Several modelling works on this comet have shown that ion composition in the coma varies based on the sublimation rate of the nucleus


as well as strong AGN/QSO and Supernova feedback that will heat and expel the gas (e.g.


Indeed, large atomic gas reservoirs, together with low molecular gas masses


indicate that GRB hosts are preferentially galaxies that have very recently started a star formation episode.


The spectral windows adopted for the analysis of the FOCAS and NIRSPEC spectra were taken to be similar to the rest-frame wavelength intervals commonly used to fit the continua of quasars


and Yoon (2016a, 2016b) discuss the wave generation in a self-consistent manner by solving the adiabatic dispersion relation and wave kinetic equation for each spatial location.


Consequently, the image separation distribution is consistent with the SDSS measured stellar VDF


and the Second Southern Sky Redshift Survey (SSRS2) inferred stellar VDF


although the two stellar VDFs are significantly different from each other concerning their corresponding parameter values.


Earth-like exoplanets, mini-Neptunes, and T-type brown dwarfs may form water clouds, composed of liquid or solid particles, but warmer planets and brown dwarfs of L-type and later have been shown to form cloud particles made of a mix of materials that is dominated by Mg, Si, Fe, and O and to a lesser extent by Ti, Al, K and other elements


In four LSP blazars (0333 + 321, 0430 + 052, 2145 + 067, 2230 + 114), the putative UV excesses are not included in our SED fitting, as they should come from the cold accretion disk


We derived AV(s) by adopting a simplified model of the local distribution of the interstellar dust density


expressed by the relation ρ = ρ0·sech2(z/hs), where z is the height of the star above the Galactic plane and hs is the scale-height of the dust, for which we adopted the value of 190 pc.


Especially during recent decades, high-resolution observations of solar super-fine structures indicate that small spicules, minor hot jets along small-scale magnetic channels from the low atmosphere upwards to the corona, petty tornados and cyclones, and small explosive phenomena such as mini-filament eruptions and micro- and nano-flares—all of these small-scale magnetic activities contribute greatly to coronal heating


NaCl was first investigated using a chirped-pulse Fourier transform microwave (CP-FTMW) spectrometer with a laser ablation source


operating between 6.0 and 12.0 GHz to sample swiftly the rotational spectra of the different species present in the supersonic expansion.


The long-slit based observations also have drawbacks: the morphology of ENLR is sometimes irregular so that the derived size depends on the orientation of slits


Then, observations of oscillation modes in


provided us new Rosetta stones to constrain the transport of angular momentum in the whole Hertzsprung-Russell diagram.


Despite some variations in survey depth and area, these survey parameters are similar to the ongoing Kilo-Degree Survey (KiDS), Dark Energy Survey (DES), or the survey with the Hyper Suprime-Cam


Many reports on the eruption of filaments are concerned with torus instability or/and kink instability


Many models in the literature also invoke the idea that AGN can effectively drive strong pressure-driven outflows and offset cooling if a large fraction of the accretion energy is thermalized


Dependent on the initial fields, varying weak (probably dominating) to strong r-process conditions can be obtained, the latter, however, only for precollapse fields beyond 1012 G


Only in a few rare instances has an appreciable shift in the location of the peaks been observed, e.g., the 1997 outburst of Mrk 501


and the activity of OJ 287 from the end of 2015 to the middle of 2017


More recently, other surveys also revealed that the fraction of high-EW Ly α emitters increases towards fainter UV magnitudes


We used a compensated filter to eliminate the small wavelength modes linked with such numerical noise


The behavior for the low- and high-dust contents is quite different.


On the one hand, the escape fractions versus NHI,cl scales for τd,cl = 1 (filled symbols in Fig. 12) as predicted by


in their “surface scatter” approximation


On the other hand, however, this is not the case for the low-dust scenario presented in Fig. 12 (with unfilled symbols) where a larger value of NHI,cl implies a lower fesc.


Mrk 421 is a very hard spectrum γ-ray source with a photon index of ≈1.77 and its semiminor and semimajor axes at 68 per cent confidence are of 0$_{.}^{\circ}$0067 as derived in


While X-ray variability studies can provide accurate information on the atomic and ionized matter on scales of the BLR, the radio emission from luminous H2O masers (the so-called “megamasers”) constitutes a fundamental instrument to study the geometry and kinematics of the molecular gas at sub-parsec distance from SMBH. H2O masers may trace distinct regions in the AGN environment, from nearly edge-on accretion discs to nuclear outflows in the form of jets or winds (for recent reviews see


The broad-band X-ray spectrum is orbital phase-dependent and can be approximately described as a power law with a high-energy cutoff and a cyclotron resonant scattering feature around 40 keV


The temperature Tcl of each cloud is determined as the result of a one-zone calculation (for details, see


Indeed, only lower limits to the high-energy cut-off have been found with NuSTAR (210 keV


Consider the following three possibilities: (1) If energetic particles maintain a highly beamed pitch-angle distribution (which requires negligible pitch-angle scattering), curvature drift energy gain strongly dominates generalized betatron energy loss, and for all practical purposes we have a first-order Fermi acceleration mechanism as a consequence of incompressible contraction or merging of curved flux-rope magnetic fields


In particular, the classical simplified approach of neglecting rotation in GCs has become untenable from the observational point of view. In fact, there is an increasing wealth of observational results suggesting that, when properly surveyed, the majority of GCs rotate at some level. As of today, more than $50{{\ \rm per\ cent}}$ of the sampled GCs show clear signatures of internal rotation (e.g.


Also, metals have been detected, using UV/optical absorption lines, around


The initially low polarization levels often rise during the plateau phase


with a polarization angle that typically remains nearly fixed throughout (e.g.


Nevertheless, the UV lines have so far mostly been used to detect absorbing gas with temperature range $10^5\, \mathrm{K} \lt T \lt 10^6\, \mathrm{K}$ from either O vi


We re-modeled fifty VLBA observations of 1308+326 obtained at 15 GHz (taken from the online MOJAVE archive webpage) between 1995.05 and 2014.07 with Gaussian components within the difmap-modelfit program


The modelfit program fits image-plane model components to the visibilities in the uv plane.


We did not apply self-calibration but used the calibration as provided by the MOJAVE team. Only circular components were used. The use of exclusively circular Gaussian components proved to be the most efficient way to parameterize the component properties. It reduces the number of free parameters, compared to the use of elliptical Gaussians, and allows a more secure identification of components across the epochs. Although it might have advantages to model the data of some of the epochs with elliptical components, our experience is that circular component modeling allows a more homogeneous analysis of all the epochs and more trustworthy identification of individual components in their long-term motion and evolution.


We used electron collisional excitation and ionization rates from the quantum mechanical computations of


A cometary nature of these NEAs was suggested and a conclusion was made that they are either extinct fragments of comet Encke or represent (together with comet Encke) the remnants of a larger comet-progenitor of the stream


For the former, we calculated the ion and electron temperatures in each cell of the post-shock medium, taking into account the effects of Coulomb collisions (see


Once the existence of a relationship between age and chemical clocks was established (see, e.g.,


In the equation above, Plin(k) is the linear matter power spectrum computed using the Boltzmann code CLASS


assuming the Planck 2015 (Ade et al. 2016) fiducial cosmology.


Numerous attempts to calibrate SZ masses have been made in the literature using


Andromeda hosts both very little gas and very little star formation, while the black hole is basically quiet and has some murmurs


while if we assume that redback companions are akin to the companions in CV systems whose outer envelopes have also been stripped through accretion, then we may expect a smaller value k2 ∼ 10−3


The case of solar pulsational stability has been studied in detail


have provided high-quality seismic data for stars of different flavours against which we can test models and further our understanding of stellar pulsations.


In this scenario, depending on the misalignment angle, the outer disk image will show narrow shadow lanes (e.g.,


Quasi-periodic oscillations (QPOs) have been detected from many Be binaries, such as


Yang et al. (2013) showed that at 2:1 and 6:1 resonances with a static/slab ocean (see Section 2.2.2 of


), Bond albedo is lower than it is for synchronous rotation and decreases rather than increases with incident stellar flux, thus destabilizing the climate as the planet approaches the IHZ.


The Sun is situated at the inner edge of the Orion arm


Here, for each of the terms we use the sign conventions given in the source code for the pulsar timing software tempo21


Frequently a major issue in these applications is the use of formulations derived assuming isotropy in turbulence that is actually anisotropic


, this being the typical case for solar wind and magnetosheath turbulence.


and found no Class II CH3OH masers in the sources of our sample


Simulations and theory together suggest that the magnetic field plays an important role in collimating the particles and giving them a jet like shape


A common mitigation strategy is to model the data as a Gaussian mixture of inlier and outlier distributions with differing variance


, we applied our method to 85 972 images from 9 Ca II K archives to derive plage areas and produce the first composite of plage areas over the entire 20th century. In particular, we analysed the Ca II K archives from the Arcetri, Kodaikanal (8-bit digitisation), McMath-Hulbert, Meudon, Mitaka, Mt Wilson, Rome/PSPT, Schauinsland, and Wendelstein sites. Five out of the nine analysed archives were amongst the most studied and prominent ones, while the remaining archives were from less studied data sources.


The strength of the UV-background heating is indicated by the dotted black curve. It represents the hydrogen photo-heating rate due to the UV-background photons following the model of


The latter is longer by roughly the mass ratio of Mars to Titan, which can be understood from Eq. (2) of


Unlike the subgrid recipes which involve kinetically prescribed decoupled winds and cooling-suppressed blastwaves, the FIRE simulations solve the ‘overcooling’ problem by explicitly modelling the radiation pressure, stellar winds, and ionizing feedback from young stars as taken directly from the population synthesis code starburst99


The galaxies presented by Bernard-Salas et al. (2009) have instead an average redshift of 0.0074, while the sample by


From studies on the optical–IR colour–magnitude diagram, it is known that FSRQs in general show an RWB trend, which is attributed to them having a luminous accretion disc


Mass transfer will continue for ≈1 Myr at a rate exceeding 10−9 M⊙ yr−1 until hydrogen shell burning is finished and the star contracts to become a carbon–oxygen WD with a thick helium layer and a small residual layer of hydrogen. The high accretion rate will heat the accreting WD significantly


It was found that the complex dielectric function from


for the sample obtained by heating bayerite at 1273 K, assuming a spheroid with depolarization parameters of (0.35, 0.003), produced an opacity with 11, 20, 28, and 32 μm features, so this component was included in the models.


