help of various modelling efforts. The studies are focused on the morphological and kinematic evolution of CMEs in the heliosphere, e.g.


The growth of dust grains through accretion in the ISM has been proposed as a solution (e.g.


Other studies suggest that the presence of preeruptive MFRs is not necessary and MFRs could be built up in the corona via magnetic reconnection processes associated with flares


For instance, it is well known that adding a tiny amount of heavy elements and dust grains alters the EOS of a collapsing cloud (e.g.


High-ionization UV lines have been detected in the spectra of z ≳ 2 galaxies through


The EWs of He II, O III]λ1666, and C III] from these works are larger than those measured in the average spectra of our LAEs, with the exception of


are computed from average spectra of a z ≈ 3 LAE population whose median UV luminosity is about two orders of magnitude brighter than ours.


From Figure 2 in Rincon et al. (2017), we further notice that the vortical component of the photospheric surface velocity field has a structure reminiscent of 2D Euler turbulence, which admits a vortex point representation


An alternative route to explain the presence of methanol in the gas phase is the reactive/chemical desorption that has been theoretically proposed by Garrod et al. (2007) and


and experimentally studied by Dulieu et al. (2013) and Minissale et al. (2016).


On the other hand, c-C3H2 is mainly formed in the gas phase


and is expected to preferentially trace dense and chemically young gas, that is, gas where C atoms have not yet been mainly locked into CO.


This gas rich in C atoms is expected in the outer envelope of an externally illuminated dense core


However, towards L1544, c-C3H2 only appears to trace one side of the core, the one closer to the sharp N(H2) edge and away from the CH3OH peak. This indicates that photo-chemistry is not uniformly active around L1544, most likely because the distribution of the envelope material (belonging to the filament within which L1544 is embedded) is not uniform, as is clearly shown by the Herschel map in Fig. 1.


is limited by their sparse numbers and by the difficulty of detecting them over large areas of the sky. Low-frequency radio observations have an enhanced capacity to detect the extended old electron population in these objects (see e.g. the recent Low Frequency Array – LOFAR – observation of the GRG UGC095551), but high-frequency radio observations are less efficient in this task due to the steep-spectra of giant radio lobes.


In this context these sources will be ideal targets for the next coming deep, wide-field surveys like, e.g. the ATLAS survey of the Australia Telescope Network Facility (ATNF


or the Square Kilometre Array (SKA) deep surveys that will have the potential to study their population evolution up to high redshifts and thus clarifying their role on the feedback for the evolution of non-thermal processes in large-scale structures.


Within a 500 arcsec radius centred on NGC 346, we find an atomic gas mass of 2.7×106 M⊙ using the Parkes+ATCA H i map


Analysis of Chandra observations revealed a hole or bubble within the ICM, cospatial with the eastern lobe of the jet


By using the RADEX2 dense cloud models developed by


to reproduce the HCN(3–2)/(1–0) line luminosity ratios in the outflow of Mrk 231, we can attempt to find a combination of XHCN, XCN, Tkin, and nH2 solutions that can also fit the CN/HCN and CN spin doublet line ratios (Table 2)


The HB pattern is generally observed in the subcritical regime and the DB pattern is observed in the supercritical regime


Previous 12CO observations either reported no detection of outflow emission toward this source


or only weak compact blueshifted emission towards east of the continuum source


The [OII]λ3737 emission traces on-going star formation


but it also depends on the metallicity and can be a poor tracer for dusty galaxies (e.g.


Moreover, other studies have compared AGN selected from various wavebands and find that their host galaxies tend to have different properties


The model atmosphere used in this work was interpolated from the line-blanketed, local thermodynamic equilibrium (LTE) ATLAS9-ODFNEW grid


Besides these necessary conditions for the applicability of the FP equation, also other simplifying assumption for a better tractability of the FP equation are being made, such as (1) the magnetic fluctuations are homogeneous in space, (2) the electromagnetic fields are quasi-static, (3) the interaction has a finite decorrelation time, etc. (see more details in the books


Unfortunately, in astrophysical and laboratory plasmas, most of the above assumptions are not valid, yet the FP equation is used extensively, without a proof of its validity.


Aside from the observational implications, the planet’s physical and chemical state can be altered by stellar activity as well due to, for example, coronal mass ejections (CMEs) and stellar particle events (SPEs)


As a further comparison, data from the SOHO/EPHIN spacecraft (red square marker) between 40 MeV and 53 MeV are also presented


The agreement appears to be good in all the three examined periods, considering both statistical and systematic uncertainties.


