adsabs/AstroCLIMB huggingface dataset:
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: ESI spectrum of AT2022lri’s host galaxy (black) and the best-fit model (red). Prominent host galaxy absorption lines are indicated by the vertical lines. The median SNR of the fitted wavelength range of 5030–5600 Å is 15.7.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Overview of the target as observed by SDO/HMI and IBIS at 15:54 UT on 2017 April 23. (a) HMI LOS magnetogram; the range of the color bar is capped for display purposes. (b) Intensity in the core of the Na I D1 line. (c) Intensity in the core of the Ca II 8542 Å line. The vertical solid lines show the eight IRIS slit positions. The dashed box outlines the Hinode/SP FOV. The solid yellow box delimits the “quiet patch” selected for inversions. The yellow circle marks the location referred to in Figure 8.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: SEDs of AT2022lri at six representative epochs (marked as dashed orange line in Figure 16). The data have been corrected for extinction (in UV/optical) and Galactic absorption (in the X-ray). The green lines show blackbody fits to the UV/optical data, with solid green lines indicating epochs where the blackbody temperature is fitted and dashed–dotted green lines where the temperature is fixed (see Section 3.3). The black lines show the NICER best-fit model with Γ fixed at 2.8 (Section 4.4.2). The purple lines depict simple power-law models used as a proxy for the SED shape in the EUV band.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Upper: evolution of bolometric luminosity L bol, 0.3–2 keV unabsorbed X-ray luminosity L X, and blackbody luminosity of the UV/optical emission L bb. Lower: evolution of L bb/L X.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Upper: evolution of 0.3–2 keV X-ray luminosities in models (C) and (D), shown both in total and contributions in different spectral components. Lower: evolution of temperature (“+” connected by dashed lines) and radius (“×” connected by solid lines) in the diskbb component in model (C) and the bbody component in model (D).
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Left: A schematic picture showing the geometry of the super-Eddington accretion flow, appropriate for our modeling with an ionized outflow as the absorber. The short dashed purple lines depict line of sights where the emission is mainly absorbed disk flux, and the long dashed blue lines highlight line of sights that primarily give rise to the emission component of the outflow. Right: a schematic picture for the reflection modeling.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Isotropic equivalent X-ray luminosity of AT2022lri and Sw J1644+57 (A. J. Levan et al. 2016; V. Mangano et al. 2016; T. Eftekhari et al. 2018) in the observer frame 0.3–10 keV, plotted as a function of rest-frame days since the assumed disruption epoch t disr. For AT2022lri, we adopt t disr = 59647 (in MJD; see Section 4.4.2); for Sw J1644+57, we adopt t disr = t trig − 15 days (A. Tchekhovskoy et al. 2014), where t trig is MJD 55648.5401.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: The mass accretion rate as a function of time in a simulated super-Eddington disk around a black hole with M BH = 106 M ⊙ and a = 0. The time-averaged accretion rate is around ﹩7{\dot{M}}_{\mathrm{Edd}}﹩. The x-axis is in unit of gravitational time r  g /c.
Paper: Subrelativistic Outflow and Hours-timescale Large-amplitude X-Ray Dips during Super-Eddington Accretion onto a Low-mass Massive Black Hole in the Tidal Disruption Event AT2022lri
Authors: Yuhan Yao, Muryel Guolo, Francesco Tombesi, Ruancun Li, Suvi Gezari, Javier A. García, Lixin Dai, Ryan Chornock, Wenbin Lu, S. R. Kulkarni, Keith C. Gendreau, Dheeraj R. Pasham, S. Bradley Cenko, Erin Kara, Raffaella Margutti, Yukta Ajay, Thomas Wevers, Tom M. Kwan, Igor Andreoni, Joshua S. Bloom, Andrew J. Drake, Matthew J. Graham, Erica Hammerstein, Russ R. Laher, Natalie LeBaron, Ashish A. Mahabal, Brendan O'Connor, Josiah Purdum, Vikram Ravi, Huei Sears, Yashvi Sharma, Roger Smith, Jesper Sollerman, Jean J. Somalwar, Avery Wold
Figure caption: Stacked XRT (0.3–10 keV) image centered around AT2022lri. The NICER FoV is shown by the dashed circle with a radius of 3.′1.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Velocity power spectra and radiative losses in a MURaM simulation. (a) LOS velocity power spectral density in the simulation (solid lines) and the inverted models (dashed lines) at the formation heights of λ5896 and λ8542 and at the height of the temperature minimum as a function of frequency. (b) Simulation vs. inversion total cooling rates in the low chromosphere for the IBIS and IBIS+IRIS models; the gray line shows the 1:1 locus; correlation coefficients and median values are displayed at the lower right.
