adsabs/AstroCLIMB huggingface dataset:
Paper: Formation of Magnetically Truncated Accretion Disks in 3D Radiation-transport Two-temperature GRMHD Simulations
Authors: M. T. P. Liska, G. Musoke, A. Tchekhovskoy, O. Porth, A. M. Beloborodov
Figure caption: The first demonstration of highly efficient energy extraction from a rapidly spinning black hole by a radiatively efficient accretion flow in a radiation GRMHD simulation. From top to bottom, the panels show the accretion rate in Eddington units, normalized magnetic flux on black hole, and outflow efficiencies (total in blue, jet in black, wind in cyan, and radiative in purple; see the legend) for the radiative stage of the simulations. Both RADPOL and RADTOR accrete at ﹩\dot{M}/{\dot{M}}_{\mathrm{Edd}}\sim 0.35﹩. The red lines demarcate the time intervals when we use either photon-conserving Comptonization (t ∈ [191, 840,  193, 650]r  g /c) or a higher-density floor (t ∈ [193, 650, 196, 550]r  g /c). While RADPOL floods the black hole with the large-scale poloidal magnetic flux and reaches the MAD state, RADTOR does not develop any net large-scale poloidal magnetic flux. In RADPOL, the total efficiency exceeds η tot ∼ 90%, for the first time demonstrating highly efficient energy extraction from a radiatively efficient accretion flow out of a spinning black hole in a radiation GRMHD simulation. The efficiencies of the jet and winds reach respectively η jet ∼ 50% and η wind ∼ 15%. In contrast, in the RADTOR simulation, the total efficiency is much smaller, η tot ∼ 40%, with a much smaller η jet ≲ 1%, and approximately the same η wind ∼ 20%. Both models achieve similar radiative outflow efficiencies, η rad ∼ 20%.
Paper: Formation of Magnetically Truncated Accretion Disks in 3D Radiation-transport Two-temperature GRMHD Simulations
Authors: M. T. P. Liska, G. Musoke, A. Tchekhovskoy, O. Porth, A. M. Beloborodov
Figure caption: Low-density, magnetically dominated, rapidly accreting, thicker corona-like accretion flow develops near the black hole only in the presence of large-scale poloidal magnetic flux. From top to bottom, the panels show the density-averaged midplane density ﹩\bar{\rho }=\int {\rho }^{2}{dV}/\int \rho {dV}﹩ (panels (a) and (b)); the ratios of density-averaged pressures, ﹩\bar{p}=\int \rho {pdV}/\int \rho {dV}﹩ (panels (c) and (d)); effective α-viscosity (panels (e) and (f); dashed lines indicate negative values); and scale heights (panels (g) and (h)) time-averaged over the radiative evolution stage of the simulations. The left panels show RADPOL and the right panels the RADTOR results. The vertical magenta lines show the location of the ISCO. While in both models the outer disk (r ≳ 20r  g ) is radiation pressure dominated, the inner disk in RADPOL becomes magnetic pressure dominated and forms a two-temperature plasma (with ﹩{\bar{p}}_{e}\ll {\bar{p}}_{i}﹩). This transition to a magnetic-pressure-supported corona in RADPOL is accompanied by a sharp drop in density and an increase in the effective scale height. The presence of a large-scale poloidal magnetic flux leads to rapid accretion in RADPOL as evidenced by the extremely high value of α eff.
Paper: Formation of Magnetically Truncated Accretion Disks in 3D Radiation-transport Two-temperature GRMHD Simulations
Authors: M. T. P. Liska, G. Musoke, A. Tchekhovskoy, O. Porth, A. M. Beloborodov
Figure caption: The absorption heating rate (λ abs, left column), emission cooling rate (λ em, middle column), and Compton cooling rate (λ sc, right column) for models RADPOL (top row) and RADTOR (bottom row). The right hemispheres show zoom-ins of the left hemisphere. Magnetic field lines are shown in black, jet boundary in white (p mag = ρ c 2), and the last scattering surface in pink (τ es = 1, integrated in the vertical direction). For clarity, we have removed data from the jet, whose thermodynamics cannot be modeled in GRMHD as explained in Section 4. Cooling in the corona of RADPOL (r ≲ 25r  g ) is concentrated near the equatorial plane, where the plasma has electron temperatures of T  e  ≳ 5 × 108 K. Here, Compton cooling is expected to give rise to a hard nonthermal emission that dominates over thermal emission. Because the plasma is optically thick (and self-absorbed) in model RADTOR, a more detailed ray-tracing analysis will be necessary to calculate the hardness of the spectrum.