Covering these spatial scales in ≤108 yr requires a diffusion coefficient of D ≥ 9 × 1028 cm2 s−1, which is slightly higher than observed in spiral galaxies


If the spatial velocity of a star in an SNR is very different from the others in the SNR, the star is very possible to be the surviving companion in the remnant


Mechanisms involving the addition of hydrocarbons, such as acetylene onto aromatic rings as well as the attachment of other aromatic rings, or hydrocarbon pyrolysis, have been proposed to characterize the growth process of PAHs


Current cosmological hydrodynamic simulations of galaxy formation employ a variety of subgrid models (e.g.


that artificially launch galactic winds,


These three spatial features nearby to the Sun appear to form part of the global spiral structure in the Galaxy. Contrary, the objects of older population with larger random velocities, for instance, main-sequence A–K stars or the oldest Cepheids and open clusters, do not currently follow the exact location of those arms (e.g.


The above equation should reduce to the jet Lorentz factor profile used in


The core stable within 200 μas constrained by the VERA can be explained by Lorentz factors within a factor of two variation for the slower ejecta, i.e., 8 ≤ Γs ≤ 17, by assuming


This scenario is in agreement with arguments by other authors that the 26Al-free CAIs formed prior to injection and homogenization of 26Al in the early solar system


When planets become massive enough, they can carve gap


Galaxies formed in these halos because of the cooling of


This allows us to use the microlensing magnifications to estimate the source size, and such work has shown that in general the accretion disks are larger than would be expected from either thin disk modeling or total flux arguments


The bright end of the UpSco population has been examined in X-rays


A full description of the GLOSTAR continuum data calibration and imaging is given in


More precisely, it takes 3–4 orbits for MRI to develop and ∼10 orbits to saturate


presented scaling relations between the azimuthal separation of the primary and secondary arms and the planet-to-star mass ratio for a single companion on a circular orbit with a mass between Neptune mass and 16 MJ around a 1 M⊙ star. They predicted with 30% accuracy that a single putative planet responsible for both spiral features of SAO 206462 would have a mass of ~6 MJ.


The most likely candidates for this task, given their reasonable agreement with observations and numerical simulations of cosmic-ray diffusion coefficients, are the quasilinear theory (QLT) of Jokipii (1966), the weakly nonlinear theory (WNLT) of Shalchi et al. (2004b), and the nonlinear guiding center theory (NLGC; or one of its variants; see, e.g.,


Our analysis was rather easy, starting from a prediction based on


Other examples of AGN with at least two variable phases of the X-ray winds are


We showed that the ambipolar diffusion module in Bifrost can cope with the passage of the solutions through the current sheets, with the level of accuracy increasing the higher the spatial resolution and in spite of the intrinsic singularity in them. Vice versa, the tests show that these functions can probe the capabilities of ambipolar diffusion modules to a larger extent than the simple ZKBP solution that has been used thus far (e.g.


The results were obtained implementing a Bayesian scheme that uses the spectroscopic constraints and frequency ratios as the parameters in the fit


, the latter being almost insensitive to the surface effects in solar-like oscillators


studied the mechanism for the flare trigger by shock waves. They used a 2D magnetohydrodynamic model with the MHD shock wave propagating towards the current sheet. A portion of the shock wave passed through the sheet, and the rest was reflected. Nothing occurred at the very beginning of the wave-current sheet interaction. However, after some time, specific plasma flows around the current sheet were formed, which led to the start of magnetic reconnection.


This shows that for reconnection to be triggered, the enhanced electrical resistivity as well as the plasma flows are important.


The release of gravitational binding energy via accretion of matter onto these BHs is expected to have a profound impact on the evolution of their host galaxies (e.g.,


Figure 1 shows the view obtained from polarimetric observations: the left panel shows the QΦ image in the J band obtained by


using SPHERE on a linear scale, and the two rings are clearly visible.


We also used some observational data obtained within several other programmes


The nuclear reaction rates are those from the NACRE project


, supplemented by the updated reaction rate from


Ccf is a factor that removes the color term from S and is a function of Johnson


Intrinsic Lν(1400)/Lν(900) ratios obtained from different stellar population models: the BC03, assuming different initial mass functions (Salpeter, Salp, and Chabrier, Chab), star-formation histories (constant, cSFR, exponentially declining with τ = 0.1Gyr, exponentially rising with τ = −0.1Gyr), metallicties (Z⊙ and 0.02 × Z⊙), and stellar-population ages;


BC03 provides the spectral energy distribution of stars obtained from a comprehensive library of theoretical model atmospheres (KBFA in the table).


