adsabs/AstroCLIMB huggingface dataset:
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: Distributions of source terms associated with the density, pressure, and temperature of neutral populations (H(1), H(2), and H(3)) along the x-axis from 70 to 140 au in Models 1 (red dots) and 2 (blue plus symbols). Top panels (a), (b), and (c) show ﹩{S}_{{{\rm{H}}}_{(1)}}^{n}﹩, ﹩{S}_{{{\rm{H}}}_{(1)}}^{p}﹩, and ﹩{S}_{{{\rm{H}}}_{(1)}}^{T}﹩ for H(1). The middle and bottom panels show the same quantities for H(2) and H(3).
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: Distributions of the temperature of the plasma (T), PUI (T PUI), and thermal proton (T p,th) in Model 1 (dashed lines) and Model 2 (solid lines) along the x-axis. Panel (a) shows the distributions on the downwind side from x = − 400 to −40 au. Panel (b) shows the distributions on the upwind side from x = 40 to 200 au.
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: Comparison of solutions obtained from our simulation with the NH and V2 observations in the supersonic SW for R ∈ [10, 80] au. The black solid lines of panels (a) and (c) show the distributions of number density and temperature obtained from the simulation for thermal protons. The number density of the PUIs and their temperature obtained from the simulation are shown in red solid lines in panels (a) and (c). The green and orange points represent the daily averages of NH data for thermal proton and PUI quantities, respectively, for R ∈ [11, 47] au. Panels (b) and (d) show the bulk flow speed and the magnetic field strength, respectively. The monthly averaged V2 data are shown with gray cross symbols.
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: Distributions of the plasma density, pressure, and temperature along the x-axis from 40 to 400 au for Model 1 (panels (a)–(c)) and Model 2 (panels (d)–(f)). The TS and HP are shown with dashed and solid gray vertical lines for Models 1 and 2, respectively.
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: Distributions of PUI pressure (top panels) and plasma temperature (bottom panels) in the meridional plane for Model 1 (left panels) and Model 2 (right panels). The HP positions are shown with the black dashed and solid lines for Models 1 and 2, respectively.
Paper: The Role of Pickup Ions in the Interaction of the Solar Wind with the Local Interstellar Medium. I. Importance of Kinetic Processes at the Heliospheric Termination Shock
Authors: R. K. Bera, F. Fraternale, N. V. Pogorelov, V. Roytershteyn, M. Gedalin, D. J. McComas, G. P. Zank
Figure caption: The same as in Figure 4, but in the equatorial plane.
Paper: Black Hole Accretion with Saturated Magnetic Pressure and Disk Wind
Authors: Jiahui Huang, Hua Feng, Wei-Min Gu, Wen-Biao Wu
Figure caption: Dominant cooling mechanism at different mass accretion rates and radii. The pink area corresponds to the region where either ADAF or SSD can exist.
Paper: Black Hole Accretion with Saturated Magnetic Pressure and Disk Wind
Authors: Jiahui Huang, Hua Feng, Wei-Min Gu, Wen-Biao Wu
Figure caption: Heating and cooling rates as a function of T i at a mass accretion rate ﹩{\dot{m}}_{10}=0.01﹩, calculated by relaxing the energy balance (Equation (5), at three characteristic radii (5, 100, and 1000 R s). ﹩{Q}_{\mathrm{vis}}^{+}﹩ is the total viscous heating rate; ﹩{Q}_{\mathrm{tot}}^{-}﹩ is the total cooling rate; and ﹩{Q}_{\mathrm{adv}}^{-}﹩, ﹩{Q}_{\mathrm{rad}}^{-}﹩, and ﹩{Q}_{{\rm{w}}}^{-}﹩ are the individual cooling components due to advection, radiation, and outflow, respectively.
Paper: Black Hole Accretion with Saturated Magnetic Pressure and Disk Wind
Authors: Jiahui Huang, Hua Feng, Wei-Min Gu, Wen-Biao Wu
Figure caption: Disk luminosity as a function of mass accretion rate. The solid curve is the bolometric luminosity, and the dashed curve is the apparent luminosity assuming isotropic emission. The Eddington luminosity defined as L Edd = 4π GM BH c/κ es is marked with a horizontal dashed line.
Paper: Black Hole Accretion with Saturated Magnetic Pressure and Disk Wind
Authors: Jiahui Huang, Hua Feng, Wei-Min Gu, Wen-Biao Wu
Figure caption: Radial structures of a hybrid disk consisting of an outer SSD and an inner ADAF, with a transition at 30 R s and a mass accretion rate ﹩{\dot{m}}_{10}=0.01﹩.