Paper: Constraints on Acoustic Wave Energy Fluxes and Radiative Losses in the Solar Chromosphere from Non-LTE Inversions
Authors: J. M. da Silva Santos, M. Molnar, I. Milić, M. Rempel, K. Reardon, J. de la Cruz Rodríguez
Figure caption: Neural network predictions vs. inversions. Temperature (top panels) and LOS velocity (bottom panels) at a column mass in the chromosphere (﹩\mathrm{log}\xi ﹩ ∼ −3) obtained through a full inversion ((a) and (c)) and the NN prediction ((b) and (d)) of the quiet patch (see Figure 1).
Paper: Double-peaked Narrow Emission-line Galaxies in SDSS-IV MaNGA
Authors: Jiajie Qiu, Shiyin Shen, Shuai Feng, Yanmei Chen, Ruixiang Chang, Qianwen Zhao, Qi Zeng
Figure caption: An example of the single and double Gaussian profile fitting for the emission lines in a spaxel in the galaxy with MaNGA ID 1-593159. Top left: the original Hα-[N II]λ λ 6549, 6586 emission lines are shown in the solid black profile in the wavelength ranging from 6500 to 6650 Å. The black dotted line is the fitting result, containing three Gaussian profiles corresponding to [N II]λ 6549, Hα and [N II]λ 6586, respectively, from left to right. Top right: the overall profile is obtained from the result in top left panel. Bottom left: the solid black profile is the same as that in the top left panel. The dotted lines are also the fitting results, but it contains 2 × 3 Gaussian profiles. The blue and red lines represent two sets of emission lines, blue- and redshifted, respectively, each of which contains three Gaussian profiles corresponding to [N II]λ 6549, Hα λ  6564, and [N II]λ 6586, respectively, from left to right. Bottom right: the overall profile is obtained from the result in bottom left panel.
Paper: Double-peaked Narrow Emission-line Galaxies in SDSS-IV MaNGA
Authors: Jiajie Qiu, Shiyin Shen, Shuai Feng, Yanmei Chen, Ruixiang Chang, Qianwen Zhao, Qi Zeng
Figure caption: The SDSS image of the galaxy with MaNGA ID 1-593159 and the Hα-[N II]λ λ 6549, 6586 line profiles of its central 6 × 6 spaxels (3″ × 3″, white box). All grids show the original emission lines with black dotted lines. Spaxels better fitted by the double Gaussian profiles are shown with the blue- and redshifted Hα lines additionally.
Paper: Reconstruction of the Total Solar Irradiance During the Last Millennium
Authors: Valentina Penza, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Lorenza Lucaferri, Raffaele Reda, Simone Ulzega, Francesco Berrilli
Figure caption: The IMFs extracted with EMD applied to the reconstruction of F  o . The panels in the first two rows, together with the leftmost panel in the third row, show the successive order IMFs. The center panel in the third row shows the residual signal of the decomposition. The modulation function (F LT), resulting from the standardized sum of IMFs 4–7 and the residual, is shown in the bottom right panel, along with the standardized F  o .
Paper: Reconstruction of the Total Solar Irradiance During the Last Millennium
Authors: Valentina Penza, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Lorenza Lucaferri, Raffaele Reda, Simone Ulzega, Francesco Berrilli
Figure caption: Top: the relationship between the annual values of the open solar magnetic flux F  o  from I. G. Usoskin et al. (2021) and the solar modulation potential ϕ from R. Muscheler et al. (2007) for the years 1513–1899. Bottom: the same relationship after the data were divided into Gaussian bins with an FWHM of 100 Mev. The error bars represent the standard deviation of the weighted mean values. The red line represents the linear regression computed for ϕ value less than 1000 Mev (Equation (1) in the text). The Pearson’s correlation coefficient is 0.996, statistically significant at p < 0.01
Paper: Reconstruction of the Total Solar Irradiance During the Last Millennium
Authors: Valentina Penza, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Lorenza Lucaferri, Raffaele Reda, Simone Ulzega, Francesco Berrilli
Figure caption: Comparison of the annual values of the open solar magnetic flux F  o , computed by I. G. Usoskin et al. (2021; green line), with the solar modulation potential ϕ values computed by R. Muscheler et al. (2007; purple line) and I. G. Usoskin et al. (2017; black dashed line).