The library consists of Kurucz (1996) spectra for O-K stars, Bessell et al. (1991) and Fluks et al. (1994) spectra for M giants, and Allard & Hauschildt (1995) spectra for M dwarfs.


The SFR_2b model is the one that best reproduces the observed A(Li) distribution while recovering the presently observed SFR and the thin-disk stellar and HI mass


There are at least three possible types of outflows around young stellar objects: (1) a disc wind launched from the accretion disc (e.g.


The net radiolysis is the combined effect of the direct primary excitations and ionisations, the core of the energy deposition by the ion, and the so-called delta rays (energetic secondary electrons) travelling at much larger distances from the core; that is, several hundreds of nanometres at the considered energies in this work


Experimental measurements by e.g. instantaneous laser tomography have given values ranging from D = 2.1−2.4 in a variety of flow geometries, with a preferred value of D = 2.35


If a single SMBH model with a BLR d of 95 light days is true (see


Instead, it is most likely that these values correspond to ram pressure, in which case they imply mass, momentum, and energy flux across Eulerian cloud boundaries, or a displacement of Lagrangian boundaries


The radiation of SNRs in different wavelength ranges is under the influence of biases as they cover different aspects of the ISM environment and SNR age and evolution


However, recent experiments indicate that this product channel occurs in only 19 percent of collisions, with 81 percent of collisions forming CH + S


Even so, significant progress has been made in the last decade, though the problem is usually made tractable by introducing at least one of the following simplifying assumptions: abandoning general relativity in favor of a pseudo-Newtonian description of the gravitational potential while performing realistic, multi-angle group radiation transport


The value R ≈ 5 mm has been constrained by several data collected at comet 67P, by laboratory experiments of dust accretion in conditions expected to occur in the solar protoplanetary disc and by observations of other protoplanetary discs


The astrophysical disk transition region is at least equally complicated since it is not only the base of the disk corona, but also the origin of purported disk winds and outflows (e.g.,


However, there is indication of non-negligible poloidal fields as well as toroidal fields—resulting in helical magnetic fields—in the jet environment of other distant AGNs, which results in transverse RM gradients with no sign changes (e.g.,


Open clusters have been used to test the scaling relations for giants


RASCAS deploys a general two-step methodology (e.g.


On the other hand, high values of temperature, surface density, and velocity dispersion in a turbulent ISM of starbursts and merging systems will shift αCO towards lower values


To our rescue, eBOSS also targets all SDSS point sources that are within 1 arcsec of a radio detection in the FIRST point source catalogue


Recent proper motion data confirm that most of the classical MW satellites do indeed have a common orbital plane


aligned with the plane normal defined by the satellite positions alone


Among these large-scale structures, the underdensities of the universe, i.e. cosmic voids, have been shown to have great potential for constraining dark energy and testing theories of gravity via several measurements. These measurements include: distance measurement via the Alcock–Paczyński test


There are further analytical approaches described in the literature


, although these models predicted a change in the spin state of the nucleus without taking into consideration the exact 3D shape model and its variation induced by mass loss.


However, since the identification of the Ly α forest in hydrodynamic simulations


it was realized that in the context of cosmological models for structure formation, the Ly α forest is due to a fluctuating, continuous IGM (e.g.


Alternatively, the origination of giant pulses is proposed from the coherent instability of plasma near the magnetic equator of light cylinder


Magnetospheric accretion (MA) shock modelling was carried out for each star by adding (blackbody) accretion contributions to the photospheric (Kurucz) spectra (see e.g. the reviews in


Therefore, on the basis of the oscillation of coronal loops, especially their oscillation characteristics in frequency, phase and attenuation coefficient, solar physicists can further understand the relationships between the coronal magnetic field, flares and CME


and obtain corresponding physical parameters associated with oscillating coronal loops


lists the orbital parameters (orientation and separation) of WDS 02499+0856 and gave θ = 194°, ρ = 5.66 arcsec and magnitude difference ΔV = 0.07 mag (the magnitude difference can be as large as ΔV = 0.36 mag, due to photometric variability of the eclipsing binary)


Complementary to the study of the overall metallicity distribution, the abundance ratios of several other elements, such as α-elements, iron peak, odd-z, and neutron capture, can provide deep insight into the variety of nucleosynthesis processes, with their production sites and time-scales (e.g.


