adsabs/AstroCLIMB huggingface dataset:
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: Fourteen NS-HMXBs on a mass-ratio against orbital-period diagram. Symbols mark different types of NS-HMXBs. Violet NS-HMXBs have measured radii, while gray do not. The blue and violet regions are theoretically permitted spaces for stable RLOF from the normal and naked helium donors. Above the fitted maximum mass-ratio envelope (blue for metal-poor Z = 0.001 massive donors and violet for Z = 0.02 helium donor stars), systems must be undergoing wind mass transfer, have a highly eccentric orbit, and be suffering delayed dynamical instability.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: The top panel displays the probability distribution of neighbor counts around AGNs at varying redshifts normalized to integrate to unity. Lighter colors represent higher redshifts, and darker colors indicate lower redshifts. The bottom panel shows the logarithm of the number of neighbors as a function of the host AGN halo M 200, with each line representing the median of neighbors counts at each mass bin. This demonstrates a near-linear relationship between halo mass and neighbor counts, with higher-mass halos having more neighboring SMBHs.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: AGN number density, AGN counts, and total number of neighboring SMBHs across redshifts. The first panel illustrates the number density of AGNs detected at redshifts under consideration. The middle and right panel presents the absolute number of AGNs and the total number of SMBH neighbors within a 30 pkpc radius of the AGNs, respectively.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: Relationship between halo mass and distance of neighboring SMBHs from their corresponding AGN across redshifts. Each line represents the median distance at a specific redshift. The increasing trend illustrates that higher halo masses correlate with a greater spread of neighboring SMBHs.
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: The eccentricities of HMXBs on a mass-ratio against the orbital-period diagram. The symbols again show the HMXB types.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: Bolometric luminosity as a function of SMBH mass for AGNs and their neighboring SMBH at three different redshifts (z = 0.05, 1, and 2). AGNs are represented by orange circles, while the neighboring SMBHs are depicted as teal triangles. The dashed line indicates the luminosity cut for defining AGNs.
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: The ratio of donor radius R to Roche-lobe radius R L of 82 HMXBs in Table 1 on a mass-ratio against the orbital-period diagram. Symbols represent the types of HMXBs in the Table. Colors (gray means unknown) show the ratio of donor radius to its Roche-lobe radius.
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: Left: the gray histogram shows ratios of a 0/a  f , which we calculate for the 128 planets that already meet the ∣g∣/α < 1 condition in the present day. Lines are color-coded by the tidal stability condition calculated in Section 3.4, with gray corresponding to planets that do not meet the condition, teal corresponding to planets that meet the condition if mutual inclination I = 5.5°, and dark teal corresponding to planets that meet the condition if mutual inclination I = 2.5°. Right: for the same sample of planets, we depict the relationship between η and a 0/a  f , with the same color coding. The vertical gray dashed line shows a 0/a  f  = 2. We conclude that planets likelier to be stable in CS2 require only modest amounts of migration.
Paper: The Molecular Cloud Life Cycle. II. Formation and Destruction of Molecular Clouds Diagnosed via H2 Fluorescent Emission
Authors: Blakesley Burkhart, Shmuel Bialy, Daniel Seifried, Stefanie Walch, Erika Hamden, Thomas J. Haworth, Keri Hoadley, Shuo Kong, Madisen Johnson, Sarah Jeffreson, Mark R. Krumholz, Min-Young Lee, Amiel Sternberg, Neal J. Turner
Figure caption: Cloud evolution for MC1, comparing ratios of H2 formation to SFR vs. H2 dissociation to SFR. Points are from the numerical simulation, and color indicates time as shown in the color bar inset in Figure 4. We overplot regions of parameter space in which different cloud evolutionary states exist, as discussed in Section 4. The state of the cloud, as it proceeds through formation, gas steady-state cycling, and cloud dispersal, can be determined by the ensemble of these rates.
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: Calculated obliquity ranges for each planet, as a function of orbital semimajor axis. The obliquity range is calculated using only the ∣g∣ values for interactions of adjacent pairs of planets (e.g., TRAPPIST-1c with TRAPPIST-1b or with TRAPPIST-1d) and the median obliquity for each range is plotted as a point on the range line. The planets with no possible obliquity for a given value of ∣g∣ are plotted as a dashed line. The value for Earth’s obliquity is also shown as a reference. There is a wide range of obliquity values possible for planets 0.01–0.4 au from their host star. Beyond roughly 0.4 au, nonzero obliquity due to capture in CS2 is no longer excited.