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Equatorial slice comparison for the radial velocity v  r  across the three stellar ages: ZAMS (z, top row), midMS (m, middle row), and TAMS (T, bottom row). The slices on the right represent the view of the whole domain, while the slices on the left show a zoomed-in view of the convection zones and their immediate surroundings. The extent of the BVF spikes in the midMS and TAMS models is also indicated on the left panels by means of red dashed circles. The green and magenta dashed circles on the right panels indicate the radial locations at which waves with 15 μHz (green, inner circle) and 10 μHz (magenta, outer) frequencies (with m = 1) become evanescent according to the 2D linear analysis by Ratnasingam et al. (2020).
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Frequency spectrum heat maps for all radii of the radial velocity v  r , integrated over all l, calculated at the stellar equator for models 7ZR10 (z, left) and 7mR10 (m, right). The dashed white lines represents the BVF N/2π, which approximately constrains the signal as expected for IGWs. The inset axes in the 7mR10 plot show a zoom in on the BVF spike.
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Frequency spectra for the radial velocity v  r  integrated over all l for all three stellar ages (ZAMS, top; midMS, middle; and TAMS, bottom) at multiple stellar radii. The blue line in each panel represents a power-law fit to the frequency spectrum profile taken closest to the domain’s outer boundary of the model. The vertical lines in each panel represent the smallest BVF value within the RZ (gray, dashed lines) and the BVF value at the r/R ⋆ location closest to the surface (light blue, dashed lines).
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: (a) Radial profiles of the time-averaged angular velocity perturbation Ω from the background rotation rate Ω0 for ZAMS (magenta), midMS (cyan), and TAMS (orange). The color-coded shaded regions indicate the depths of the shear flows located directly above the CZ of their respective models. (b) Radial profile for the time-averaged rate of specific angular momentum transport, ﹩{\partial }_{t}\left({r}^{2}\langle {\rm{\Omega }}\rangle \right)﹩ for the ZAMS model; the shaded area illustrates the location of the CZ.
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Frequency spectra of the radial velocity v  r  for the ZAMS (labeled “Z,” left panels) and midMS (labeled “m,” right panels) models for angular degrees l = 2 (top panels), l = 3 (middle panels) and l = 4 (bottom panels). The white vertical lines (whose length has been varied to aid readability) are the mode frequencies for the relevant model and l value as computed with GYRE. The modes are numbered according to the Eckart–Osaki–Scuflaire–Takata scheme, with negative numbers representing g-modes, positive numbers are p-modes, and zero representing the f-mode.
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Temporal evolution of the ratio between the divergences of the Reynolds and viscous stresses, ξ, as a function of fractional radius for the ZAMS (z, top) and midMS (m, bottom) models. ξ > 1 values (blue) correspond to the Reynolds stress dominating, while for ξ < 1 (red) viscous fluxes are stronger.
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Comparison between simulation spectra (black, full lines) taken 0.07H  P  below and above the CB (top and bottom panels, respectively), with power-law generation spectrum profiles generated by turbulent eddies (dotted–dashed, maroon and magenta), a power-law generation spectrum from a 2D hydrodynamical simulation (green dotted–dashed), and two exponential generation spectrum profiles caused by overshooting convective plumes (dashed lines, blue and orange).
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Mollweide projections at constant radius for the ZAMS (left) and midMS (right) models, taken at three radial locations: at the CB (top row), and at 0.02 R ⋆ (middle row) and 0.15 R ⋆ (bottom row) above it. We do not show TAMS as there is very little structure outside the BVF spike.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: Left: the binned observed CMD of all stars in density bins between 0 and 11.5 stars/arcsec2. Right: the binned observed CMD of all stars in density bins between 12 and 17 stars/arcsec2. In both CMDs, isochrones with log(age) = 6.6 to log(age) = 7.4, the F275W and F336W 50% completeness, and an A  V  = 1 vector are overplotted.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: Maps of the spatially resolved SFR as a function of lookback time with linear time bins (R.A. = [60.03–60.226], decl. = [308.50, 308.95]). Each subfigure has the same dimensions, tick marks, and extent as Figure 2. We include a color image from the unWISE catalog (Meisner et al. 2022) in the W1 and W2 filters from NEO7, taken from legacysurvey.org.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: Yellow boxes showing HST footprint of the 14 pointings of our data overlaid on a Galaxy Evolution Explorer (GALEX) NUV image from the GALEX Nearby Galaxies Survey (Gil de Paz et al. 2007 and references therein). In the magenta thumbnail is an example of the resolution of the HST data in F336W to illustrate the high spatial resolution that allowed us to get spatially resolved stellar photometry.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: Grid pattern determined via quadtree with the positions of good-quality stars in pink. The quadtree algorithm works by iteratively subdividing regions that exceed a set number of stars into four equal squares until it hits a minimum cell size, 3″ × 3″ (100 pc × 100 pc) in this study, which is roughly the size of clusters. For more details on our implementation of the quadtree algorithm, see Section 2.3.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: Maps of the spatially resolved SFR as a function of lookback time with logarithm time bins (R.A. = [60.03–60.226], decl. = [308.50, 308.95]). These plots use the same data as Figure 5, but use logarithm time bins to produce better time resolution at recent times. Each subfigure has the same dimensions, tick marks, and extent as Figure 2.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: Left: total stellar mass formed per unit area in the past 25 Myr. Right: GALEX NUV–far-ultraviolet (FUV) color image taken from legacysurvey.org.