The thermal state and kinematics of the progenitor hot plasma halo drive the formation and evolution of all the condensed structures, which inherit some of the parent properties. Part of the inner condensed gas eventually accretes onto the central supermassive black hole (SMBH), igniting the feedback response and efficiently self-regulating the entire atmosphere over several gigayears (e.g.,


Furthermore, given the demonstrated sensitivity of computed low-energy galactic electron intensities to various turbulence quantities (see


, it may be possible to draw conclusions from Jovian electrons to better understand the behaviour of those quantities in regions of the heliosphere where spacecraft observations of this character do not exist


As motivation, we note that a variety of observations in the solar wind


have suggested that fluctuations near the end of the magnetohydrodynamic (MHD) inertial cascade range, and approaching the kinetic plasma range, may consist primarily of kinetic Alfvén waves (KAWs).


Events that took place in the far past are expected to have induced a thickening of the early Galactic disc,


and second by agitating the gaseous disc from which new stars are born, generating early stellar populations with higher initial velocity dispersions than those currently being formed


There have not been many simultaneous multi-wavelength studies of flaring stars


There is a particular dearth of simultaneous data in the EUV which is critical for studies of exoplanetary upper atmospheres, but where measurements are difficult due to ISM absorption. More observations are needed, but if young, magnetically active stars display broadband continuum enhancements during flares, similar to AU Mic, this would mean that large altitude ranges in planetary atmospheres are affected.


Although hampered by the short duration of the quenching process, the search for galaxies in this critical phase of evolution has been carried on by several authors in the past decades. Galaxies characterized by both a tidally disturbed morphology and intermediate colours (e.g


have been considered as valid 'recent time' quenching candidates.


There are a number of such ground-based experiments, including


the Shaped Antenna measurement of the background RAdio Spectrum (SARAS;


The reliability of the used method is also underlined by the good qualitative agreement between the Density Functional Theory (DFT) and MP2-F12 calculations as found in previous works


Theoretical models by Granato et al. (2004) suggest that forming clusters will go through a phase in which multiple members will undergo near-simultaneous massive bursts of star formation. The spectral energy distribution of these objects would be dominated by the far-IR, as is the case for local massive starbursts (e.g.


While the K2 optical data set detected a 3.3 day periodic 1% photometric modulation, it is not present in the Spitzer observations


Other possible alternative mechanisms leading to the acceleration of HVSs are the encounter between a single star and a massive black hole binary in the GC (e.g.


Conversions to magnitude are based on the standard zero-points in the Vega system as described in the ACS Data Handbook


At high accretion rate, the inner region of a standard α-disc


Recent works suggest that the deformation of the magnetic field lines is determined by the parameter δ (the ratio of the gravity to the magnetic pressure)


Bayesian reconstruction methods have become increasingly popular in cosmology and have been applied in a range of different applications such as


After 1500 A.D., the GNP moved to Canada. This caused the geomagnetic field latitude of China to decrease considerably. Meanwhile, the field intensity decreased to its minimum value in the last 2000 yr. Under these conditions, it would have been very rare to observe the aurora in most places in China after the 16th century, just like the present case


In what are sometimes called ‘semi-empirical’ methods [also called subhalo abundance matching (SHAM) or halo occupation distribution (HOD) models; see Wechsler & Tinker 2018], galaxy properties are mapped on to the properties of dark matter haloes such that a set of observational quantities is reproduced


In the case of midplane spiral structures, their origin may be linked to the presence of a companion—stellar, fly-by, or planetary


The accretion of gas and the dynamical evolution of BSBHs are likely to be coupled


such that the occurrence rate of BSBHs depends on the initial conditions and gaseous environments at earlier phases


For comparison, we also show the integral number count


and from the high-resolution ALMA follow-up of LESS


The dust distribution away from the midplane is better captured by hydrodynamical simulations than by simple prescriptions relying on a parameterization of the turbulence strength (see, e.g.,


since it depends on the particular source of turbulence.