Paper: Formation of Magnetically Truncated Accretion Disks in 3D Radiation-transport Two-temperature GRMHD Simulations
Authors: M. T. P. Liska, G. Musoke, A. Tchekhovskoy, O. Porth, A. M. Beloborodov
Figure caption: Accretion rate ﹩\dot{M}﹩ (upper panels) and MRI quality factors Q  r,θ,ϕ  (lower panels) as a function of radius averaged over the final 1000r  g /c runtime of the respective simulation. Dashed lines show negative values. While RADPOL achieves inflow equilibrium within r ≲ 25r  g , RADTOR is thermally unstable and never achieves inflow equilibrium. The MRI quality factors give the number of cells per MRI wavelength. RADPOL is sufficiently resolved throughout the domain while RADTOR becomes underresolved (Q ≲ 10) within r ∼ 10r  g  as the disk undergoes runaway thermal collapse.
Paper: Formation of Magnetically Truncated Accretion Disks in 3D Radiation-transport Two-temperature GRMHD Simulations
Authors: M. T. P. Liska, G. Musoke, A. Tchekhovskoy, O. Porth, A. M. Beloborodov
Figure caption: A transverse slice through density in RADPOL and RADTOR. The right hemisphere is a zoom-in of the left hemisphere. Velocity streamlines are illustrated in black, and radiation streamlines are illustrated in red. In model RADPOL, both the radiation and gas flow out radially. In RADTOR, the gas velocity shows a chaotic structure, while the radiation escapes mostly vertical.
Paper: MIGHTEE-HI: Evolution of HI Scaling Relations of Star-forming Galaxies at z < 0.5 
Authors: Francesco Sinigaglia, Giulia Rodighiero, Ed Elson, Mattia Vaccari, Natasha Maddox, Bradley S. Frank, Matt J. Jarvis, Tom Oosterloo, Romeel Davé, Mara Salvato, Maarten Baes, Sabine Bellstedt, Laura Bisigello, Jordan D. Collier, Robin H. W. Cook, Luke J. M. Davies, Jacinta Delhaize, Simon P. Driver, Caroline Foster, Sushma Kurapati, Claudia del P. Lagos, Christopher Lidman, Pavel E. Mancera Piña, Martin J. Meyer, K. Moses Mogotsi, Hengxing Pan, Anastasia A. Ponomareva, Isabella Prandoni, Sambatriniaina H. A. Rajohnson, Aaron S. G. Robotham, Mario G. Santos, Srikrishna Sekhar, Kristine Spekkens, Jessica E. Thorne, Jan M. van der Hulst, O. Ivy Wong
Figure caption: Left: ﹩{\mathrm{log}}_{10}({M}_{* })﹩ distribution of our spectroscopic galaxy sample (blue) and of the parent photometric sample (orange). Center: distribution of our sample (blue colormap histogram) on the ﹩{\mathrm{log}}_{10}(\mathrm{SFR})-{\mathrm{log}}_{10}({M}_{* })﹩ plane, with the main-sequence parameterization from Speagle et al. (2014), average trends from our sample, the parent photometric sample, and the SIMBA simulation overplotted as green solid, red dashed, orange dashed‒dotted, and black dotted lines, respectively. Red, orange, and green shaded regions indicate uncertainties on the curves of the same colors. Right: redshift distribution of our spectroscopic galaxy sample.