Paper: Reconstruction of the Total Solar Irradiance During the Last Millennium
Authors: Valentina Penza, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Lorenza Lucaferri, Raffaele Reda, Simone Ulzega, Francesco Berrilli
Figure caption: Dependence of the spot parameter P  k  on the k-cycle-averaged open solar magnetic flux F  o . The individual solar cycle numbers are indicated in the plot, with error bars representing the 1σ standard error of the mean. This relationship is well described by the linear model (solid line) provided in Equation (6). The Pearson’s correlation coefficient is 0.80, with a confidence level greater than 95% (p = 0.048).
Paper: Reconstruction of the Total Solar Irradiance During the Last Millennium
Authors: Valentina Penza, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Lorenza Lucaferri, Raffaele Reda, Simone Ulzega, Francesco Berrilli
Figure caption: Reconstruction of the open solar magnetic flux F  o  for the last century, depicted in blue. The light blue region illustrates the uncertainty range in the reconstructed time series. For comparison, data from M. J. Owens et al. (2017) spanning the time interval 1950–2022 are shown in red.
Paper: Reconstruction of the Total Solar Irradiance During the Last Millennium
Authors: Valentina Penza, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Lorenza Lucaferri, Raffaele Reda, Simone Ulzega, Francesco Berrilli
Figure caption: Relationship between monthly plage and sunspot area coverage for the years 1903–2023. The red curve represents the power-law fit to the data (Equation (5) in the text). The Spearman’s rank correlation coefficient is 0.930, statistically significant at p < 0.01.
Paper: Reconstruction of the Total Solar Irradiance During the Last Millennium
Authors: Valentina Penza, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Lorenza Lucaferri, Raffaele Reda, Simone Ulzega, Francesco Berrilli
Figure caption: Top: reconstruction of sunspot area coverage from 971 CE to the present. Bottom: the reconstructed time series (red curve) and its uncertainty range (light red region) are shown from 1900 to the present. The actual measured monthly sunspot area coverage by S. Mandal et al. (2020) is shown in green.
Paper: Reconstruction of the Total Solar Irradiance During the Last Millennium
Authors: Valentina Penza, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Lorenza Lucaferri, Raffaele Reda, Simone Ulzega, Francesco Berrilli
Figure caption: Comparison between the TSI–PMOD composite (red) and the reconstructed TSI time series (blue) from 1980 to 2020 CE (Equation (13)). The light blue region represents the uncertainty range in the reconstructed time series.
Paper: Reconstruction of the Total Solar Irradiance During the Last Millennium
Authors: Valentina Penza, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Lorenza Lucaferri, Raffaele Reda, Simone Ulzega, Francesco Berrilli
Figure caption: The same as Figure 7, but for the plage area coverage. The plage area composite by T. Chatzistergos et al. (2020) is shown in green.
Paper: Reconstruction of the Total Solar Irradiance During the Last Millennium
Authors: Valentina Penza, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Lorenza Lucaferri, Raffaele Reda, Simone Ulzega, Francesco Berrilli
Figure caption: Three different TSI reconstructions are shown for comparison. The blue line, covering the period from 971 to 2020 CE, along with its uncertainty range (light blue region), represent the results from this work. The TSI values from C.-J. Wu et al. (2018) are depicted in green, while the purple line shows the reconstruction from our 2022 study (V. Penza et al. 2022).