For example, studies of young clusters embedded in moderate-mass MCs (∼104M⊙)


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


The Blandford–McKee blast wave of the ultrarelativistic shock moving into a medium of uniform external density ρ0 has radius R ≃ 2cT Γ2/(1 + $z$) and explosion energy per unit solid angle E/Ω ≃ ρ0R3Γ2c2, which gives Γ ≃ 9(Eiso, 53/n0)1/8(T/[(1 + $z$)day])−3/8, where $E=10^{53}\, \mbox{erg}(\Omega /4\pi)E_{iso,53}$ and n0 is the external density in cm−3


Note that such large values of the Lorentz factor of the emission region in the jet have been already postulated in terms of other models in order to explain extremely short flares observed in this source


Type II radio sources often show non-radial propagation trajectories (see Mann et al. 2003, and references therein). Wave-like large-scale disturbances propagating over the solar disk in extreme ultraviolet observations (usually referred to as âEIT wavesâ or âEUV wavesâ) are in close empirical correlation with type II radio bursts


In other words, the velocity equivalent of the observed line width, Wobs = c × Δλ/λ, at 1/e of the peak intensity results from instrumental, Doppler, and turbulence (non-thermal) broadenings by (1)\begin{equation} W_{\rm{obs}}^2 = \left(c\times \frac{\Delta\lambda}{\lambda}\right)^2 = W_{\rm{instrumental}}^2 + W_{\rm{Doppler}}^2 + W_{\rm{turbulence}}^2, \end{equation}Wobs2=c×Δλλ2=Winstrumental2+WDoppler2+Wturbulence2,assuming that all three line broadening components have a Gaussian profile (Eq. (4.17) of


In the fitting procedure the spectroscopic parameters (i.e., the rotational, centrifugal distortion, and fine structure constants) were kept fixed at the values derived by


The pexrav model assumes an exponentially cutoff power-law spectrum reflected from neutral material


n0 is limited between 10−5 and 100 cm−3, in line with what has been found in these sources


This affects weak and strong magnetic fields in the LoS magnetograms differently, with the daily variation remaining less than 30 G for field strengths below 1000 G and less than 75 G for field strengths below 2250 G. On average during a day this is roughly ±35 G


Nevertheless, the strength of these instrumental and observational effects does not account for the strong flux cancellation we observe in AR 11226 prior to eruption.


The presence of ISM grains makes it possible for the observed molecules to survive for a very long time, longer than 350 yr. The lifetimes in the presence of the large grains considered by


are typically a few times shorter than the age of the remnant.


However, the latest observations by Planck


indicate that there may be some problems with such an inflationary scenario


Their simulation results also reveal that the bipolar pulses reported in the Enceladus plume by


and Pickett et al. (2015) could most probably be ion holes.


The analytical expressions for the Sérsic model are taken from Prugniel & Simien (1997) (see also


SNe IIn span a wide diversity of late-time decay rates, ranging from some SNe IIn that have essentially flat light curves for many years, like SN 2005ip


down to those that have only weak CSM interaction and faster decline rates that are difficult to distinguish from radioactive decay or light echoes.


Recent works have studied lensing effects in the existing LIGO/Virgo O1 and O2 events


In fact observations show either no or positive relationships between star formation rates and SMBH accretion rates but no negative trends are seen


The third Fermi–LAT catalogue (3FGL catalogue:


has been used to include the contributions of sources inside the ROI.


Aside from electron dissociative recombination of C4H3NH+


neutral production of CH3C3N can occur in a few ways


Typical values for the underlying parameters are: $\varepsilon _{\operatorname{\text{p}}}^{\operatorname{\text{pin}}}\simeq 0.05-0.2$, $\varepsilon _{\operatorname{\text{p}}}^{\operatorname{\text{f}}}\simeq 0.1-0.5$ (see e.g.


Recently, quasars observed with multiple measurements, another potential cosmological probe with a higher redshift range that reaches to z ∼ 5, is becoming popular to constrain cosmological models in the largely unexplored portion of redshift range from z ∼ 2 to z ∼ 5. A sample that contains 120 angular size measurements in intermediate-luminosity quasars from the very long baseline interferometry (VLBI) observations


has become an effective standard ruler, which have been extensively applied to test cosmological models


An alternative scenario, such as dust formation in the KN that could also explain such a blue-red evolution, has been ruled out


The authors used their new results together with the available literature results covering up to z = 1.3


to further solidify the evidence supporting passive evolution and a formation redshift zform ≈ 2.


The upcoming LoTSS catalogs, covering a large sky area, will help us to explore further regarding


and the current puzzling dipole signal observed with radio catalogs


general-relativistic effects will rotate the polarization position angle along null geodesics from the corona towards the disc


and the situation becomes more general for incident disc irradiation, i.e. any incident state of polarization is possible. Our computations, apart from the unpolarized case, assumed two extreme cases of initial $p = 100\,{\rm {per \, cent}}$ polarization in order to estimate its possible effects in comparison with the completely unpolarized light and in order to test that the code adheres to the stated orientation conventions.


While spatially extended optical jets and bipolar CO molecular outflows have been observed in numerous Class 0/I protostars


near-infrared high-resolution spectroscopy and spectroimaging observations in the past two decades have made it possible to study the kinematics of the outflowing gas and physical properties at the base of the jet within a few hundred au of the driving source in Class 0/I protostars (e.g.


XRD of their sample obtained from heating boehmite to 1173 K


suggests δ-alumina to be present, though some amounts of θ-alumina and α-alumina are present, as they deduce from XRD and infrared and NMR spectroscopy.


AGNs can release copious amounts of energy into the intracluster medium (ICM) through many ways, including: jetted outflows that inflate cavities, weak shocks, sound waves, or turbulence in the ICM (e.g.


It has been shown that the fraction of AGN in mergers tends to increase as the separation between the two galaxies decreases


On the other hand, a positive correlation exists between the average Φ and the average Fidx with the linear PCC = 0.65 (refer to Figure 5(b)). Such correlation of Φ with flaring activity in individual ARs has been reported in many previous studies (e.g.,


We have compared to N-body simulations the well-known GSM


We have concluded that, among the three, QGQ is the only model capable of providing a precise redshift-space correlation function on scales down to ∼5 h−1 Mpc over the range of redshifts covered by future surveys.


As BHs are heavier than typical stars, they are expected to relax into the steeper cusps. The relaxation time of BH populations is much shorter: 0.1–1 Gyr


The background Alfvén or slow continuum can be due to the variation of the plasma density


Five other teams made independent detections of the same optical transient and host galaxy all within about one hour and reported their results within about five hours of one another


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


Internally, the ejecta release their energy through


and produce the prompt gamma-ray emission of GRBs.


The multi-DM search for single pulses (colored in yellow) on each of these visibility beams would need to be executed on a separate FRB cluster, followed by coincidence filtering to remove spurious events


In the obtained size distribution, erosive collisions are more important than catastrophic collisions (see Fig. 10 of


Taking into account the size distribution and erosive collisions, we derive t0 according to the collisional cascade (see Appendix E for derivation), (3)\begin{eqnarray} t_0&\sim& 1.3 \left( \frac{s_{\rm p}}{\rm 3000\,km} \right)^{0.96} \left( \frac{R}{\rm 2.5\,au} \right)^{4.18}\nonumber\\ &&\quad\times \left(\frac{\Delta R}{0.4 R}\right) \left( \frac{e}{\rm 0.1} \right)^{-1.4} {\rm Gyr},\label{eq:t0} \end{eqnarray}t0~1.3sp3000 km0.96R2.5 au4.18where sp is the size of planetesimals, R is the radius of the planetesimal belt, and e is the eccentricity of planetesimals.


Their presence at high redshift can be hardly explained by pure SFGs, even requiring uncommon assumptions (e.g., large stellar rotation, binary stellar population, top-heavy initial mass function, extremely low metallicity) as discussed by a number of recent works (see


When the characteristic time of variability of the mass flux along the accretion disk is longer than the relaxation time of the local disk equilibrium, it is possible to use the approximation of local equilibrium


see also Bisnovatyi-Kogan (2011), to calculate the transient disk structure.


The heating by jets propagating through the galaxies could prevent gas from cooling and cut-off the gas supply for further star formation


With such a bin width of ∼0.03 dex, any biases in ξ are less than $5{{\ \rm per\ cent}}$ of the observational uncertainty for a BOSS CMASS-like sample (see


As they pass by, they modify the transverse magnetic field and velocity components but, do not alter the gas pressure or the mass density


at least in the linear limit and in a homogeneous background plasma.


Power asymmetry from CMB data has also been a matter of intense debate and scrutiny


Although thermochemical equilibrium models predict the formation of condensate clouds with various composition in these hot atmospheres


recent laboratory works highlighted that photochemistry could strongly affect the composition of exoplanet atmospheres and lead to the formation of aerosols in a variety of conditions, including the ones encountered in hot Jupiters


Equation (16) describes turbulent fluctuations from a Lagrangian point of view


Similarly, Kamazaki et al. (2001) found small condensations of 1000 au scale inside the SM1 core in the Oph A region based on 3 mm dust continuum observations with the Nobeyama Millimeter Array (see also


The masses of the condensations are around 0.01−0.1 M⊙, comparable to or larger than the local Jeans mass.