These pads provide the digital readout of the detector up to 22 particles m−2, allowing the count of the air shower charged particles without any significant saturation up to primary cosmic-ray energies of about 200 TeV


Analysis of the stellar clusters in the complex reveals them to have ages of 1.5 Myr for Danks 1 and 3 Myr for Danks 2,with the former possibly being triggered by the latter


In order to fulfil equation (2) during the whole inbound orbit, cometary activity is driven by at least the five ices listed in Table 2, reporting the nucleus and gas coma parameters computed by means of the activity model


we find log FFUV/FJ = −2.49, log FNUV/FJ = −2.11


Analytical fits of these neutron-star EoSs have been constructed in order to facilitate their inclusion in astrophysical simulations


and Mennella et al. (1998) and in the present study this correction was not applied


The majority of observed SPDBs are connected to solar flares


On the other hand, the annual variation in the IMF polarity in the band of 256–512 days, which is referred to the Rosenberg–Coleman effect


The authors indicated that such a result should be attributed to a more stable and flat heliospheric current sheet that only appears in the ascending phase of solar cycles and strong disturbance of the heliospheric current sheet that is present in the declining phase and minimum time of solar cycles, and the Rosenberg–Coleman effect had been confirmed by the IMF Bx component during 1964–2002.


flows of accreting matter in neutron stars


This can be done either in the EoS parameterizing methods


and the results are well consistent with each other.


Moreover, in DR processes, the H ejection is in general favoured more than H2 ejection


Currently, there are two possible scenarios on the origin of S0 galaxies.


The other is that S0 galaxies are intrinsically different from spiral galaxies since their formation


In this respect, GRGs have a crucial role in the acceleration of cosmic rays over large cosmic scales (e.g.


Gap-type emission models offer a promising alternative and different realizations have been proposed in the literature (e.g.,


The correlated angular momenta result into correlated inclination angles of neighbouring galaxies and thus ultimately into correlated ellipticities


We address this issue by calculating local number density of galaxies using kth nearest neighbour method


It is supported by correlated optical/γ-ray flares in FSRQs (e.g.,


Thus, for planets in the Solar System, it was shown both in the observations


that the presence of a weak magnetic field can intensify atmospheric escape.


Numerous investigations of tidal activity on extrasolar planets have been conducted, with a range of topics


The inner few arcseconds is a complex mix of


polarized, broad optical emission lines due to scattering by dust


that the enthalpy fluxes associated with both evaporating and condensing plasma are at all times in approximate balance with the excess or deficit of the heat flux relative to the transition region radiation loss rate.


Some of these fragments have been recovered


For the purposes of this study, we adopt the composition of type I CAIs as the representative value of refractory objects because they are seemingly the most abundant type and lack the characteristic elemental depletions of other CAI groups (e.g.,


Hence, we think that the radio jet is transferring its energy and momentum to the ambient medium through an extended shock front, which creates turbulence in a dense clumpy ISM. Such a great impact of the radio jet has been observationally shown in many cases (e.g.


We also plot the results of previous blank-field surveys


This model has been previously used for the modelling of planetesimal formation in PPDs


The size distribution is probably shallower


All our low-mass galaxies are characterized by moderate Ly α luminosities in a narrow range between 1042.19 and 1042.74 erg s−1 (Fig. 6a), that are slightly below the values for confirmed LyC leakers (blue filled circles) by Izotov et al. (2016a,b, 2018a,b) and high-redshift galaxies (grey open circles) by Ouchi et al. (2008), Hashimoto et al. (2017), Jiang et al. (2018), Matthee et al. (2017), Matthee et al. (2018), Sobral et al. (2018), but are ∼1 order of magnitude higher than those for GPs (black asterisks;


While the fluorescent signal powered by the diffuse metagalactic UV background


with an expected surface brightness (SB) of $\rm SB_{Ly\alpha }\sim 10^{-20} \,erg \,s^{-1} \,cm^{-2} \,arcsec^{-2}$


is still out of reach for current optical instrumentation (but see


Ly α fluorescence is predicted to be boosted up into the detectable regime in the vicinity of bright ionizing sources, as luminous quasars


In literature studies, CO line ratios do appear enhanced in low-metallicity regions or galaxies (e.g.,


The NFW profile has been shown to provide an overall good agreement with observations and simulations over a broad range of scales in GR


While some phenomena exist in the early Universe, such as quasars or radio galaxies, which are so powerful and intrinsically bright that they have been able to serve as beacons to early searches near the epoch of H I reionization (z ~ 5.5–10,


the bulk of the galaxy population residing in the early Universe does not contain such phenomena


or the $\rm [O\, III]$ flux weighted radius


As evolved stars ascend the RGB, C and N abundances may be changed by first dredge-up


The discovery of this correlation has led to an increased interest on the abundances of other elements in planet hosts(e.g.