Paper: Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b 
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, Y. Aoyama, G.-D. Marleau, J. Bary, C. Robinson, M. Janson, W. Balmer, G. Chauvin, P. Palma-Bifani
Figure caption: Accretion rates for individual emission lines. Circles indicate data from Eriksson et al. (2020). Stars and diamonds represent our epochs 1 and 2, respectively. Accretion rates derived using both “stellar” empirical scaling relations (open symbols; Alcalá et al. 2017) and “planetary” accretion models (filled symbols; Aoyama et al. 2021) are shown. ﹩\dot{M}﹩(Hα) is also estimated using the line luminosity model of Thanathibodee et al. (2019, light gray). ﹩\dot{M}﹩ (Hα 10%) is estimated using a “stellar” empirical relation (dark gray; Natta et al. 2004).
Paper: Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b 
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, Y. Aoyama, G.-D. Marleau, J. Bary, C. Robinson, M. Janson, W. Balmer, G. Chauvin, P. Palma-Bifani
Figure caption: Predicted line ratios for local line excitation (“stellar”; Kwan & Fischer 2011, blue squares), and accretion shock emission (“planetary”; Aoyama et al. 2018, purple/yellow circles) models. Delorme 1 (AB)b’s NIR line ratios (panels (a)‒(c)) are shown in black with markers (stars, diamonds) indicating epoch as in Figure 2. Panel (d) shows Paγ/Hα line ratios, with Delorme 1 (AB)b values (unfilled markers) derived from our Paγ observations and the noncontemporaneous Hα measurement of Eriksson et al. (2020).
Paper: Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b 
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, Y. Aoyama, G.-D. Marleau, J. Bary, C. Robinson, M. Janson, W. Balmer, G. Chauvin, P. Palma-Bifani
Figure caption: TripleSpec 4.1 JHK-band spectra of Delorme 1 (AB)b (top; green: UT 2021-11-20, magenta: UT 2022-01-24) and Delorme 1 AB (bottom; blue: UT 2022-01-23, magenta: UT 2022-01-24) The NIR emission lines, Paγ, Paβ, and Brγ, are highlighted with red labels. The lines are shown in greater detail in the inset images for the companion (top; with best-fit Gaussians shown by dashed black lines) and binary host (bottom). Other atomic and molecular features are labeled in black. Gray bands indicate regions of high atmospheric absorption.
Paper: Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b 
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, Y. Aoyama, G.-D. Marleau, J. Bary, C. Robinson, M. Janson, W. Balmer, G. Chauvin, P. Palma-Bifani
Figure caption: Mass accretion rate vs. mass for all known isolated substellar accretors (gray), PMCs (black squares), and a representative sample of low-mass stars. Delorme 1 (AB)b’s NIR-derived ﹩\dot{M}﹩ is highlighted (colored markers, symbol as in Figure 2). The canonical ﹩\dot{M}\propto {M}^{2.1}﹩ (Muzerolle et al. 2005) relation for higher-mass objects (consistent with formation via collapsing prestellar cores) is shown (solid line) and a predicted relation for substellar objects formed via disk fragmentation (dashed line, α ∼ 0.001, Stamatellos & Herczeg 2015). Delorme 1 AB(b) Paγ and Brγ measurements have been offset in mass for clarity.
Paper: Stars That Approach within One Parsec of the Sun: New and More Accurate Encounters Identified in Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Color–absolute magnitude diagram, with M  G  computed assuming zero extinction. The red/yellow colored points are the 61 encounters with ﹩{d}_{\mathrm{ph}}^{\mathrm{med}}\lt 1﹩ pc identified in this work, color coded according to ﹩{d}_{\mathrm{ph}}^{\mathrm{med}}﹩. Circles denote good encounters; squares denote the questionable encounters, which are marked with a † or b in Table 1. The 13 encounters with ﹩{d}_{\mathrm{ph}}^{\mathrm{med}}\lt 0.5﹩ pc plus several others of possible interest are labeled by their order of increasing distance (row number in Table 1). For orientation, the black lines are unreddened solar metallicity PARSEC isochrones for 1 Gyr (solid) and 10 Gyr (dashed) from Marigo et al. (2017), and the small blue dots are a random subset of all sources in Gaia DR3 with ϖ > 50 mas and ruwe  < 1.2.