The flares are accompanied by the variability of the equivalent hydrogen column density ($\rm \mathit{ N}_{\rm H}$) and of the fluorescent iron lines, which is believed to be associated with clumpiness of the stellar wind, launched from the donor star


Large uncertainties in VCME restrict further improvements to the TT prediction of the shock. Possible solutions to this restriction could include adopting the CME’s radial speed, which is derived from models (such as cone models) based on single spacecraft observations


The influence of tidal truncation is therefore limited to stellar multiples


or during the decay of higher order multiplicity


Many stars in the solar neighbourhood are born in regions where UV fields are sufficient to significantly shorten disc lifetimes


However, in Tomaru et al. (2019, hereafter Paper I) we show instead that thermally driven winds can explain this switch (see also


However, this may be an unlikely hypothesis, because A-type asteroids that could represent mantle material (almost pure olivine) from differentiated bodies do not exist extensively in the orbital space related to Psyche, but instead are distributed randomly in the Main Belt


When the line of sight to the compact object passes through one of these clumps, X-rays are absorbed by the moderately ionized material in the clump, leading to a so-called dipping event. This is also observed for other sources


This strengthened earlier results based on smaller samples (e.g.,


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


In this regard, the upcoming ADITYA-L1 mission


with the Visible Emission Line Coronagraph


will provide much better data and hence will help in arriving at much stronger conclusions on the evolution of CME legs.


during our last observing season as starting values,


Recent high-resolution hydrodynamical simulations of ‘zoomed’ cosmological haloes have shown that there is a significant difference between the velocity distributions of DM particles and galaxies themselves; whether galaxies (i.e. overdensities of stars in hydrodynamical simulations) or DM subhaloes are used makes comparatively little difference


Interaction of CRs with molecular clouds is accompanied by various processes generating observable radiation signatures, such as


as well as production of neutral pions whose decay generates gamma-rays in the GeV (e.g.,


The distance to GoHam is not known precisely, but a value d = 250 ± 50 pc is required to satisfy all the existing observational constraints


We here adopt this value with the uncertainty.


Figure 13a shows that this evolution exhibits three distinct phases: (i) the early phase (between t = 0 and 250 s), where the velocity growth occurs exponentially (linearly on the logarithmic-linear scale), which is called the linear growth regime; (ii) the middle phase between t = 250 and 665 s, where the growth rate is slower compared to the linear phase, which is called the Rutherford regime


and (iii) the final phase, which starts at t = 665 s, where the instability suddenly develops in an explosive way, and finally saturates at a later time, which we call the post-Rutherford regime.


This model was successfully applied to explain several observed core distances


however it is not able to explain all observations


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


spiral shocks associated with very young binary systems orbiting within a circumbinary disc


Recent studies increasing the statistics of sources with detection of molecular outflows have widened the range of measured energetics (e.g.


While the Loison et al. (2015) CH3C3N model corroborates the upper atmospheric abundance of C4H3N inferred by


a large disparity between the photochemical models (and within the ensemble of models produced by Loison et al. 2015) arises in the lower atmosphere due to the poorly constrained C4H3N branching ratios and reaction rate coefficients at temperatures appropriate for Titan.


In the case that there is an MS star close to an AGB star, a substantial fraction of the mass loss may be accreted onto the MS companion


As a result, the metallicity of the companion may change. Such early stage low-mass stars become chemically peculiar, and their future evolution will be strongly affected.


Even more interestingly, the detection of multi-periodic brightness variations in low-mass WDs


has brought about new classes of pulsating stars known as ELMVs and pre-ELMVs, respectively (ELM and pre-ELM variables, respectively).


Overall, we find that constraints on tides, radius, possible p–g instabilities


and the EoS from GW190425 are consistent with those obtained from GW170817


For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm−3 is assumed


To convert from surface brightness to density, we use the following widely used approach


Nogueras-Lara et al. (2020a) have used the luminosity of red clump stars to conclude the majority ($\sim 95\, \mathrm{per\, cent}$) of the nuclear stellar disc formed more than $8\, \mathrm{Gyr}$ ago with some evidence of a more recent ($\lt 1\, \mathrm{Gyr}$ ago) star formation burst


This is consistent with ongoing/recent star formation within the central molecular zone


and is broadly consistent with the conclusions of Bernard et al. (2018) on the wider bar/bulge but possibly suggesting the nuclear stellar disc is on average older than the surrounding bulge.


Furthermore, our photometric data also constrain the long-term variability of DES17X1boj to a level below what was seen in SN2009ip


in the years before the brightest event (MV in range −13 to −14).


The orbit has a period of ∼10 days (typical value of Kepler planets), and it is sufficiently close to the central star to be subject to significant photo-evaporation effect


Using the J0740 proper motion value from Table 1, the Sun’s Galactocentric velocity and the distance (240 km s−1 and 8.34 kpc, respectively;


we calculated these corrections to the pulsar period derivative: $\dot{P}_{\rm S}=3.0\times 10^{-21}$, $\dot{P}_{\rm G,\perp }=-1.6\times 10^{-22}$, $\dot{P}_{\rm G,p}=3.8\times 10^{-23}$ for the minimum and $\dot{P}_{\rm S}=6.9\times 10^{-21}$, $\dot{P}_{\rm G,\perp }=-2.2\times 10^{-22}$, $\dot{P}_{\rm G,p}=8.9\times 10^{-23}$ for the maximum pulsar distance estimates.


AREPO has been used to produce simulations of the Universe at a wide range of scales. At the largest scales, we have uniform volume cosmological simulations such as the Illustris


suites. These simulations have box sizes ranging from ∼50 to ∼300 Mpc and baryonic mass resolutions ranging from ∼105 to 107 M⊙.


In addition, the linear polarization P.A.s across pulse phase can constrain the beam size and inclination angles, with respect to the pulsar’s rotation axis and our line of sight (LoS). For example, the rotating vector model (RVM) predicts a smooth ‘S’-shape, due to the projected vectors of the magnetic field lines as they sweep across our LoS (e.g.


This trend is consistent with previous results in the literature, which have shown that large-scale bias is more strongly correlated with halo-centric overdensity than it is with halo mass (see e.g.


BCGs constitute a special category of objects with peculiar star formation histories (SFHs) seen from both observations


Studies of SMGs over the past few tens of years have provided valuable insights into their properties. These include


From the median values of $\bar{\mathcal {R}}_{190814}=7\rm \, Gpc^{-3}\, yr^{-1}$


we obtain the effective surveyed space–time volumes $VT=1.2/\bar{\mathcal {R}}$ for each of these three events (‘1.2’ is the median of $\mathrm{d}P/\mathrm{d}\mathcal {N}$).


Alternatively, such a change in the PA can be obtained due to magnetic reconnection, e.g. in the ICMART model


where the local magnetic field orientation, which is orthogonal to the wave vector of the emitted photon, itself changes by 90○ as the field lines are destroyed and reconnected in the emission region


We used dmcopy tool in CIAO: Chandra's data analysis system


to restrict the energy range to 0.7−7 keV for both imaging and spectral analysis in all of the four data product files: event file, blank-sky observation, RMF and ARF.


Perhaps more customary today, and equivalently, is to introduce a hierarchy of formally independent time variables (e.g.,


In addition, there are no dust condensations along the direction of isolated synchrones, which could have indicated short bursts of activity


or several separated short bursts, as in the case of P/2013 P5


The prompt emission of GRB 090709A possibly showed evidence of a periodic signal


however this was ruled out with a more careful analysis of the prompt data from BAT, X-ray Telescope (XRT) and X-ray Multi-mirror Mission (XMM) observations of the X-ray afterglow


However, in the majority of these studies, the authors have targeted a constant spin period whereas a magnetar central engine is expected to have a rapidly decelerating spin period which would be very difficult to detect in standard searches for periodic signals.


have found a +208 ± 110 ppm difference between the 3.6 and 4.2 μm bands, suggesting CO2 absorption.


While kink waves, both propagating and standing, are routinely observed in the corona (e.g.,


The investigations developed by Marcus et al. (2010) and


suggest that incorporating a realistic model of volatile transport and removal in an N-body code, may lead to reduced water contents on the resulting terrestrial-like planets, in comparison with those derived from classical models that assume perfect mergers.


The use of Planck and WISE data resulted in the discovery of the brightest known, dusty starburst galaxy at z > 1, the “Cosmic Eyebrow”


which has also been independently recovered as one of the LPs presented in this survey work.


Classical bulges might have formed as a result of


It is interesting to note, however, that if we assume a steeper exponent for the distribution function described by Eq. (7) (i.e., q = 0.80), we get a very good match with observations at all fluxes, when assuming a flux-dependent scaling factor (k = k(S); see Eq. (9)) for the


median size – flux relation (black solid lines on the right).


Line luminosities of detected CO-bearing disks span almost two orders of magnitude, in which the brightest disks have luminosities that are comparable to those of fainter Herbig Ae and T Tauri disks


While for operational reasons, S4 could not be measured close to the dust impacts, S4 was clearly identified in periods where the coma was very dusty


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 (e.g. thermodynamics of the host galaxy interstellar medium;


obtained additional imaging data of about 3000 deg2


These authors compute the collisional rate coefficients for collisions with electrons, either using perturbation methods such as those used by


In this scenario, the present γ-ray emission from the Fermi bubbles arises predominantly through inverse Compton scattering of an energetic non-thermal cosmic ray (CR) electron population in the remnant structures with ambient radiation supplied by the interstellar radiation field (ISRF) and the cosmological microwave background (CMB). A subdominant component due to non-thermal bremsstrahlung may also be present, emitted primarily from regions of high gas and non-thermal electron density within the bubble (OY22). Models of this nature are broadly referred to as ‘leptonic’ models (see also


Although the contribution from discrete sources in the ROSAT data cannot be subtracted as accurately as it can for Chandra data, their contribution is only about 1 per cent of the diffuse gas luminosity for these high-mass galaxies (see


Infrared and submilimetre observations of


confirm the presence of ∼0.1–1.0 M⊙ of dust, indicating that a substantial fraction of refractory elements in their ejecta went to dust grains.


The use of the geodesic equation for a quasi-particle must be questioned, if this particle associates with pure quantum fluctuations


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


there is now ample evidence that there is no tight universal relation between the UV slope and the attenuation (e.g.,


The LPT for dark matter fluctuations in MG was developed in Aviles & Cervantes-Cota (2017), and further studies for biased tracers in


Among the rich variety of low-frequency waves observed in the Sun’s atmosphere, flare-related quasi-periodic fast propagating wave trains have received much attention


Their quasi-periods usually range from 25 to 400 s. These wave trains were


and extensively observed in images acquired with the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory (SDO/AIA;


In Table 3 we provide the coordinates, radial velocities, and the sum of the equivalent widths for the cluster member stars, both measured (“m”) and corrected (“c”) to the system of


In this paper, we consider an analysis of the PDF at redshift z = 1 in a survey volume of V = 100(Gpc h−1)3, which is smaller than the effective volume of upcoming surveys such as Spherex with Veff ≈ 150(Gpc h−1)3 and somewhat larger than existing surveys such as BOSS with Veff ≈ 55(Gpc h−1)3


However, there are increasing studies suggesting that a lower-mass binary scenario is more favorable for most SNe Ib/c, considering the measured low ejecta masses


At present, data from large-scale spectroscopic surveys


have led to the discovery of this trend at different galactocentric radius, R, and average height, |Z|, across the Galaxy shedding light on the disc formation and evolution scenarios.