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: Ratio of characteristic tidal timescale to critical tidal timescale, t s/t s,c (for t s,c at I = 2.°5), plotted against the ratio η = ∣g∣/α for each planet we consider. The histogram of the η values shows η is most commonly between values of 0.01 and 1, where the points have the densest overlap. Above the horizontal gray dashed line, planets are tidally stable, with t s/t s,c. To the left of the vertical gray dashed line, η < 1. We can identify points in the upper left “quadrant” made by these intersecting dashed lines as the 36 that satisfy both conditions for tidal stability and high obliquity.
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: Roughly half of the values of α and g for our planet sample overlap with a peak value roughly corresponding to a period of ∼1000 yr. For each planet in the sample, we calculate α, the spin-axis precession constant, and g, the nodal precession frequency. All values for g are shown in the histogram. Note the commensurability of the two distributions, making Cassini State capture plausible.
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: Left: characteristic tidal timescale t s for all planets in the sample, plotted against the ratio η = ∣g∣/α. We require η < 1 for excitation to a nonzero obliquity (see Equation (5)). We find that this condition is met more often for planets with shorter characteristic tidal timescales. Right: critical tidal timescale, t s,c, for all planets in the sample, similarly vs. η (shown for two assumptions for mutual inclination I: 2.°5 and 5.°5). The opposite trend holds for planets that satisfy the η < 1 condition; they tend to have longer critical timescales.
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: Oblique planets in CS2 rotate subsynchronously. The horizontal axis plots our predicted values for obliquity. The vertical axis shows the ω eq/n values calculated using Equation (6).
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: The length of a “solar day” lasts longer than an orbital year for planets captured into CS2. The horizontal axis shows the orbital period for the sample and the vertical axis shows the computed T solar. The gray dashed line corresponds to T solar = P, or permanent day and permanent night for a tidally locked planet. Earth, shown for reference, has a T solar much smaller than its orbital period.
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: The four innermost planets in the TRAPPIST-1 system are amenable to capture into a nonzero-obliquity state. We note that TRAPPIST-1d and TRAPPIST-1e (the green and red points, respectively) are in the habitable zone for the planet, which ranges from roughly 0.02 to 0.04 au.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: Evolution of dual AGNs that do not merge. The figure shows the evolutionary properties of a dual AGN system from the time that they were in two distinct halos until z = 0. The colors and properties of each panel are the same as Figure 12.
Paper: The Extremely Metal-rich Knot of Stars at the Heart of the Galaxy
Authors: Hans-Walter Rix, Vedant Chandra, Gail Zasowski, Annalisa Pillepich, Sergey Khoperskov, Sofia Feltzing, Rosemary F. G. Wyse, Neige Frankel, Danny Horta, Juna Kollmeier, Keivan Stassun, Melissa K. Ness, Jonathan C. Bird, David Nidever, José G. Fernández-Trincado, João A. S. Amarante, Chervin F. P. Laporte, Jianhui Lian
Figure caption: Radial extent of different mono-abundance stellar populations for Milky Way analogs from the TNG50 simulation (A. Pillepich et al. 2024). The left panel shows the radius R GC that encloses 68% of a mono-abundance population as a function of [M/H] for a handful of example galaxies. This left panel shows that for (at least these) simulated galaxies the most metal-rich stars are very centrally concentrated, forming a knot of ≲1 kpc. This is in qualitative agreement with our analysis of the Milky Way (see Figure 3). However, in these simulated galaxies the central confinement encompasses stars within Δ[M/H] = 0.4 of the maximal metallicity, whereas in our Galaxy the stars in the knot are within 0.1 dex of the maximal metallicity. To eliminate issues revolving around metallicity systematics, we also consider which fraction of the stars’ MFD is part of this central knot. The right panel shows, for a much larger set of TNG50 Milky Way analogs, the (most metal-rich) fraction of the MDF that is confined to within R GC = 1.5 kpc: typically between 5% and 15% of all stars within 20 kpc; these fractions barely change if we calculated them for stars within 1.5 kpc but beyond 0.5 kpc, to simplistically mimic the effect of dust extinction very close to the Galactic center. By comparison, the face-value fraction of stars in the Milky Way’s knot (i.e., in the Gaia XP sample as defined in Section 2) is dramatically lower, only 0.1% (Figure 3). However, this observed fraction constitutes a lower limit, as the most centrally concentrated populations in the Milky Way are inevitably most extincted, and hence most underrepresented in the Gaia XP sample.