Paper: Can the Distance‒Redshift Relation be Determined from Correlations between Luminosities?
Authors: V. Petrosian, J. Singal, S. Mutchnick
Figure caption:  D  L (z) as would be determined by Equation (3), the method of RL, utilizing an X-ray and UV data set of quasars analyzed in Singal et al. (2022). The points show D  L (z) for individual quasars as determined for γ = 0.28 obtained by Singal et al. (2022), while the solid black line shows the best-fit curve of the form Equation (8) for these points. The dashed–dotted blue line is the result reported by RL for γ = 0.633. The dashed red line shows D  L (z) for ΛCDM. As evident, a lower value of γ yields a larger deviation from ΛCDM at high z, as discussed in Section 3.
Paper: Can the Distance‒Redshift Relation be Determined from Correlations between Luminosities?
Authors: V. Petrosian, J. Singal, S. Mutchnick
Figure caption: A determination of the best-fit power-law correlation between the X-ray and UV fluxes of quasars, in the form of Equation (4), as determined for the data set assembled in Singal et al. (2022). Results, with statistical uncertainties, are shown for both 10 (stars) and 100 (red pluses) bins of redshift with equal numbers of objects, in respective bins. The average value in each case is close to γ  f  = 0.36. These results evidence a significantly larger dispersion than those obtained by RL.
Paper: Stars That Approach within One Parsec of the Sun: New and More Accurate Encounters Identified in Gaia Data Release 3
Authors: C. A. L. Bailer-Jones
Figure caption: Perihelion (encounter) times and distances for the 61 stars that have a median perihelion distance (﹩{d}_{\mathrm{ph}}^{\mathrm{med}}﹩) below 1 pc. Negative times indicate past encounters, positive times future ones. The circles/squares show the median of the perihelion time and distance distributions computed from the 1000 data resamples (surrogates); the error bars show the 5th and 95th percentiles. Circles denote good encounters; squares denote the questionable encounters, which are marked with a † or b in Table 1. The color of each point indicates the median encounter velocity; those faster than 100 km s−1 are white.
Paper: Exponentially Amplified Magnetic Field Eliminates Disk Fragmentation around Population III Protostars
Authors: Shingo Hirano, Masahiro N. Machida
Figure caption: Phase diagrams of the absolute magnetic field strength for models B20, B15, and B10 (top to bottom) at t ps = 0, 10, and 1000 yr after the first protostar formation (left to right). The white dotted line in the top-left panel shows the power law B ∝ n 2/3 through flux freezing during the cloud compression.
Paper: Preferential Heating of Protons over Electrons from Coherent Structures during the First Perihelion of the Parker Solar Probe
Authors: Nikos Sioulas, Chen Shi, 辰 时, Zesen Huang, 泽森 黄, Marco Velli
Figure caption: Average (a) T  e  and (b) T  p  conditioned on the spatial lag, normalized to the ion inertial length d  i , estimated separation from PVI events that exceed a PVI threshold. Note that T  j , j = e, p has been normalized by the average value ﹩{\tilde{T}}_{j}﹩ within a window that spans δ ℓ = 2 · 105 d  i  and is centered around the discontinuity under study.
Paper: What are the Composition and Power of the Jet in Cyg X-1?