Some studies have indicated that not only [C II] emission is deficient in some sources, but other FIR cooling lines ([O I], [O III], [N II]), as well (e.g.,


In particular, two major categories of MR have been proposed: the steady state model with a single X line and the outflow approaching the Alfvén speed


The identification of Ka = 0 and lower-frequency Ka = 1 transitions, originating from J0 J and J1 J energy levels, was relatively straightforward and their assignment and analysis could be easily expanded up to 340 GHz (J˝ = 64) with the help of the Loomis-Wood-type plot technique from the AABS package


in the last decades there has been a debate on the coefficient of the metallicity term of the KB and PL relation (see e.g.


High velocity outflows from AGN host galaxies have been reported in numerous studies in the literature


The results obtained with these methods appear to be strongly dependent on a few assumptions, e.g., the degree of the polynomial adopted, the photometric technique, the centroid determination, calibrating instrument systematics over the out-of-transit only or the whole observation (e.g.,


identified C- and D-type asteroid spectral features for both prograde and retrograde families based on spectroscopic observations of JV-JXIII and suggested them to be similar to Jupiter’s Trojan asteroids.


In L1544, the 14N/15N ratio of several different molecules has been measured:


The crystallization age of EC 002 also predates all those of the other dated achondrites, such as


However, Simpson et al. (2015) point out that the submillimetre sizes are consistent with resolved 12CO detections, while the sizes derived from 1.4 GHz imaging are about two times larger because of the cosmic ray diffusion, which can explain the results before higher frequency observations at ALMA were possible


For comparison, to obtain the Hubble Ultra Deep Field (UDF) image, ∼400 hr of actual observation time (∼1 yr in real time) was needed


A tight relationship between O/H and N/O abundances is indeed observed in both H ii regions and local galaxies, especially at M⋆ ≳ 109.5M⊙


Other works report, however, that LiRG can be randomly located in the HRD


The distinction is crucial to understanding the processes that may provide an explanation for the phenomenon,


One can show that the spatially varying background magnetic fields lead to the adiabatic focusing effect of charged energetic particle transport and introduces correction to the particle diffusion coefficients (see, e.g.,


Using the relatively strong neutral lines (i.e., “O i” 1355.60 Å and “S i” 1401.51 Å), we also perform an absolute wavelength calibration for the spectra at the “O i” and “Si iv” windows, respectively


Newer, alternate cosmological probes could help alleviate this issue. Recent examples of such probes include


QSO angular size measurements that reach to z ∼ 2.7


Here, we have included excitation through infrared pumping for all studied species, mostly through bands lying in the mid-infrared, where the flux in IRC +10216 is large


After a significant fraction of the core has crystallized, the temperature approaches the azeotropic point and the existing calculations indicate that the liquid phase is enriched in 22Ne relative to the solid


The mean speed of network jets is very similar, as reported in previous works (e.g.,


Theoretical stellar libraries like, e.g.


are generally available for both a large range in wavelength and in stellar parameters, whereas empirical libraries are found to be more incomplete in both respects. However, the advantage of the latter ones is that they are not hampered by the still large uncertainties in the calculation of model atmospheres.


The transverse velocities of pulsars (based on proper motion and distance estimates) are particularly large, with a mean close to 310 km s−1


Since for this present UM, the estimation of H0 from CMB alone is compatible with the local estimation of H0 by


thus, we can safely add both the data sets to see whether we could have something interesting.


The rationale behind this search is that the radio lobes of these AGNs are most likely bent because of the ram pressure that occurs due to the relative motion of the AGN host galaxy and the ICM (e.g.,


, which makes these sources good tracers for finding galaxy clusters.


significantly increased the size of LAEs samples used by stacking ≈2000 and ≈4500 LAEs at redshift z ≃ 3 and 2.2 ≤ z ≤ 6.6, respectively.


found typical Lyα halo exponential scale lengths of 5–10 physical kpc.


The line force is exerted mainly by the radiation flux in the UV band (200–3200  Å), because the metal lines are densely distributed (e.g.


Other studies have used similar methods for budgeting oxygen


A harvest of astronomical observations from ground-based telescopes (e.g. UKIRT, IRTF, CFHT, and VLT) or satellites (e.g. IRAS, ISO, Akari, and Spitzer) of such lines of sight has led, since the late seventies, to the deciphering of the chemical compositions, column densities, and variations associated with these ice mantles (e.g.


The dynamics of the cyclotron line was shown to be dependent on the luminosity state of XRPs (see


The term φi + 1/2 is the so-called flux limiter


A large proportion of the spiders, whether BWs or RBs, have been observed to exhibit (quasi-)periodic eclipses of the pulsars’ radio emission (e.g.


that are generally attributed to excess material in the orbits


interfering with the propagation of the radio emission.


Studies of such eclipses are key for understanding mass loss from the irradiated companion stars, the properties of the medium causing the eclipses, interactions between the pulsar wind and the eclipse medium, and the mechanisms responsible for the apparent attenuation of pulsar radio emission during the eclipse.


This basic idea has allowed the development of global “Enthalpy-Based Thermal Evolution of Loops” (EBTEL) models that describe the evolution of the average temperature and density in the coronal part of the loops;


these models are generally in good agreement with one-dimensional hydrodynamic simulations


Alternatively, it is recently proposed that VHE gamma-rays from distant blazars may be the secondary gamma-rays produced in the rectilinear propagation of the UHECRs escaping from these blazars (e.g.


In the latter case, UHECRs interact with background photons, i.e. EBL photons and microwave background (CMB) photons, which creates UHE electrons and photons through Bethe–Heitler (BH) pair production and photo-meson production. These UHE electrons and photons would interact with background photons again, and then pair cascades are induced; the secondary photons are inverse-Compton-scattered (ICS) CMB photons by the pair cascades.


whereas KEPLER was used to evolve the star along zero age main sequence and calculate nucleosynthesis yields and light curves


The observational analysis of PDRs, H II regions, and IBLs has improved considerably since the availability of far-infrared spectroscopic data from the Herschel Space Observatory (see


The timescale on which the coronal rain forms following the heating onset is much shorter than for the quiescent scenario; in the studied event condensations appear 10 min after the reconnection event, whereas observations of quiescent rain suggests it recurs in the same loop of the order of hours


An individual star-forming galaxy is expected to evolve along the relation of star-forming galaxies in the mass–size plane


while the average size of the population as a whole increases with decreasing redshift due to processes such as mergers


and ’puffing up’ due to strong active galactic nuclei (AGNs) feedback


but also new galaxies forming with larger radii


These outflows can explain the nearly constant temperatures inferred from the spectrum of optically bright TDEs


There is evidence for a few additional smaller shock fronts throughout the cluster volume


In support, observations of V404 Cyg do indicate the source


and was enshrouded by rapidly varying Compton-thick outflowing material


We segmented the sky into equal-area pixels using the HEALPix scheme


The derived central engine parameters are sometimes ad hoc or inconsistent. For instance, the analyses


led to a curious conclusion that the bulk Lorentz factor of the outflow of different layers are decreasing with time. This would lead to no, or at most very inefficient, internal shock emission. Yet both bursts have dominant non-thermal emission.


observe two sequences in the inner regions.


The thermal emission from the aligned dust grains is then polarized with polarization segments perpendicular to the field lines


The two coherent emission mechanisms are


and electron cyclotron maser (ECM) emissions


Nevertheless, there are examples of weakly magnetized WD pulsars, which can be explained even in the GR framework, e.g.


where magnetic fields hardly affect their mass–radius relations.


Both categories of method have been applied to large stellar spectroscopic surveys, including


A similar decrease of eZ,rel,int with increasing mass is found for the bulk metal content of Solar System giants


where the mass where eZ,rel,int reaches 1 is extrapolated to be at about 11 MJup.


The scaling laws derived from the numerical simulations of downward overshooting


agree well with Zahn’s analytical model.


Together with the findings of Blum et al. (2020), our results have important implications for the analysis of time delays and a potential solution to the H0 tension


The resulting gas density probability distribution function


with an additional few per cent of the mass in a power-law tail at high density


This discrepancy in results might originate in the nature of the collisions studied in these different experiments:


and Higa et al. (1996) performed collisions of a particle with a flat surface, while Heißelmann et al. (2010) observed particle-particle collisions in a free-floating environment.


The minimum gap-opening mass depends on the viscosity and scale-height of the disc


We confirmed that this is indeed negligible for [O i] 6300 Å emission based on observations of comet C/2012 S1 (ISON) that were performed at a similarly high airmass with ARCES, and found that the production rates derived from the ISON [O i] 6300 Å measurements were consistent with values determined using other methods


Among the better recent claims of QPOs in the gamma-ray band are of


found as part of a continuing analysis of blazar Fermi–LAT observations.


Matthaeus et al. (2007) presented a similar spectrum in different regimes: energy range, inertial range, and intermediate regime where the spectrum is proportional to k−1 to coincide with observations


Previous studies have considered the implications of structure models


on the shape of the afterglow light curve


However, comparing the observational constraints reported in Table 3 (without R18 data) and Table 4 (with R18), one can see that the inclusion of R18 data


does not seem to improve the constraints on the model parameters. In fact, the estimation of the Hubble constant H0 remains almost similar to what we found in Table 3.


According to recent theoretical analyses of gap structure around a planet


the depth and width of the gap are controlled by the planetary mass, the turbulent viscosity, and the gas temperature.


It is found that generally the FIP bias is higher in AR and QS regions (mainly occupied by closed loops) than in CH regions (generally taken up by open magnetic field lines)


MBHBs are in fact expected to emit a large amount of EM radiation in different bands


and possibly even through pre-merger signals


The distance of this source is around d ∼ 11 kpc


Many studies suggest that BH growth precedes spheroid assembly


however, other studies find no significant evolution with redshift (e.g.