However, these studies do not explore lower metallicities, despite available evidence for the existence of a low-metallicity ISM in the past through the discovery of stars


as well as several others with $\rm {[Fe/H]} \lt -5$


while BL Lacs are powered by an advection-dominated, low radiative efficiency accretion flow


Given the rh = 20 au distance of our measurements (and the expected large size of 2014 UN271), we adopted a beaming factor η = 1.175 ± 0.42, based on measurements of 85 Centaurs and TNOs


At very large densities, though, owing to the increased dust absorption coefficient, the gas becomes opaque to its own radiation. This is sometimes referred to as the opacity limit


At this point, the fragmentation is halted, setting a scale below which no fragments form.


On scales up to a few Mpc from the nearest galaxy cluster, possibly along filaments, only a few diffuse synchrotron sources have been reported


The inertial range, which is dominated by magnetohydrodynamic (MHD) turbulence, follows the cascade models with spectral indices αi from around 3/2 to 5/3


The expanding box uses these comoving coordinates, approximating the spherical coordinates by the Cartesian ones


To assess the star formation contribution to the Hα flux, we consider lines from the most extreme AGN photoionisation models of Groves et al. (2004), to the location of solar metallicity star-forming galaxies (see also


In addition, the theoretical definition of cores also depends on whether the star-formation scenario is quasi-static or dynamic. In the former scenario, cores are gas condensations sufficiently dense to be on the verge of gravitational collapse, and they convert the core gas into stars


A commonly used tactic to increase the efficiency and improve the stability of these simulations is to artificially increase the luminosity (or nuclear energy for convective cores or burning shells) and to modify the thermal diffusivity of the reference stellar model. This tactic is common and has been used, for example, in


This approach is used to increase the Mach number of the convective flow, reducing the disparity between advective and acoustic timescales, improving the efficiency of time-explicit codes limited by the Courant–Friedrich–Levy constraint. It is also used to provide numerical stability or to accelerate the thermal relaxation. But no examination of its potentially far-reaching impact has been conducted.


The beam fluxes used had values of 3 × 109, 1 × 1010, and 3 × 1010 erg cm−2 s−1, while the low-energy cutoff EC covered the parameter space where flare values are usually found (20–120 keV;


Galaxies satisfying all three of these criteria are rare; in principle the Milky Way GC databases could be used, but cluster-to-cluster foreground reddenings differ strongly, the published SDSS indices


show considerable scatter versus metallicity, and the variety of studies from which the UBVRI indices were derived are completely different from the SDSS survey, so that aperture-size mismatches are significant.


However, such a dynamical system is linearly unstable to parametric instabilities and large-amplitude Alfvén waves are known to decay into compressible and secondary Alfvénic modes through three- or four-wave resonances that lead to a variety of parametric instabilities, depending on the plasma beta and dispersive effects, such is the case of parametric decay


Recent works on laboratory measurements of cohesion between crystalline water-ice particles at vacuum conditions provided encouraging results that dust particles composed of water ice might be much more cohesive than previously believed


This equation and the condition $F_i-q^\prime _if\ne 0$ furnish the generalized NBH equations


In the avoidance scheme, smooth-spectrum foregrounds should, in the ideal case, occupy a wedge–shaped region of the two–dimensional power spectrum space (where the wavenumber k can be decomposed into k⊥ and $k_\Vert$ that are the transverse and line-of-sight wave numbers, respectively) whereas the remaining area – the so-called EoR window – is dominated by the 21 cm emission


Maybe we do not need to intentionally take to heart such the classical dichotomy, because waves and reconnections may interact with each other


The cluster merger induced relatively strong shocks, which travelled through the ICM, accelerated particles to produce relics towards the north and south of the cluster


On kpc scales and in the discs of nearby star-forming galaxies, τdep is approximately constant around 1–2 Gyr


applied a Gaussian process, principal component analysis (PCA), and deep learning neural networks to radiative transfer models of SNe.