Authors: Andrzej A. Zdziarski, Elise Egron
Figure caption: The spectra of Cyg X-1 in the hard state. (a) The radio to IR region. The black error bars give the fluxes from Pandey et al. (2007) and Fender et al. (2000), and the red error bars are the IR fluxes (Persi et al. 1980; Mirabel et al. 1996), which are strongly dominated by the emission of the donor supergiant. The black dotted line gives a power-law fit to the 2.25–221 GHz measurements from Fender et al. (2000), with α = 0 and F  ν  = 13 mJy. The 235 and 610 MHz fluxes lie below that fit, which appears to be due to electron energy losses in the jet termination region (Zdziarski et al. 2014). The cyan symbols in the IR region show the broken-power-law fit of Rahoui et al. (2011), claiming the possible position of the break frequency. (b) The hard X-ray to soft γ-ray average spectra measured by different instruments. The spectra from the OSSE, BATSE, and COMPTEL detectors on board the Compton Gamma Ray Observatory are from McConnell et al. (2002), the spectra from the INTEGRAL ISGRI and PICsIT detectors are from Zdziarski et al. (2012), and that from the SPI detector is from Jourdain et al. (2012b). The black solid line gives a power-law approximation to its high-energy tail with the spectral index of α X ≈ −2.53 and EF  E (511 keV) ≈ 1.57 × 103 eV cm−2 s−1. The dashed lines show an approximate uncertainty of the power-law normalization (with ﹩{\rm{\Delta }}{\mathrm{log}}_{10}{F}_{E}=\pm 0.1﹩).
Paper: Preferential Heating of Protons over Electrons from Coherent Structures during the First Perihelion of the Parker Solar Probe
Authors: Nikos Sioulas, Chen Shi, 辰 时, Zesen Huang, 泽森 黄, Marco Velli
Figure caption: Binned mean of proton (T  p  in blue) and electron temperatures (T  e  in red) plotted against PVI. Error bars are also shown indicating the standard error of the mean, ﹩{\sigma }_{i}/\sqrt{n}﹩, where σ  i  is the standard deviation of the samples inside the bin. The PDFs of the electron and proton temperature p(T  e ) and p(T  p ), and the PVI index p(PVI) are shown separately in red and blue on the top and right margins of the plot, respectively.
Paper: Is Thermohaline Mixing the Full Story? Evidence for Separate Mixing Events near the Red Giant Branch Bump
Authors: Jamie Tayar, Meridith Joyce
Figure caption: Same as Figure 2 but zooming in on the abundances to emphasize that the abundances of lithium (green dotted–dashed line) and (C/N) (purple solid line) change only slightly until the thermohaline region (green) meets the base of the surface convection zone (pink), at which point the abundances of both elements at the surface begin to drop together. The abundances are rescaled so as to appear on similar axes by linearly shifting the ﹩\mathrm{log}10﹩ abundance of lithium by a factor of roughly 15. We emphasize that we do not intend or attempt to provide predictions for specific values of abundances in this study: That is a much more difficult problem, impacted by numerous physical assumptions and their uncertainties that are not relevant to our investigation of the sequence of dilution events alone.
Paper: Is Thermohaline Mixing the Full Story? Evidence for Separate Mixing Events near the Red Giant Branch Bump
Authors: Jamie Tayar, Meridith Joyce
Figure caption: Model predictions for the abundances of lithium (top) and [C/N] (bottom) are shown as the star evolves in surface gravity. Rescaled abundances are presented in the same normalized log scale as in Figures 2 and 3. The red vertical line marks the beginning of the dilution event related to the thermohaline front meeting the surface convection zone. This occurs slightly after the red giant branch bump, indicated with a purple dashed line. We show that this drop is predicted to begin at the same time step in both elements (emphasized in the zoomed-in panels on the left) and that the decline in the surface abundances at this point is significant compared to the slight changes visible earlier than and near the red giant branch bump (emphasized in the zoomed-out right panels). We note that in order to make the exact location of the initial changes visible, this figure is zoomed in significantly below the level of precision the observations can probe. For confirmation that these results are consistent across different choices of mixing efficiency α th, see Fraser et al. (2022) and the associated public repository.
Paper: Is Thermohaline Mixing the Full Story? Evidence for Separate Mixing Events near the Red Giant Branch Bump
Authors: Jamie Tayar, Meridith Joyce
Figure caption: The location in surface gravity, as a function of metallicity, of the drop in [C/N] associated with extra mixing (blue triangles), and the drop in lithium near the same point (teal diamonds). The empirical locations of the red giant branch bump from Shetrone et al. (2019) are marked by filled circles, and the estimated locations of the bump in Kirby et al. (2016) clusters that were studied by Nataf et al. (2013) are marked as open circles. While the drop in [C/N] is always above the red giant branch bump as expected, the drop in lithium abundance seems to happen significantly earlier, suggesting that a different mechanism is responsible.