Electrostatic solitary waves have been observed in Saturn’s magnetosphere


Because the relatively small [Na/Fe] variation is expected from the chemical evolution model for metal-rich bulge stars and the O-depletion is indistinct in some metal-rich GCs, such as NGC 6121 and 47 Tuc (see


the direct comparison of bulge stars with similarly metal-rich GCs on the Na–O plane would require further spectroscopic observations for such GCs in the bulge.


The fact that disc accretion rate was not the single factor that controlled the size or temperature of the Compton cloud, used to model the hard state spectra, lead to the conclusion that some unknown parameter, related to the truncation radius of the disc, is responsible for the hard X-ray tail


Vázquez-Semadeni, González-Samaniego & Colín (2017) have recently shown that the simulations of Colín et al. (2013) in fact produce stellar age histograms highly resemblant of the observed ones


On the other hand, the discovery of isolated L dwarfs in young clusters


and very cold very nearby Y dwarf objects (e.g.,


show that very low-mass isolated brown dwarfs exist and overlap with the planetary masses.


Based on this evidence, Troja et al. (2017) suggested that a structured jet model (e.g.


provided a coherent description of the entire broad-band data set. Within this framework, the peculiar properties of GRB170817A/AT2017gfo could be explained, at least in part, by its viewing angle


On the other hand, it is also suggested that the gamma rays could be emitted by the hadronic processes. The relativistic protons accelerated in the Crab pulsar outer gap interact with the matter inside the nebula. and this process may contribute in the high-energy gamma-ray range (see, e.g.,


X-ray reverberation in black hole X-ray binaries was first robustly detected in GX 339–4 by


and fit Kurucz ATLAS9 stellar atmosphere models


Such mini-outbursts or night-side activities have been observed before at


and comet 103P/Hartley 2 by the EPOXI mission


Under the assumption of the steady state of collisional cascade, the power-law size distribution of bodies is analytically obtained and the power-law index depends on the size dependence of the collisional strength of bodies (see Eq. (32) of


The radial velocities show a distinct and well-known gradient across the SMC with higher velocities in the eastern part (see also fig. 5 of


High-resolution mid-infrared (MIR) interferometric observations have revealed a two-component morphology in the brightness distribution: (i) a larger scale, elongated component in direction of the ionization cone (along PA ≈ 107°) with a full-width at half-maximum (FWHM) size of roughly 0.8 × 1.9 pc, which is responsible for 80 per cent of the total MIR flux and was interpreted either as the directly illuminated funnel walls of the dusty molecular torus or as part of the (filamentary/clumpy) outflow; (ii) a disc-like component with an FWHM size of roughly 0.2 × 1.1 pc and elongated along PA ≈ 46°


and in the seeding of large-scale magnetic fields in the universe (e.g.


These bright PNe seem to resemble the younger, metal-rich population in the outer stream of M31, as revealed by HST pencil-beam pointings on the Giant Stream


The properties that make RR Lyrae standard candles are


the period–luminosity relation in the near-infrared (NIR) filters and in particular in the K 2.2 μm band (see e.g.


Among these, the very nature of the turbulent cascade of the solar wind flow and its relationship with the small-scale processes still need to be described in full


This is basically consistent with the detection rate and the distance distribution of BH–NS merger candidates detected during LVC O3 (e.g.,


The characterized convex synchrotron radio spectrum peaks at around 100 MHz in the case of compact steep spectrum (CSS) sources, at about 1 GHz in the case of GHz-peaked spectrum (GPS) objects, and up to a few GHz (e.g., 5 GHz) in the case of high-frequency peakers (HFPs;


exist that favour a compact corona, we used extended coronae.


observations exclude nearby CSM at high significance.


Mid-IR (MIR) and far-IR (FIR) observations have revealed bright atomic lines from H ii regions ([S iii], [Ne iii], [Ne ii], [O iii], etc.) and PDRs ([C ii], [O i]) (e.g.,


Those blended emission lines can be easily detected at the position of the flare ribbon, including known and unknown emission lines, such as the C i line at 1354.29 Å, the Fe ii lines at 1353.02 Å, 1354.01 Å, and 1354.75 Å, the Si ii lines at 1352.64 Å and 1353.72 Å, and the unidentified lines at 1353.32 Å and 1353.39 Å (e.g.,


Some multiscale polarization observations and numerical simulations suggest that turbulent motions, rather than magnetic fields, are dynamically important to form complex gas morphologies of protostellar envelopes


was used, with the variable errors handled according to York (1966) in the implementation of Tellinghuisen (2020).


These are produced from the collapse of the helium core of a red supergiant that had lost most of its hydrogen envelope before exploding, so the ejecta expand into the stellar wind from the pre-SN star


We use a fully coupled ocean model because alongside atmospheric heat transport, ocean heat transport plays a vital role in the climate of Earth


Importantly, the instrument on board Cassini, the Radio Plasma Wave Science instrument, does not have the ability to determine the polarity of the electric fields associated with the ESWs observed with 100% certainty as it lacks the ability to perform interferometry


The first identified phosphorus compound in the ISM was PN through observations of its rotational transitions in Orion-KL, W51M, and Sgr B2


While we do not find the signature in the ACF amplitude, this does indicate that a [Fe/H] dependence might be expected, as was also suggested by 3D hydrodynamical simulations of convection


the Chandra 4 Ms source catalog in the CDFS field


The typical sensitivity limits of these X-ray data are


∼10−17 to 10−16 erg cm −2 s−1 for the CDFS and HDFN fields.


However, the virialization of dark matter perturbations in the non-linear regime cannot be independent from the properties of DE


which demonstrated that the preliminary track annealing led to unpredictable changes in track lengths, resulting in a lower accuracy of nuclear charge determination.


For SIBEC-DM given by the field Lagrangian in Eq. (1), the self-interaction is constrained to Rc  1 kpc, otherwise an early radiation-like period and a large comoving Jeans’ length washes out too much structure to be consistent with observations


This stochastic acceleration process typically causes the particle distributions to have a pronounced curvature in the energy spectrum


Due to its simplicity and in order to allow comparison with previous work (e.g.,


), we used the cutoffpl model for all subsequent analysis.


Cosmologists have worked hard to decipher the dark energy code, but we still ignore the physical nature of the DE and hence of the ultimate cause of the observed acceleration of the Universe. Such theoretical conundrum is the so-called Cosmological Constant Problem (CCP)


The dashed blue line is the limit above which a halo must grow in order to overwhelm the impact of LW radiation, Mmin, LW


, we derived the precession time of T ≈ 530 yr.


This value is quite large for the wiggling waves that we see.


Such a gap could be opened by a super-Neptune-mass planet, depending on the parameters of the disk, such as the turbulent viscosity


In this context, the investigation of the evolution of group members in the nearby universe acquires a great cosmological interest because more than half of galaxies reside in such environments. Furthermore, since the velocity dispersion of galaxies is significantly lower in groups than in clusters, the merger probability and the effects of interaction on galaxy evolution are much higher. Consequently, groups provide a zoom-in on phenomena driving the galaxy evolution before the galaxies fall into denser environments (e.g.,


Over the past decade, many attempts to address this issue have been carried out, such as from the perspective of conventional nuclear physics and even exotic physics beyond the standard BBN framework


If there is no break in the spectrum, the energy budget for these particles would be untenable


This electric field is generated by the density gradient and different mobilities of electrons and ions


We can assume additional trapping due to the interaction of hydrogen with helium in the material, since helium bubbles serve as trapping sites for hydrogen atoms through synergistic effects


, leading to a lower critical dose in the case of mixed hydrogen and helium exposure


The technique was originally devised under the premise that the intervening absorption lines in QSO spectra arose from discrete absorbing clouds, but this picture was challenged early by the smoothly distributed IGM captured in cosmological hydrodynamical simulations (e.g.


interferometric observations in the (sub)millmetre domain


In addition, observations of magnetic fields in voids provide bounds on their strength, depending on the analytical model: From the simplest ones, it is possible to obtain lower bounds, although when improving such models a bounded range of magnetic field strength values can be provided, ranging from 10−25 to 10−15 nG


From observations, field stars in dwarf galaxies do exhibit different abundance ratios from MW field stars, e.g. lower [α/Fe] ratios and variations in neutron-capture element ratios at intermediate metallicities. However, these typically do not show up until [Fe/H] ∼ −1.5


Since 2006, it has been suspected that mergers of compact objects could also produce the so-called long–short GRBs (also known as the supernova-less long GRBs, which are apparently long-lasting but do not show any signal of supernovae down to very stringent limits), which share some properties of both long- and short-duration GRBs


Interesting explorations on the origin of PCEB (and specifically sdB+MS/BD) circumbinary planets can be found in Zorotovic & Schreiber (2013),


Bear & Soker (2014), and Völschow et al. (2016).


In fact, the E0 distribution for the high κ solution is qualitatively similar to the FIDO one


Secondly, there is growing evidence that the mass of any classical bulge, if present in the Milky Way, must be small


For these reasons, we prefer to present a second model, our Model II, which does not include any spherical central component, and which is still compatible with the rotation curve of the Galaxy, as given by Reid et al. (2014).


near-infrared high-resolution spectroscopy and spectroimaging observations in the past two decades have made it possible to study the kinematics of the outflowing gas and physical properties at the base of the jet within a few hundred au of the driving source in Class 0/I protostars (e.g.


In our MHD simulations, βrot is adopted to be 0.4% based on the observational estimates of the core mass of ∼1 M and the angular speed of the core rotation of 4 × 10−14 s−1. The angular speed was estimated based on the global velocity gradient along the major axis of the dense core observed with single-dish telescopes


A complementary result is the following: when the initial condition has positive net flux and its negative part has compact support, then the whole solution evolves into a positive function after a finite time


The Artificial Neural Networks (ANNs) have found application in not only the traditional tasks in extragalactic astronomy


but also in more specialized problems such as


In the visual passband, the luminosity L depends on Z in the form of the so-called RR Lyrae luminosity–metallicity relation (see e.g.


In the former scenario, galaxies experience a mass-loss from wind driven by active galactic nuclei (AGNs) or supernovae feedback, which lead to an expansion in size due to a change in the gravitational potential. In the latter, mergers either major involving merging with another galaxy of comparable mass, or minor that involves accretion of low mass companions, have to be dry to keep the low star formation rate


We approximate the NS as a polytropic star of index n = 0.5 (e.g.,


The turning point of increased relative production of carbon from massive stars takes place at A(O) ~ 8.7 dex (see Fig. 2 of


This observed behaviour of [C/O] is in contrast to the steady increase of [C/O] up to [Fe/H] ~ 0.3 dex found, for example, by Franchini et al. (2021).


and that of the gamma-ray emission about the hadronic process have been also investigated (see, e.g.,


However, with the establishment of more and more high-energy observatories, some telescopes have possessed the performance of observing photons of exceeding to the PeV from the astronomic objects.