Paper: Migration of Accreting Planets and Black Holes in Disks
Authors: JT Laune, Rixin Li, 日新 李, Dong Lai
Figure caption: The top two panels are the same as Figure 4, but for Runs Ia (left) and Ib (right) (with sink radii different from Run I, r  s  = 0.05r  H  and r  s  = 0.2r  H , respectively). The ﹩\dot{J}﹩ profiles before and after iteration are plotted in the bottom panels.
Paper: The Extremely Metal-rich Knot of Stars at the Heart of the Galaxy
Authors: Hans-Walter Rix, Vedant Chandra, Gail Zasowski, Annalisa Pillepich, Sergey Khoperskov, Sofia Feltzing, Rosemary F. G. Wyse, Neige Frankel, Danny Horta, Juna Kollmeier, Keivan Stassun, Melissa K. Ness, Jonathan C. Bird, David Nidever, José G. Fernández-Trincado, João A. S. Amarante, Chervin F. P. Laporte, Jianhui Lian
Figure caption: Age distribution of different mono-abundance stellar populations for a handful of Milky Way analogs selected from the TNG50 simulation (A. Pillepich et al. 2024). Specifically, we show the 16th and 84th percentiles of the stellar ages as a function of [M/H]. According to TNG50, the stars in the metal-rich knot have a wide range of ages, 2 Gyr ≲ τ ≲ 10 Gyr, just as indicated by the data for the Milky Way (Figure 6 and T. Bensby et al. 2017).
Paper: Migration of Accreting Planets and Black Holes in Disks
Authors: JT Laune, Rixin Li, 日新 李, Dong Lai
Figure caption: Left: the global disk surface density for the nonaccreting Run In (top) and the accreting Run I (bottom; see Table 1). The green “+” indicates the planet location. Middle: zoomed-in plots of the surface density in polar coordinates with stream plots indicating gas velocity. Right: same as the middle column, but zoomed closer to the planet.
Paper: Migration of Accreting Planets and Black Holes in Disks
Authors: JT Laune, Rixin Li, 日新 李, Dong Lai
Figure caption: The components of AM flux through the disk for Run In. The dashed–dotted line is the advected AM flux, ﹩{\dot{J}}_{\mathrm{adv}}﹩ (Equation (4)). The dashed line is the viscous AM flux, ﹩-{\dot{J}}_{\mathrm{vis}}﹩ (Equation (5)). The dotted line is the torque density exerted by the planet’s gravity, − ﹩{T}_{{\rm{g}}}^{\gt r}﹩ (Equation (7)). The solid line is the total AM flux, ﹩\dot{J}﹩ (Equation (8)).
Paper: Migration of Accreting Planets and Black Holes in Disks
Authors: JT Laune, Rixin Li, 日新 李, Dong Lai
Figure caption: Same as Figure 2, but for an accreting planet in Run I. The magenta lines indicate the profiles from the iterated simulation (see Section 2.4); the dashed cyan lines indicate the profiles before iteration.
Paper: Migration of Accreting Planets and Black Holes in Disks
Authors: JT Laune, Rixin Li, 日新 李, Dong Lai
Figure caption: Disk profiles for the nonaccreting Run In. Top: the azimuthally averaged surface density profile, Σ(r). Bottom: the mass flux through the disk, ﹩\dot{M}(r)﹩ (Equation (3)).
Paper: Migration of Accreting Planets and Black Holes in Disks
Authors: JT Laune, Rixin Li, 日新 李, Dong Lai
Figure caption: Same as Figure 3, but for an accreting planet in Run I. The magenta lines indicate the profiles from the iterated simulation. The dashed cyan line indicates the ﹩\dot{J}﹩ profile before iteration.
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: The CDF for the probability of evolution into tidal Cassini equilibrium 2 (P tCE2). Note that P tCE2 can exceed 1, at which point capture into CS2 is guaranteed (that is, the CDF jumps vertically to a value of 1.0 at P tCE2 = 1.0). The CDF is ∼20% or higher for tidally stable planets in our sample. We calculate P tCE2 for the top and bottom of our mutual inclination range, I = 2.°5 and 5.°5, using an approximate analytical formula, Equation (14) from Y. Su & D. Lai (2022a) where η sync ≈ ∣g∣/α; and Ωs,i is the planet spin frequency at the start of migration, which we assume to be 10n, where n is the mean motion, 2π/P. The dashed CDF curves are the P tCE2 values for all planets in the sample. The solid CDF curves are P tCE2 for tidally stable systems, those where t s ≥ t s,c. The horizontal gray dashed line is to guide the eye for P tCE2 values at the 50% mark of each CDF. Values of P tCE2 can exceed 1, meaning the planet is guaranteed to be captured into tCE2.