Paper: Is Thermohaline Mixing the Full Story? Evidence for Separate Mixing Events near the Red Giant Branch Bump
Authors: Jamie Tayar, Meridith Joyce
Figure caption: With large samples of stars binned in metallicity, it is possible to trace chemical evolution as a function of surface gravity using lithium (teal diamonds) and [C/N] (blue triangles) as well as empirically identify the red giant branch bump (purple circle and descending line for reference). In analogy with the figures in Shetrone et al. (2019) and in order to make the changes in abundance clearer, we have indicated with lines the approximate level of the post-dredge-up, pre-bump abundances (teal and blue lines).
Paper: A Light-curve Analysis of the X-Ray Flash First Observed in Classical Novae
Authors: Mariko Kato, Hideyuki Saio, Izumi Hachisu
Figure caption: X-ray light curves for the X-ray flash models. Each panel corresponds to each model in Table 1. The red lines are the temporal variations of the photospheric temperature, T ph, which are scaled on the right-side vertical axis in red. The black lines show the estimated 0.2–10 keV (SRG/eROSITA) band flux while the blue line in panel (a) indicates the (0.3–10) keV (Swift/XRT) band flux. They are scaled on the left vertical axis. Each open circle on the black lines corresponds to the epoch when winds start. The dotted part means a wind phase. The large red dots on each black line show the X-ray luminosity at the epoch of kT ph = 28.2 eV (﹩\mathrm{log}{T}_{\mathrm{ph}}\,({\rm{K}})=5.515﹩), corresponding to the observed blackbody temperature of the YZ Ret flash. The origin of time denoted by t 0 is the observed time with SRG/eROSITA at the 23rd scan. The two green arrows indicate 4 hr before (22nd scan) and after (24th scan) the observation (23rd scan).
Paper: A Light-curve Analysis of the X-Ray Flash First Observed in Classical Novae
Authors: Mariko Kato, Hideyuki Saio, Izumi Hachisu
Figure caption: Close-up view only of the rising phases of novae in the HR diagram. Optically thick winds start at the open circles on each track. The track to the right of the open circle (low-temperature side) corresponds to the wind phase, denoted by a dotted line. Each model corresponds to those in Table 1, from upper to lower, black (Model J), red (I), blue (C), and green (D) lines, all for 1.35 M ⊙ WDs, Model E (black) and F (magenta) for 1.3 M ⊙, B (1.2 M ⊙: black), and A (1.0 M ⊙: black). The red dot with the error bars denotes k                      ﹩{T}_{\mathrm{ph}}={28.2}_{-2.8}^{+0.9}﹩ eV, L ph = (2.0 ± 1.2) × 1038 erg s−1, and radius R ph = 50,000 ± 18,000 km (= 0.07  ± 0.026 R ⊙) estimated for YZ Ret (König et al. 2022).
Paper: A Light-curve Analysis of the X-Ray Flash First Observed in Classical Novae
Authors: Mariko Kato, Hideyuki Saio, Izumi Hachisu
Figure caption: Comparison of nova outbursts in the HR diagram between a 1.0 M ☉ white dwarf (WD) (Model A) and 1.35 M ☉ WD (Model I), where L ph and T ph are the photospheric luminosity and temperature, respectively. The green lines show equiradius lines, the value of which is labeled beside each line, based on the relation of ﹩{L}_{\mathrm{ph}}=4\pi {R}_{\mathrm{ph}}^{2}\sigma {T}_{\mathrm{ph}}^{4}﹩, where R ph and σ are the photospheric radius and Stefan–Boltzmann constant, respectively. Each arrow indicates the direction of evolution. The filled red circle with error bars corresponds to the X-ray flash in YZ Ret (König et al. 2022). The open circles indicate the start of optically thick winds while the open squares represent the end of winds.