Paper: Spatially Resolved Recent Star Formation History in NGC 6946
Authors: Debby Tran, Benjamin Williams, Emily Levesque, Margaret Lazzarini, Julianne Dalcanton, Andrew Dolphin, Brad Koplitz, Adam Smercina, O. Grace Telford
Figure caption: 50% completeness limits in both F336W and F275W plotted as a function of stellar density. The mean completeness limit of the low-density regime is overplotted as dashed–dotted and dashed lines. There are no stars with densities between 11.5 and 12, and thus none are plotted.
Paper: Influence of Solar Wind Variations on the Shapes of Venus’ Plasma Boundaries Based on Venus Express Observations
Authors: C. Signoles, M. Persson, Y. Futaana, S. Aizawa, N. André, S. Bergman, A. Fedorov, V. Lindwall, N. Martinez, C. Mazelle, S. Rojas Mata, A. Wolff, T. L. Zhang
Figure caption: BS cross section at the terminator dependence on the direction of the IMF. All plots are shown in VSE (Y, Z) [Rv] coordinates, where the Y-axis is in the direction of the IMF, and the Z-axis is in the direction of the solar wind convective electric field, both perpendicular to the solar wind flow. (a) Dependence on θ VSE at solar minimum (blue arcs) and solar maximum (orange arcs), revealing the magnetic north/south asymmetry of the BS cross section. The solid arcs are the fitted R  T  values for each θ VSE bin, and the dashed circles represent the mean radius at the terminator values, indicated in the legend. (b) and (c) Dependence on the IMF cone angle, illustrating the magnetic pole–equator asymmetry of the BS cross section in the terminator plane at (b) solar minimum and (c) solar maximum. All BS crossings are extrapolated to the terminator plane (see Section 2.5). BS crossings for low cone angles (green dots,  <25°) and high cone angles (violet diamonds, >70°) are fitted by an ellipse. For clarity, the crossings are here shown with an absolute value of Y VSE, with crossings at low cone angles to the left, and at high cone angles to the right. The number of crossings N and the semi-axis y and z values are indicated in green (upper left) for low cone angles and violet (lower right) for high cone angles. The center black circle in all panels represents Venus.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: Halo mass function at different redshifts: blue z = 0, orange z = 1, green z = 3, and red z = 5. Histograms represent the HMF of our mock catalog of surviving haloes; solid lines are the HMF determinations by Tinker et al. (2008). The difference between HMF for the catalog and the Tinker et al. (2008) determination is due to the fact that the catalog keeps into account only surviving haloes at z = 0.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: sHAR functions. Colors are as in Figure 1. Histograms are the sHAR distributions for our mock catalog; solid lines the reconstructed total sHAR for all the haloes. sHARs tend to increase with redshift on average.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: SMF from Davidzon et al. (2017). Colors are as in Figure 1. Solid lines are the SMF for star-forming galaxies; dashed lines for quenched.
Paper: TwO Parameters Semi Empirical Model (TOPSEM): Galaxy Evolution and Bulge/Disk Dicothomy from Two-stage Halo Accretion
Authors: L. Boco, A. Lapi, F. Shankar, H. Fu, F. Gabrielli, A. Sicilia
Figure caption: Fraction of disks and ellipticals as a function of stellar mass at z = 0. Solid lines are the model results; square dots are GAMA data. Orange stands for the ellipticals fraction, while the blue line is the disk fraction, and its just the reciprocus of the orange line.