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: Critical initial mass ratios q ad as functions of stellar radius for 20 M ⊙ models. The solid and dashed lines correspond to Z = 0.001 and Z = 0.02 stellar models. Red and blue lines correspond to models with standard mixing-length envelopes q ad and artificially isentropic convective envelopes ﹩{\tilde{q}}_{\mathrm{ad}}﹩ for fully nonconservative mass transfer. Gray lines show stellar models with standard envelopes q ad for fully conservative mass transfer.
Paper: Plausibility of Capture into High-obliquity States for Exoplanets in the M Dwarf Habitable Zone
Authors: Natalia M. Guerrero, Sarah A. Ballard, Yubo Su
Figure caption: We predict that temperate planets are highly likely to be captured in a spin–orbit resonance that is amenable to exciting high obliquity. Further, we note that these temperate, oblique planets are primarily hosted by cool stars (median T eff = 3720 K). The horizontal axis plots the equilibrium temperature, T eq in Kelvin and the vertical axis plots α/∣g∣. Recall that values of α/∣g∣ > 1 permit obliquity excitation. The thin gray horizontal lines mark obliquity values corresponding to selected values of α/∣g∣. Note 23°, Earth’s obliquity, is shown. The color map corresponds to Teff, the stellar effective temperature in Kelvin. The dashed gray horizontal and vertical lines bound the region of T eq = 200–400 K and α/∣g∣ > 1.
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: The left-hand panel shows the evolution for 20 M ⊙ stars with different metallicities in the Hertzsprung–Russell diagram. The right-hand panel presents their helium core masses M He, where core hydrogen mass fraction first reaches 0.15, as a function of their radii. Solid and dashed lines are stars with metallicities of Z = 0.001 and Z = 0.02.
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: Example critical mass ratios q ad for conservative and nonconservative mass transfer. The initial parameters are labeled. The black solid line marks the radius response during the adiabatic mass-loss process. The blue dashed line is the inner radius R KH. The dashed–dotted lines are the Roche-lobe radii under conservative (black), semiconservative (violet), and fully nonconservative (cyan) mass transfer.
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: Critical mass ratios q ad as functions of stellar radius for metal-poor massive stars. The masses in units of M ⊙ are labeled for each track. The solid (black) and dotted (blue) lines correspond to models of fully conservative and nonconservative mass transfer.
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: The evolution of metal-poor (Z = 0.001) stars. Black solid lines indicate massive donor stars, while gray dotted lines are low- and intermediate-mass stars. Some of the intermediate and low-mass stars were studied by H. Ge et al. (2023). We also extend the donor spaces in this study. Open circles are placed at ﹩{\rm{\Delta }}{\mathrm{log}}_{10}R=0.1﹩ from the ZAMS.
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: The impact of metallicity on helium core mass M He (left-hand panel) and the radius R (right-hand panel) as functions of a 20 M ⊙ star’s age. Solid and dashed lines are Z = 0.001 and Z = 0.02 stars.
Paper: Adiabatic Mass Loss in Binary Stars. V. Effects of Metallicity and Nonconservative Mass Transfer—Application in High Mass X-Ray Binaries
Authors: Hongwei Ge, Christopher A. Tout, Xuefei Chen, Song Wang, Jianping Xiong, Lifu Zhang, Zhenwei Li, Qingzhong Liu, Zhanwen Han
Figure caption: Critical mass ratios q ad as functions of stellar radius for 5 M ⊙ stars. The solid (black) and dotted (blue) lines correspond to models of fully conservative and nonconservative mass transfer.
Paper: Dual Active Galactic Nuclei: Precursors of Binary Supermassive Black Hole Formation and Mergers
Authors: Vida Saeedzadeh, Arif Babul, Suvodip Mukherjee, Michael Tremmel, Thomas R. Quinn, Lucio Mayer
Figure caption: The relationship between the bolometric luminosity and mass of SMBHs in single and dual AGN systems. Single AGNs are represented by gray dots, primary AGNs in dual systems by orange dots, and secondary AGNs by blue dots. The top panel shows the normalized distribution of SMBH mass for the different populations, while the right panel displays the normalized distribution of bolometric luminosity. Dashed lines showing the medians.