The JAGUAR catalogue provides emission line fluxes and EWs for the main lines based on modelling with the beagle code


Toward this goal, conventionally, new summary statistics that can only be measured with imaging have been proposed. These include the three-point correlation function


Direct detection of progenitor stars is still elusive for SNe Ic, which prevents us from further testing the theoretical evolution of massive stars


FTD models driven only by the Babcock–Leighton mechanism


currently have the best agreement with observations


because the length of the simulated overlap is short and it occurs only during the minimum at low latitudes.


In some sources it has been found that coronae can have extremely high energy cut-off (e.g. NGC 5506,


and therefore thermal energy, which is inferred by measuring the curvature of NuSTAR spectra at high energy and in this context K–N effects cannot be neglected.


This work focused on the chemistry in atmospheres with T > 1000 K and a C/O ratio of 1 (representing C enhancement compared to the solar value of 0.54), because chemical models predict that the abundances of hydrocarbon and nitrile species increase by several orders of magnitude in these atmospheres compared to atmospheres with a low C/O ratio


Therefore, they can be considered as better candidates for the formation of complex organic molecules with longer carbon chains.


As of today, many more mass ejection channels have been discussed: matter that becomes unbound on secular time-scales (∼1 s) from the post-merger accretion torus


and do not fully rule out a spatially non-flat Universe


Meanwhile, enormous efforts have been made to refine the reaction rates of key BBN reactions in the past 20 yr


but the probability of solving or alleviating the 7Li problem by improving our knowledge of relevant nuclear reaction rates still cannot be eliminated.


The comet's surface revealed a wide diversity in morphology such as layering


The morphology resulting from this particular type of wind–binary interaction is shown in Fig. 3 in


In reality, the MW stellar halo contains a wealth of substructure that is not yet phase mixed, in the form of stellar streams (e.g.,


The key achievement of LPF was placing two gold-platinum cubes known as “test masses” into a freefall so pure that it was characterized by accelerations at the femto-g level (e.g.,


the level required to detect the minute disturbances caused by passing gravitational waves.


Grillo, Lombardi & Bertin (2008) introduced a methodology to estimate cosmological parameters using strong-lensing systems (SLS; see also


However, if a single stellar loop were flaring, the cooling time of the confined plasma would be proportional to the loop length


However, the discovery of ubiquitous propagating transverse oscillations with CoMP


led to the possibility of continuous diagnostics in time, i.e., dynamic coronal seismology.


Because of the faintness of the transient and its proximity to the larger, brighter main source, an automated detection algorithm such as SExtractor


implemented in GAIA36 2016A, was unsuccessful in deblending the two sources.


For example, SNe that explode within dense molecular clouds may be limited to disrupting their natal gas clouds, whilst SNe that explode into lower density environments can drive hot expanding bubbles to much larger distances (tens to hundreds of pc) and influence galactic scale processes (e.g.


Simultaneous observations were made with


Especially for late M dwarfs the cut-off at 4.545 μm leads to non-negligible loss in incoming radiation of up to ≈5% (see also


Hence, HZ boundaries obtained with the models lie closer to the star than would be expected when accounting for this missing portion of irradiation.


Particles up to gigaelectronvolt energies are accelerated by strong shocks driven by CMEs of very high speeds (∼2000 km s−1) and intense, soft X-ray flares (see


Theoretical work suggests major mergers can provide the torque to displace such an overwhelming fraction of the angular momentum of the gas, allowing for the highest accretion rates on to the central black hole whilst transforming the galaxy morphology


As relevant observational evidence is steadily growing, particular attention has been devoted to tackling with SNR temporal evolution in an inhomogeneous medium, aiming at deciphering the observed asymmetries of emission morphology or clarifying the effects on the synthetic radio polarization maps exerted by various configurations of the interstellar magnetic field (e.g.,


In order to make the sample as complete as possible, we retrieved and added all known spectroscopic RSGs in both optical and mid-infrared (MIR) bands from Simbad


In Table 3 we provide the coordinates, radial velocities, and the sum of the equivalent widths for the cluster member stars, both measured (“m”) and corrected (“c”) to the system of


This type of geometric configurations for the BBH–disk accretion systems has been revealed by many numerical simulations and analysis


Local thermodynamic equilibrium (LTE) is a good approximation for the H2CO level populations under optically thin and high-density conditions


For comparison, we show in Fig. 13 the predictions of the most recent one


where the updated nuclear reaction network was used.


This is consistent with the ${\approx } 30\, {{\rm per\, cent}}$ amplitude modulations observed in the source at 3 GHz


being caused by refractive interstellar scintillation in the Milky Way interstellar medium


The previously reported anti-correlation between tdepl and sSFR


is also further supported by our galaxies at z = 4.4 − 5.9 (Fig. 6, middle panel).


Our numerical experiments, however, do not seem to support claims of the steepening of the R ∝ Mα relation for CGs towards values α ≳ 1


Our results appear to stand apart from similar studies in full spherical shells (e.g.,


in that the differential rotation is strongly quenched as a function of the magnetic Reynolds number.


We calculate this by using the slug stellar population synthesis code


We use the $\mathcal {N}_\mathrm{LyC}$ for each H ii region as determined from the radio observations outlined in Table  2 (i.e.


and solve for the direct radiation pressure using equation (4).


However, uncertainties on the observational and theoretical sides mean that the true level of disagreement is unclear. For example, while


derived a PN abundance of 10−8 relative to H2 in IK Tau, De Beck et al. (2013) and Velilla Prieto et al. (2017) derived higher abundances, (3–7) × 10−7, in this source.


Then, we consider the REFLKERR where the hard X-ray Comptonisation spectrum is computed with the COMPPS model


which appears to be a better description of thermal Comptonisation when compared to Monte Carlo simulations


We derive a ratio ∼0.05, which is very similar to the average ratio derived in the disc of M 31 (see e.g.


and to determine the redshift of galaxies


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


The left-hand panel of Fig. 2 shows sources from Gaia’s DR2 LPV catalogue


chosen to lie within a 15° aperture of the LMC.


Recent results from solar flares observed from space


demonstrate an NUV spectrum originating largely from Hydrogen Balmer continuum emission.


However, it has been shown that these events can be explained using physics beyond the standard model, as many models suggest that AAEs lend support for axionic dark matter, sterile neutrinos, supersymmetry, or heavy dark matter


Note that the minimum value of the drag parameters we used here is 1 × 10−9 km s−1, which was revealed as the lowest possible value


Nevertheless, an early ROSAT observation of the old open cluster M 67, which lies at ∼840 pc


Earlier observations of the physical sizes of SMGs by CO detection and 1.4 GHz imaging suggest larger sizes (e.g.


These low ratios are consistent with the values found for several other stars with strong chromospheric activity


For instance, shallow gradient in metallicity is seen in SBS 0335−052 (


while no significant variations were seen in Mrk 35


However, our result is consistent with other NLFFF results


In late-type AGN-host galaxies, the gas kinematics appears complex at all scales, showing several components such as bars, rings, and (warped) discs, with high velocity dispersion regions (e.g.


Although the current corotation radius is rco ≈ 2.25 RJ, Jupiter at its time of formation was much larger than it is today


and this means that the corotation radius was also larger than the current one if the conservation of the angular momentum of Jupiter is assumed. Considering the transport of the angular momentum from Jupiter to the disk, the angular momentum should have been conserved since the disk disappeared.


TDSs are also expected along the Parker Solar Probe orbit


The consideration of ambipolar diffusion processes in solar physics started many decades ago


but it has undergone a true explosion in terms of its use in large numerical models (e.g.


Such numerical calculations often encounter a problem: given the comparatively high values of χa in different cosmic environments, the advance in time may grind to a halt in magnetised regions when a standard Courant-Friedrichs-Lewy condition is adopted for the timestep based on ηa.


For this reason, we obtained a considerable amount of biases (150−300 frames) and twilight flat-fields (25−100 frames) each night to reduce the Poisson noise to less than 0.2 mmag


However, as rapidly rotating stars evolve off the main sequence they slow down considerably and become much cooler making it relatively easy to search for planets around them. This fact was exploited by dedicated planet searches around intermediate mass sub-giants leading to dozens of planet discoveries


Most studies to date find that cusp-core transformations are challenging at the likely mass-scale of UFDs (M200c ∼ 109 M⊙; M* ∼ 105 M⊙; e.g.


However, different works used different mono-energetic bins to represent this channel, e.g.,


This is probably ram pressure caused by the relative motion of galaxies with respect to the ICM


The influence of tidal truncation is therefore limited to stellar multiples, either in bound systems


The fitted radio spectral index α1 from this study is −0.53 ± 0.04, consistent with broad-band spectral indices determined using radio, optical, and X-ray data at various epochs, where the typical value is approximately −0.58 (e.g.


Along with an increasing number of observational cases, the study of fast kink oscillations in coronal loops has been significantly advanced


see Figure 8 for a comparison of the arc redshift distributions adopted by the pre-HFF and new HFF+ lensing models;


We also used some observational data obtained within several other programmes


It has only recently become widespread to model the formation of galaxies ab initio (e.g.


Currently, a limited number of observations


are available to explore the environment dependence of the metallicity, and most of our current understandings are based on simulations


Several solutions have been successfully proposed in order to deal with stellar oscillations and granulation phenomena, such as:


using daytime spectra of the Sun in order to measure the solar oscillations (e.g.,


This picture is consistent with the observed low temperature, large radius, and super-Eddington luminosity (see


However, there are two notable discrepancies between the HST observations and the xstar model predictions. The first is that the $[{\rm O\, \small{III}}]\, {\lambda }$5008 emission line is observed to be 230 per cent brighter than predicted by xstar. This excess emission could be attributed to the extended source of $[{\rm O\, \small{III}}]\, {\lambda}$5008 seen in the nucleus of NGC 3327


Volonteri et al. (2015b) suggest that in the merger phase, the AGN dominates the bolometric luminosity but the accretion can be very stochastic (see also


This image reconstruction problem inspired several computational approaches like


Interstellar scintillation (ISS) is difficult to distinguish from intrinsic variability without fully time-resolved data (see e.g.


and references therein), and can coexist with it


However, to obtain precise photometric transit and spot parameters, we recommend the use of a planetary pixel radius between 15 and 50 pixels


at the same locations, we obtain the metadata for each observation, including the magnitude limit mlim of the observation, the seeing of the observation, and the standard deviation σpix on the background at the pixel on which the SN is located.