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Properties of the Rosseland mean opacity toward the highest temperature of our tables, at high density for ﹩\mathrm{log}(R)=6﹩. The chemical composition is defined by X = 0.7, Z = 0.01, with a scaled solar chemical mixture following E. Magg et al. (2022). Each curve corresponds to ﹩\mathrm{log}({\kappa }_{{\rm{R}}})-\mathrm{log}({\kappa }_{{\rm{R}}}^{i,\mathrm{off}})﹩, where κ R is the full opacity, including all opacity sources considered here, and ﹩{\kappa }_{{\rm{R}}}^{i,\mathrm{off}}﹩ denotes the reduced opacity obtained by excluding the specific absorbing species. This displays the temperature window to which a given opacity source contributes the most. The IPD effect is ignored in the computations of the left panel, whereas it is incorporated in the results of the right panel. In both cases, we apply thermal Doppler plus microturbulent velocity profiles for molecular transitions.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Left panel: map of the gas pressure as a function of T and R. Contour levels are distributed every 1 dex in ﹩\mathrm{log}({P}_{\mathrm{gas}})﹩. The white contour draws the locus of points where the logarithmic difference in Rosseland mean opacity treated with a thermal Doppler profile and pressure broadening equals 0.001 dex in the regime where molecular transitions are important, for T ≤ 4000 K. Right panel: map of the differences in Rosseland mean opacities between computations that include the IPD effect and pressure broadening for molecular transitions and those that ignore the IPD and assume Doppler broadening regardless of pressure. Contour levels are distributed every 0.05 dex in ﹩{\rm{\Delta }}\mathrm{log}({\kappa }_{{\rm{R}}})﹩. The chemical composition is the same as in Figure 10.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Comparison of Rosseland mean gas opacities computed in this work and by other studies. Left panel: Comparison with M. G. Malygin et al. (2014). The reference solar chemical composition is taken from N. Grevesse & A. J. Sauval (1998), with metallicity Z = 0.01696 and hydrogen abundance X = 0.7347. Right panel: Comparison with R. S. Freedman et al. (2014). The reference solar chemical composition is taken from K. Lodders (2003), with metallicity Z = 0.0133 and hydrogen abundance X = 0.7491. Values for ﹩\mathrm{log}(R)﹩ are labeled.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Left panel: molecular gas opacity as a function of wavenumber at T = 1585 K, gas pressure P gas = 211 bar, and density ρ = 0.004 g cm−3. The reference solar chemical composition is taken from E. Magg et al. (2022), with metallicity Z = 0.02 and hydrogen abundance X = 0.7. The blue curve represents the monochromatic opacity without the contribution of alkali atoms Na and K, whereas the magenta curve includes the two atoms’ opacity contributions. Right panel: the Rosseland mean opacity as a function of temperature at three densities (g cm−3). Magenta lines include the opacity from alkali atoms Na and K, whereas dashed blue lines do not. The chemical composition is scaled solar according to E. Magg et al. (2022), with metallicity Z = 0.01 and hydrogen abundance X = 0.7.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Rosseland mean gas opacities computed in the temperature range 100 ≤ T/K ≲ 30,000 and encompassing the R interval ﹩-8\leqslant \mathrm{log}(R)\leqslant 6﹩ in steps of 0.5 dex. The chemical composition is defined by X = 0.7, Z = 0.01, with a scaled solar chemical mixture following E. Magg et al. (2022). Left panel: opacities assuming Doppler plus microturbulent velocity molecular line profiles and ignoring the IPD effect. Right panel: opacities assuming pressure broadening for molecular line profiles and accounting for the IPD effect.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Properties of the Rosseland mean opacity for temperatures where solid grains dominate, at low density (﹩\mathrm{log}(R)=-3﹩, left panel) and high density (﹩\mathrm{log}(R)=6﹩, right panel). The chemical composition is defined by X = 0.735, Z = 0.0165, with scaled solar elemental abundances following E. Magg et al. (2022). Each curve represents the contribution of major solid species to the total Rosseland mean opacity, and it is calculated as ﹩\mathrm{log}({\kappa }_{{\rm{R}}})-\mathrm{log}({\kappa }_{{\rm{R}}}^{i,\mathrm{off}})﹩, where κ R is the full opacity including all opacity sources considered here, and ﹩{\kappa }_{{\rm{R}}}^{i,\mathrm{off}}﹩ is the reduced opacity computed by excluding the specific absorbing species.
Paper: ÆSOPUS 2.1: Low-temperature Opacities Extended to High Pressure
Authors: Paola Marigo, Francesco Addari, Diego Bossini, Alessandro Bressan, Guglielmo Costa, Léo Girardi, Giada Pastorelli, Michele Trabucchi, Guglielmo Volpato
Figure caption: Comparison of the widths of Doppler line cores vs. Lorentzian profiles in the pressure–temperature diagram according to the analysis of C. Hedges & N. Madhusudhan (2016). The boundary between the two regimes is denoted by the white line. Above the horizontal black line, molecular transitions are treated with a Voigt profile extracted from the ExoMolOP database (K. L. Chubb et al. 2021).