A good agreement between observations and theoretical predictions for the Galaxy is obtained by models that are based on the assumption that the disc formed via the infalling of gas


Following this, higher level calculations on the electronic structure, rotational constants, and harmonic vibrational frequencies of each isomer were performed using CCSD(T) together with the Dunning basis sets aug-cc-pV(X+d)Z (X = T, Q, 5)


Our investigation is based on a magnetospheric model that synthesizes the corotating magnetosphere model and the vacuum model


, in which multiple quasi-stable magnetospheric states are described by the parameter y such that the charge filling fraction of a state corresponds to a y value and a change in the charge filling fraction corresponds to a change of state which is signified by a change in y.


In some cases, the stellar system resulting from the merger event may show significant internal rotation (in fact, for many years this has been the preferred dynamical route to form rotating star clusters; see


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


For example, in Mrk 501 the shift in both peaks strongly implies the same particle distribution for the overall emission, while for OJ 287 the shift of only the high-energy peak can be reproduced by either inverse Compton scattering of the broad-line region photon field


Secondly, although a fraction of LBV stars are isolated (e.g.


For internal consistency, all EWs in this work have been adjusted to the measurement scale of


The shock is then revived by adding an energy injection following the parameterized method of


In particular, the CN index distribution shows the largest spread. Note that a bimodality or a large spread in CN distribution is generally observed in most GCs


A similar feature has also been observed


As the SN explosions start occurring within the cavity formed by the stellar wind bubbles, super-bubbles are created (e.g.


), which may eventually reach kiloparsec sizes.


In particular, it was noted that “the Simpson et al. (2017) stars do not define a red giant branch in the theoretical plane, suggesting that their parameters are not correct” (Fig. 1 of


In the non-rotating case, the GW emission from the post-bounce phase has been studied using self-consistent 3D simulations by many groups


High temperatures in the accretion disc can induce exothermic nucleosynthesis too


All these processes taken together in an advective disc will produce very hot jet base.


Magneto-Rossby waves are basic mechanism in variability of various objects in plasma astrophysics. Magneto-Rossby waves determine the large-scale dynamics of the Sun and stars


(Eq. (6) with q = 0.62, see left column) does provide a good approximation of the observed distributions, when assuming the original Θmed − S relation described by Eq. (7), only at flux densities S150 MHz≳10 mJy (see long-dashed lines). This is perhaps not surprising considering that this relation was calibrated at 1.4 GHz down to a few mJy fluxes. At the lowest flux densities (S150 MHz≲1 mJy) we need to assume a steepening of the parameter m (see Eq. (8)), to get a good match with observations (dotted line in the top left panel).


Similarly, the peak bolometric luminosity of SN 2012au (∼ [6.56 ± 0.70] × 1042 erg s−1) is higher than the mean peak luminosities of SNe Ib and Ic, but still lower than those of SNe Ic-BL


Putting aside large-scale eruptions so as to focus on the quasi-steady input of energy into the corona, it is possible to distinguish three broad magnetic configurations of the solar atmosphere for modelling purposes.


CH3C3N itself may form the protonated species, C4H3NH+, through reactions with the HCNH+ and C2H5+ ions producing HCN and C2H4, respectively


Proton plasma properties provide an alternative to determine the solar wind type


A clear advantage of this approach is that the required observables are available from more spacecraft.


However, if the kink-unstable filament is heated during magnetic reconnection, it is often observed in the AIA 1600 Å channels (e.g.,


By comparison, the total background at 850 μm inferred from COBE-FIRAS is 3.1–4.4 × 104 mJy deg−2


Summing these separate surface brightness densities together, we find that the LBGs with L1700 > 1029 erg s−1 Hz−1 in our z ∼ 3, 4, and 5 samples comprise around 6–8 per cent of the submm background at 850 μm (where the range of values simply reflects the uncertainty in the COBE-FIRAS result).


the diffuse form observed for the ICL is consistent with the scenario where this component formed by stripped material from the outskirts of a galaxy in a close passage with the cD


Although this may suggest better X-ray detection prospects for external galaxy bubbles than our results would imply, we note that these Galactic observations may include a very significant thermal bremsstrahlung contribution from all the gas in the Milky Way halo, which likely extends to a radius of ∼250 kpc


the Galactic bulge, and gas heated by the shocks associated with the bubble


none of which is included in our model (and could evolve as the bubble ages).


The penultimate point has been widely discussed (e.g.,


involving the role of the flare material and the interacting CMEs on seed particles.