A large number of kinematic arches with various morphologies not known prior to Gaia were found


In parallel, theoretical works and simulations have tried to explain the physical mechanisms that reproduce the measured global properties


In Equation (3), ΔE denotes the width of the respective energy bin; for the typical radial velocity of solar wind in the flanks and the downwind hemisphere of the inner heliosheath, we assumed uR = 140 km s−1 as measured by Voyager 2, whereas uR = 40 km s−1 for the heliosheath in the Voyager 1 direction


Solar wind velocity distribution moments are described in


The constant, 4.64, is the r-band magnitude of the Sun in the AB system


Assuming the width of the gaps corresponds to 4RHill


On the contrary, ground-based telescopes usually have instruments which can cover several spectral lines simultaneously, e.g.


One of the major error sources is the uncertainty in ξ in various studies, including ours, based on spectra at different wavelengths


Recently, Papaloizou (2015) proposed a semi-analytical model of three-planet resonances taking into account only the interactions between consecutive planets in the chain, with a particular focus on the Kepler-60 system (12:15:20 resonant chain, see also


For the purpose of this study, we equipped the code with an on-the-fly non-equilibrium chemical network, which was implemented via the public chemistry library KROME


Since the rotation period of the secondary star should not change (and the effect of differential rotation for star spots at different latitudes is small for M dwarfs


we conclude that the star-spot signal cannot be originating on the secondary component.


The broad-band spectral energy distribution (SED) of blazars is characterized by a two-hump structure, one peaking at low energies in the optical/IR/X-ray region and the other one peaking at high energies in the X-ray/MeV region


One possibility to solve this issue is that the potential Psyche asteroid family was created at an early time, e.g. within the first 500 Myr of Solar system history


This would allow the family fragments to be ground down by collisional evolution and be unobservable today. The same models show that, even in this case, today there should be several surviving fragments having diameters around 20 km and above the detection limit.


The first study to determine masses for a sample of metal-poor halo giants with both seismic information


and chemistry from high-resolution APOGEE


The authors used scaling relations at face value and reported masses larger (M >  1 M⊙) than what would be expected for a typical old population.


Similar results were obtained by Casey et al. (2018), also using scaling relations for three metal-poor stars.


These findings led to the need for further tests of the use of asteroseismology in the low metallicity regime.


Theoretical stellar libraries like, e.g. BaSeL


are generally available for both a large range in wavelength and in stellar parameters, whereas empirical libraries are found to be more incomplete in both respects.


However, since such diagnostics usually involve the [N ii]/[O ii] or the [N ii]/[S ii] line ratios, they are strongly dependent on the assumed relation between the N/O ratio as a function of the oxygen abundance O/H, which is affected by a large scatter and whose evolution with cosmic time and/or dependence on galaxy mass is also indicated as a possible origin of the observed evolution of the emission-line properties in high-zgalaxies


This is illustrated in Fig. 5, where thick blue and red data points show mild high-energy excesses of the electron spectra derived by Kraus (2018),


, Kerszberg (2017) over broken power-law models derived from the fits to lower energy data.


NATs, which are especially common in clusters, (e.g.,


result from sustained relative motion between an RG and its ambient ICM; that is, the RG effectively evolves in a wind that deflects the RG jets and their discharge downwind.


The number of convincing dual AGN systems, mostly detected by X-ray and radio observations (e.g.,


are relatively few compared to the theoretically predicted abundance


Mass–radius relation is employed to estimate radius in case of white dwarfs and neutron stars (see e.g.


We convert the ASAS-SN distributions into estimates of the true luminosity function using the V/Vmax method


Subsequent studies found the same trend of [α/Fe] with mass


leading to the dominant interpretation that in more massive ETGs, the duration of star formation was substantially shorter than in less massive ones, with timescales short enough (e.g. 0.5 Gyr) to avoid the dilution of the α element abundance (produced by Type II supernovae) by the onset of Fe production by Type Ia supernovae. This is considered to be one of the main pieces of evidence for the shortening of star formation.


In this model, the dissipation of the kinetic energy of the equilibrium tide inside the star is often taken to be constant throughout the system evolution and calibrated on observations


The quasar survey data are also used for studies to constrain cosmological parameters


We make the simplifying assumption that the cloud temperature does not vary with radius; for solar composition, photoionization equilibrium is achieved at temperatures T ∼ 104 K across a wide range of ionization parameter (equation 5), and the gas temperature will therefore vary weakly with radius (e.g.


or parametric equations tuned by direct comparison with the outcome of numerical simulations of collisions of live galaxy pairs (e.g.


Regarding the radiation-hydrodynamic evolution, the conservation equation $\Delta_\alpha T^{\alpha \beta }_{\rm (total)}=0$ is solved using the piecewise parabolic method


Other sources of dark energy include scalar fields such as


Usually, the downstream sheath regions have larger density, temperature, mean magnetic intensity, and compressibility, and higher plasma β, as compared to the upstream solar wind


The large differences noted in Figure 9 are surely related to the different approximations underlying both the complex hydrodynamical simulations of ILLUSTRIS-1 and our simplified approach.


A key role is also played by the host cluster itself, because the mass profile of this latter becomes steeper and steeper in the core due to dynamical relaxation. Consequently, the environment gets denser with time; this trend is found to be quantifiable in terms of the number of dynamical times elapsed since the cluster formation (e.g.,


Therefore, each galaxy has to attain a sufficiently cold core in order to first survive in the cluster environment and then grow by accretion of matter from the ICM and mergers with other substructures.


was X-ray selected (and optically selected for the sample of Zhu et al. 2021), which may lead to the radio jet power being very feeble compared to the bolometric luminosity in most of the RLAGNs.


and black hole mass of the source are $\log (\dot{\mathscr {M}})$ = $2.63^{+0.16}_{-0.67}$ and log (MBH/M⊙) = $6.78^{+0.31}_{-0.06}$ with the reverberation mapping technique


respectively, where $\dot{\mathscr {M}}\equiv \dot{M}_{\bullet }c^2/L_{\rm Edd}$, $\dot{M}_{\bullet }$ is mass accretion rates, c is speed of light, and LEdd is the Eddington luminosity.


As this model is nonrotating and the proto-neutron star convection happens after the core bounce, the gravitational strain shows a loud bounce signal at time zero, and then it is followed by a low-frequency peak PNS oscillation, which could be caused by the g-mode oscillation although the nature remains controversial


Then, interestingly, it followed by the quadruple radiation of the standing accretion shock instability


signal, which was suggested to be seen in the GW data


With regards to the inclusion of extra information, a recent example in template methods includes using surface brightness as a prior in spectral energy distribution templates


, motivated by the knowledge of surface brightness dimming (1 + z)4.


In empirical methods this application is more straightforward, since algorithms are constructed such that it is not difficult to add extra input parameters.


The primary DEMs for this analysis is the quiet Sun (QS) and active region (AR) DEMs as needed for estimating the daily variations of the solar XUV spectral irradiance for the XPS Level 4 product


For βapp and δvar we used the fastest measured radial, non-accelerating apparent jet speed from the MOJAVE kinematic analysis


There have been rather strong claims of AGN QPOs in different bands of the electromagnetic spectrum, ranging from minutes through days through months and years (e.g.


Since CVs are intrinsically rather faint (typically, MV > 4 mag; e.g.


, in general the correction for the interstellar extinction will represent an upper limit.


In contrast, when the primary X-ray continuum is scattered close to the SMBH, Doppler and general relativistic effects combined may give rise to a significantly broader line (FWHM tens of thousands km s−1), reported in at least ∼36% of AGNs


Along the dust lane of the elliptical galaxy, there is a molecular gas component of mass ∼109 M⊙ as probed by various molecular lines


Note that the perpendicular heating rate is a nonnegligible fraction of that observed in the solar wind, where


If f > fm, the index of the power-law relation between A(f) and f changes


Entire sample is shown in Toomre Diagram of rotational velocity (VLSR) and sum of quadrature of radial and vertical velocities ([$\rm {\it U}_{\rm LSR}^2 + {\it W}_{\rm LSR}^2]^{1/2}$)


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


To this we can add that Zimbardo and coworkers reported in a series of papers that spacecraft observations of SEP intensity-time profiles ahead of interplanetary shocks yielded power laws instead of the exponential profiles predicted by standard DSA. They interpreted this as a sign of superdiffusive spatial SEP transport in the shock vicinity resulting in superdiffusive shock acceleration. They predicted the superdiffusive shock acceleration to be more efficient, producing a harder accelerated power-law spectrum for SEPs, than standard DSA


As the hot Fe xxi line is absent in the non-flaring spectrum, the rest wavelength for the Fe xxi line (i.e., 1354.09 Å) is determined by averaging the line centers of the Fe XXI profiles which were used in the previous IRIS observations


, while the rest wavelengths for the C i and Si iv lines, i.e., 1354.29 Å and 1402.77 Å, respectively, are determined from their quiet-Sun spectra


This layered-accretion scenario has been refined as additional non-thermal ionization sources (X-rays, UV radiation) and non-ideal magnetohydrodynamic (MHD) effects (ambipolar diffusion and the Hall effect) have been included (e.g.


The neon abundance can be compared and related to the results from stellar abundance analysis, as neon (and oxygen) originates from primary nucleosynthesis in massive stars (≥10 M⊙) and is therefore nearly independent of the evolution of LIMS, the progenitor stars of PNs


Assumption of the thermal blackbody radiation could overestimate the emissivity of ionizing photons at Z ∼ Z⊙ owing to the line-blanketing effect, especially for stars with M* ∼ 10 M⊙ (e.g.