Paper: Slowly Rotating Accretion Flow Around Supermassive Black Holes in Elliptical Galaxies: Case With Outflow
Authors: Razieh Ranjbar, Shahram Abbassi
Figure caption: Global solutions for L = 85, α = 0.1, γ = 5/3, and T out = 6.5 × 106 K. The three solutions shown have (s, r c) = (0, 3.1981), (0.2, 3.3651), and (0.4, 3.4381), respectively. The position of the critical point is indicated by a solid dot (saddle). The dotted curves show the Keplerian angular momentum ΩK and the Keplerian specific angular momentum l K = ΩK r 2. Variations in the flow variables with the radius r are seen in all four panels. Panel (a): variation in the radial velocity of the accretion flow with the radius. Panel (b): radial variation in the angular momentum Ω in the three solutions. Panel (c): specific angular momentum of the accretion flow l flow = Ωr 2 as a function of the radius; as a comparison, we also show the Keplerian angular momentum in the same figure. Panel (d): variations in the density of the flow ρ. These solutions are drawn for different values of s, s = 0 (black), s = 0.2 (blue), and s = 0.4 (red). The vertical dashed line and the vertical dotted line correspond to the location of the marginally stable orbit (ISCO) and the Bondi radius r B, respectively.
Paper: Slowly Rotating Accretion Flow Around Supermassive Black Holes in Elliptical Galaxies: Case With Outflow
Authors: Razieh Ranjbar, Shahram Abbassi
Figure caption: Mass accretion rate of the flow as a function of the radius, where ﹩{\dot{M}}_{\mathrm{out}}﹩ is the accretion rate at radius r = r out. The colored lines indicate the results for different values of s. The top horizontal line shows the mass accretion rate without outflow (s = 0).
Paper: Slowly Rotating Accretion Flow Around Supermassive Black Holes in Elliptical Galaxies: Case With Outflow
Authors: Razieh Ranjbar, Shahram Abbassi
Figure caption: Various velocities of the accretion flow. The adiabatic index γ = 5/3 is adopted in the calculations. For comparison, the Keplerian velocity v K and freefall velocity v ff are plotted on top of the curves.
Paper: Seismic Signatures of the 12C(α, γ)16O Reaction Rate in White Dwarf Models with Overshooting
Authors: Morgan T. Chidester, F. X. Timmes, Ebraheem Farag
Figure caption: Top: mass fraction profiles without overshooting (NOV) during the CHeB phase. Left: mass fraction profiles after core helium depletion, terminated prior to the first thermal pulse at ﹩\mathrm{log}(L/{L}_{\odot })\gt 3.0﹩. Middle: mass fraction profiles at the first wd_builder model step. These profiles have been shaved of their excess hydrogen envelope prior to running on the WD cooling track. These are the initial hot WD profiles. Right: mass fraction profiles when the models have cooled to T eff = 10,000 K. The smoothness in the profiles reflects the element diffusion processes included in the calculation. Bottom: mass fraction profiles with core overshooting (OV) during the CHeB phase, in the same format as above. Green curves represent positive σ  i  12C(α, γ)16O reaction rates, gray curves represent negative σ  i  12C(α, γ)16O reaction rates. For both positive and negative σ  i , the shading grows fainter the further σ is from the standard rate (σ = 0; black curve).
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: SED of the 159–350 disk, the only system in our sample with the disk component detected at VLA K band. Black points are flux density measurements from ALMA Band 7, ALMA Band 3, and VLA K Band. Error bars represent the total (measured plus calibration) uncertainty. Blue lines are 200 power-law fits to the two ALMA points while varying them within their uncertainties. The K band flux density is consistent with these fits (and thus with arising from dust emission) although it is on the brighter end of the expected range.
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: Disk radii and dust masses of the twelve proplyds in this sample. Masses computed assuming 20 K dust are in blue, whereas masses computed using a dust temperature set by external radiation (T  d ) are in red. The green star is the Minimum Mass Solar Nebula. The gray dotted line is the disk size–mass relation found by Tripathi et al. (2017) in low-mass star-forming regions.
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: Size of the proplyd ionization fronts vs. their projected separation from θ 1 Ori C.
Paper: Isolating Dust and Free–Free Emission in ONC Proplyds with ALMA Band 3 Observations
Authors: Nicholas P. Ballering, L. Ilsedore Cleeves, Thomas J. Haworth, John Bally, Josh A. Eisner, Adam Ginsburg, Ryan D. Boyden, Min Fang, Jinyoung Serena Kim
Figure caption: Size of the proplyd disks vs. size of the proplyd ionization fronts.