In such a case, to accelerate particles up to an energy Ec via a diffusive mechanism, the mean-free path λc ∼ rg(γc, B)2/s in the shock downstream region, where B is a small-scale field, has to be smaller than Larmor radius in Bjd


These astrophysical observations are furthermore theoretically explained by deep crustal heating due to pycnonuclear reactions


In particular, theoretical studies have shown that the MBH–halo occupation fraction can be low in dwarf galaxies


and even in systems hosting MBHs, their growth is strongly suppressed because of the typically low gas densities in the host (compared to more massive disc galaxies) and the strong impact of supernova explosions, both at low and high redshift


These nebulae, whose first examples were detected in Hα


more recently have been discovered and observed in X-rays and sometimes in radio


show some bending of the jets towards the tail. This bending in numerical models (for slow incompressible ISM flows) is connected with the numerical dissipation inherent in the numerical schemes. Numerical viscosity may cause the boundary layer breakage on the surface of the astropause, which consequently causes the pressure asymmetry that deflects the astropause. This may be the explanation for the fact that the tube of the astropause is always deflected to the tail in the numerical models. The above-described numerical effects have nothing to do with physical dissipation phenomena responsible for the bending of real astrospheres.


The physical dissipation mechanisms (e.g. magnetic reconnection, finite resistivity, Hall effects) should be explored as a possible cause of the astropause bending in the models with slow subsonic ISM flow.


claim that previous estimates of the evolution in the RS GLF


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


We test the results in Stanimirović et al. (2014) and


Meanwhile, a similar power-law index of energy distribution for non-repeating FRBs is also found


The results presented here are based on the assumptions that the CBPs do not interact with the material ejected from their binary star. However, numerical studies have indicated that this material is neither lost isotropically from the binary during the CE phase, nor does it all become unbound. Instead, 1–10% of the ejecta may fall back into a CB disk according to Kashi & Soker (2011), and Passy et al. (2012) suggest that ∼80% of the ejected material may remain gravitationally bound to the binary (also see


In recent years, a deficit of star-forming galaxies in the infalling region of clusters has been reported (e.g.


In the local universe, relationships between strong emission line ratios and metallicity can be calibrated to âdirectâ electron temperature-determined metallicities from


or photoionization models of star-forming regions


We utilized a sample of ALMA-identified SMGs in the UKIDSS-UDS field, which has been studied in detail with proper SED fittings


Similarly to our observations, the sample of


was drawn from a flux-limited sample produced by the SCUBA-2 Cosmology Legacy Survey


Many authors have studied the global and local reconnection rates and timescales of solar reconnection during solar flares based on analysis of the ribbon motions in the chromosphere


Moreover, if we consider the inverse covariance of the time domain noise as the weights, the GLS estimate is also a minimum variance and a maximum likelihood solution to the problem. However, computation of the solution in such a case may require


or an application of some iterative procedure


These latte typically involve several matrix-vector multiplications at each iteration step.


Moreover, precisely determined DIB profiles


showing a specific substructure pattern each, should facilitate their carrier's identification.


For the radio-loud magnetars, given their large variability, we have chosen the brightest radio pulses reported in the literature (data collected from


detected PAHs on subarcsec scales in about half of their sample of 29 nearby Seyfert galaxies.


They argued that the high column densities in the torus around the AGN would provide shielding that enables PAHs to survive, and the implied central star formation rate density was much higher than in the circum-nuclear region.


A similar conclusion about PAH survival was reached by Esparza-Arredondo et al. (2018) for their sample of 19 AGNs, based on the lack of relation between the X-ray luminosity and a central PAH deficit – while PAHs were detected in most AGNs, the equivalent width was lower in the centre.


Knots in SS433’s jet can be resolved at radio frequencies using very long baseline interferometry (VLBI) and indicate the presence of highly relativistic electrons


, while the baryon content is revealed by emission lines ranging from H and He lines in the optical through to highly ionized Fe lines in the X-rays


Further monitoring, predominantly at frequencies between 0.6 and 15 GHz, has since taken place (e.g.


Multilevel FIR transition lines have now been widely surveyed in local galaxies, originally by ISO (e.g.


Here different line features appear, more or less visible depending on the BH spin and radial distance, such as the clear iron absorption edge that occurs at around ∼6–7 keV (see e.g.


The Galactic sample of post-AGB stars have been found to be a very diverse group of objects


In contrast, a sub-population of backsplash cluster galaxies would be expected to peak significantly at $|\Delta \mathrm{V}|/\sigma _{r_{200}}\sim 0$ for values at or beyond our definition of the virial radius, with their fraction reaching zero at some upper limit (e.g.