These surveys offer unprecedented detection, astrometric, and spectrophotometric capabilities that allow us to characterize fainter and closer giant planets, such as the recent discovery of 51 Eri b (2 MJup at 14 au, T5-type, of an age of 20 Myr;


Such surveys also provide key spectral and orbital characterisation data for known exoplanets (e.g.,


were used as inputs for the turbulence quantities (e.g.,


Furthermore, mean free paths such as those discussed have,


Within these weak processes, although the modified Urca processes involving leptons are important, it has been shown that non-leptonic processes involving hyperons contribute more significantly towards bulk viscosity at temperatures lower than a few times 109 K


By pushing current observatories to their limit, recent studies derived constraints on the relative fraction of SN events that effectively contribute to the ICM enrichment. These measurements showed that SNIa and SNcc contribute relatively equally to the overall chemical enrichment in the ICM


Based on a literature review for papers where VLBI parallax measurements were determined using an in-beam calibrator, we find 24 similar measurements, the majority of which have been used to measure parallaxes to pulsars


the study of binary systems such as eccentric MSPs like PSRs J1903+0327


which are interesting due to their peculiar binary evolution


To confirm the importance of VO, water and an inversion layer


obtained repeated HST observations of the transmission spectrum and the secondary eclipse using the STIS and WFC 3 instruments.


The optical transmission spectrum displays rich variation, with multiple features consistent with VO absorption that Evans et al. (2018) could reproduce by assuming an isothermal T-P profile at 1500 K and a metallicity equivalent to 10× to 30× solar. Absorption bands of TiO appeared to be muted in the transmission spectrum, which was explained by Evans et al. (2018) as evidence of condensation of Ti-bearing species, which commences at higher temperatures than condensation of V-bearing species, producing for example, calcium titanates (Lodders 2002) while VO remains in the gas phase.


formation of globally unstable disks, and radial gas transport by dynamical friction


A tight relationship between O/H and N/O abundances is indeed observed in both H ii regions and local galaxies,


and it is set by the predominant nucleosynthetic origin of nitrogen from CNO burning of pre-existing stellar carbon and oxygen in low- and intermediate-mass stars experiencing the AGB phase (i.e. the ‘secondary’ nitrogen production mechanism,


For CC iron meteorites, we examine the isotopic compositions of Mo and Ni, respectively, because these are siderophile elements (so are therefore present in appreciable concentrations in iron meteorites, unlike Ti and Cr) whose compositions have also been relatively well studied in a number of iron meteorites as well as chondrites and their components


We predict the noise in the Planck lensing map assuming the detector sensitivity and beam sizes listed in the Planck Bluebook


The FNm can be written explicitly as an integral over the eccentric anomaly


F_{Nm} = \frac{1}{\pi }\int \limits _{0}^{\pi } \frac{\cos \left[N\left(E - e\sin E\right) - mf(E)\right]}{\left(1 - e\cos E\right)^2}\,\,\mathrm{d}E.


The second issue is the pseudo- versus classical bulge argument – the model we use assumes an inner classical spherical bulge; bulges instead may be pseudo-bulges, which may not have a spherical shape, and profile well-described by a spherical Hernquist profile


In fact, it is commonly believed that dynamical interactions in GCs facilitate the formation of close binary systems and exotic objects such as cataclysmic variables (CVs), low-mass X-ray binaries (LMXBs), millisecond pulsars (MSPs), and blue straggler stars (BSSs) (e.g.,


The luminosity during the 2020 giant outburst reached a record high, which was significantly higher than the critical luminosity


Lastly, the results from this approach critically depend on the choice of low-b cutoff fitting techniques, where different techniques might result in inconsistent T0 and γ measurements


Cepheids have also been found to show additional complications that include cycle-to-cycle variations in their light and radial velocity curves (see


It is of importance to planned future surveys to investigate suitable strategies for source-finding in linear polarization with interferometers such as LOFAR,


and with the ability to make precise Faraday rotation measurements


Specifically, we use m* values computed from Bruzual & Charlot (2003) models in the same fashion as described in previous SPT publications


The warm Neptune GJ436b, which is the lowest mass planet found evaporating to date


), shows transit absorption depths up to 60% in the Ly-α line.


Semi-analytic modelling is a particular simulation method which is optimized to connect the observed properties of the galaxy population – abundances, scaling relations, clustering and their evolution with redshift – to the astrophysical processes that drive the formation and evolution of individual galaxies (e.g.


Minima and transition states (TSs) were optimized using the DL-FIND


Over the last few decades, the PTA collaborations have not found GW signals, but the increasingly sensitive data sets offer increasingly stringent constraints on the SGWB


which suggests that at least some FRBs originate from magnetars born from the core collapse of massive stars (e.g.,


Approaches of this type are widely used in astronomy, for example to infer star formation histories or stellar mass distributions from observed colour–magnitude diagrams (CMDs; e.g.


Infalling and rotational motions on scales from 100 to 3000 au have been observed in molecular lines with single-dish telescopes and interferometers


This must typically be done with a numerical Poisson solver


discussed four estimators which attempted to correct for biasing in the degree of linear polarisation in the presence of low signal-to-noise ratios.


Note that the majority of the studies related to the MIR bubbles are mainly carried out for a single H ii region or several H ii regions on scales of a few parsecs (e.g.,


have isotropic ∼5 GHz luminosities of between 1040 and 1042 erg s−1 whereas the rest


have luminosities in the range 1037 to 1039 erg s−1 at similar frequencies. The higher power events are believed to result from observing down the axis of a relativistic jet, resulting in the energy of photons being significantly boosted. Even accounting for boosting, these relativistic events have a higher total energy output than their thermal counterparts.


are also overplotted. The three parallel lines are the reddening vectors drawn from the tip of the giant branch (left), from the base of the MS branch (middle)


Given this deficit, we provide only a simplified estimate using radial velocities of OBA-type stars from


Since they belong to the same young population, we assume that they have a similar distance distribution and kinematics as the Cepheids.


The mainstream grains have 12C/13C ratios between 10 and 100 (solar: 89), and the 14N/15N ratios of most of them are higher than the solar ratio of 440, the ratio measured for the solar wind


We recall that this relation is valid only under the assumption that the mean star formation activity of the emitting galaxies is constant on a timescale of a few Myr, roughly comparable to the typical time spent by the stellar population responsible for the ionisation of the gas on the main sequence


Velocity fluctuations have been studied thoroughly (see, e.g.,


although the kinetic scales still remain quite unexplored for instrumental limitations, most notably in the sampling time resolution.


Detection of rebrightening during the outburst decay supports the argument that the formation of a compact jet and its interaction with the accretion environment are imprinted on the multiwavelength behaviour of the GBHTs


The relevant methodology is straightforward and well established. One needs to calculate the likelihood function of the data given the model – namely the probability of the occurrence of the data within the framework of the assumed model


However, an optimal metric – expressed as an entropy functional – is not known in advance and therefore needs to be chosen individually


It was found that if we assume a single H desorption energy in models, the dust temperature range over which efficient H2 formation occurs is narrow (6–10 K for olivine grains)


scenario, the MRI and subsequent turbulence in the inner accretion disk are suppressed due to large-scale magnetic flux (see, e.g.,


have indicated that dissipation, acceleration, and thermalization of turbulent plasmas mainly take place near intermittent structures on kinetic scale, while the actual physical mechanisms behind dissipation remain unclear.


A small number (currently six) of confirmed TDEs, including ASASSN-14li, have also been detected at radio wavelengths and the population may form a bi-modal distribution, consisting of more common non-relativistic ‘thermal’ events and rarer relativistic jets. Three events (Swift J1644+57


have isotropic ∼5 GHz luminosities of between 1040 and 1042 erg s−1


The higher power events are believed to result from observing down the axis of a relativistic jet, resulting in the energy of photons being significantly boosted.


On the other hand, long-duration gamma-ray bursts (lGRBs


are associated with the core collapse (CC) of dying massive stars


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


stimulate a renewed investigation on density statistics


have shown that the higher J lines of CO arise from warmer, denser gas than the cold gas responsible for the emission of for example CO J = 1−0.


generally lead to mixed results. This encourages to keep investigating it, as it indicates that the origin of the radio emission in RQ AGN is still an open question.


The estimated continuum slope is consistent but somewhat flatter than the typical slope of luminous quasars


The upper atmospheres (above optically thick clouds) of giant exoplanets and those of smaller planets around M stars can be probed using spectroscopy during primary and/or secondary transits


and other large-scale surveys, as well as analyses that combine kinematic data with information about chemical abundances and/or specific stellar populations, have led to discoveries of additional substructures in the Galaxy and brought renewed attention to this topic (e.g.,


The full particle simulations are performed using


both of which solve Maxwell equations and push particles using relativistic approaches. The VPIC code directly evolves electric and magnetic fields, whereas in the NPIC code the fields are advanced using the scalar and vector potentials.


Although the two codes have very different algorithms, all of the key results are in good agreement for this study, thus providing additional confidence in our conclusions.


Dynamic ocean heat transport on completely ocean-covered worlds (i.e., no continents) leads to warmer global mean temperatures and a reduction in day–night temperature differences on synchronously rotating planets


In future works, our group plans to couple our GCM with a dynamic ocean model to study the interactions between oceans, continents, topography, and observable features.


In the outer regions of a Shakura-Sunyaev disk, the opacity is expected to be mainly due to free-free absorption, while Thomson scattering dominates the opacity in the inner regions of the disk (see Eqs. (2.16) and (2.19) of


The geometrical thickness of the disk scales with the radius R following a (slightly) different relation; it is proportional to R−21/20 in the inner Thomson scattering-dominated, regions and to R−9/8 in the outer regions. At the boundary between these two zones (i.e., at a radius Rjump) a jump is expected. We calculated Rjump according to our results for Ṁin and assuming the same value for α in both equations. We found Rjump between 3 × 104 RG and 7 × 104 RG in all the epochs considered.


Consequently, many libraries of limb-darkening coefficients covering a wide range of effective temperatures (Teff), surface gravity (log g), and metal-licities (M/H) have been produced


using various radiative transfer codes, such as


In fact, Sanders (1998) points out that, too close to the MBH, molecular clouds should get disrupted by its gravitational field preventing star formation; even if the Milky Way nucleus features a population of young stars very close to the MBH


supporting instead the idea of possible central star formation, it seems unlikely it can develop such steep profiles.


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


with the disk gradually building up around them.


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


In transition regions from diffuse ISM to dense clouds