adsabs/AstroCLIMB huggingface dataset:
Paper: A Blind All-sky Search for Star Clusters in Gaia EDR3: 886 Clusters within 1.2 kpc of the Sun
Authors: Zhihong He, 治宏 何, Kun Wang, 坤 王, Yangping Luo, 杨平 罗, Jing Li, 静 李, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Same as Figure 2, but for the new candidates at high Galactic latitudes.
Paper: A Blind All-sky Search for Star Clusters in Gaia EDR3: 886 Clusters within 1.2 kpc of the Sun
Authors: Zhihong He, 治宏 何, Kun Wang, 坤 王, Yangping Luo, 杨平 罗, Jing Li, 静 李, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Histograms of the cluster extinctions derived from the isochrone fittings in this work and unrecovered OCs in CG20.
Paper: A Blind All-sky Search for Star Clusters in Gaia EDR3: 886 Clusters within 1.2 kpc of the Sun
Authors: Zhihong He, 治宏 何, Kun Wang, 坤 王, Yangping Luo, 杨平 罗, Jing Li, 静 李, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Same as Figure 2, but for the highly extinguished new candidates.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Corner plot showing the correlations between three characteristics of interest (period, OES, and temperature) and OES, temperature, and Gaia color. Core sample targets are shown in black while noncore KEBC systems are shown in gray. A few outlier systems have been removed from the OES plots for clarity (see discussion in text). Note the logarithmic x-axis of the period plots.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Corner plot showing the correlations between three characteristics of interest (period, OES, and temperature) and morphology parameter, primary eclipse depth, and absolute Gaia G magnitude. Core sample targets are shown in black while noncore KEBC systems are shown in gray. A few outlier systems have been removed from the OES plots for clarity (see discussion in text). Note the logarithmic x-axis of the period plots.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Corner plot showing the correlations between three characteristics of interest (Gaia color, morphology parameter, and primary eclipse depth) and morphology parameter, primary eclipse depth, and absolute Gaia G magnitude. Core sample targets are shown in black while noncore KEBC systems are shown in gray.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Plots comparing the primary eclipse depth to ∣OES∣. Core sample targets are shown in black while nontarget KEBC systems are shown in gray. The red dashed line shows the ODR correlation for the KEBC. The left panel’s axes are scaled linearly, while the right panel’s axes are scaled logarithmically. Both axes are in units of normalized flux. KICs 9777984, 9935311, and 11347875 are excluded from the left panel for clarity. No correlation is apparent in the left panel, but a weak correlation can be seen in the right panel.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Histogram comparing the morphology parameters for 211 of the 212 core sample targets (solid red), and all 2745 entries in the KEBC (dashed gray) that have μ ≠ −1. KIC 7667885 is not included because it lacks a value for μ (see discussion in Section 2.5). The two distributions differ significantly, particularly for μ < 0.5. The core sample also has few systems with 0.6 ≤ μ ≤ 0.7.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Plot comparing the OES to the period. Core sample targets are shown in black while nontarget KEBC systems are shown in gray. The y-axis is in units of normalized flux. KICs 9777984, 9935311, and 11347875 are excluded for clarity. Note the positive correlation in core sample systems with P < 0.5 days.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Light curves of four eclipsing binary models detailing the area around the primary minimum. Parameters for all four models are identical except for inclination. The asymmetry grows significantly more pronounced as the system changes from partially eclipsing (i = 74°, 75°) to totally eclipsing (i = 76°, 77°), demonstrating the asymmetry’s strong dependence on total eclipses.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Averaged (left) and Kepler (right) light curves of KIC 10544976 using short-cadence data showing important features, including the sharp primary eclipse and numerous flares. The right panel also plots the averaged light curve in gray for comparison.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Averaged light curve of KIC 11347875 showing the system’s concave-up region following the primary eclipse.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: Landscape of convection in main-sequence stars of different mass and spectral type. Large opacities in low-mass stars are responsible for Deep Envelope CZs and fully convective stars. Thin ionization-driven CZs can be caused by the recombination of hydrogen (H I), helium (He I and He II), and iron group elements (FeCZ) in early-type stars. For masses above 1.1 M ⊙, nuclear burning leads to steep enough temperature gradients to drive core convection. This outline is informed by 1D stellar evolution calculations; see Figure 2 in Cantiello & Braithwaite (2019) for a more quantitative picture. We warn that some of the thin ionization-driven CZs might have subcritical Rayleigh numbers and so may not have convective motions in real stars (see, e.g., Jermyn et al. 2022a).
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The angular velocity Ω is shown in terms of log T eff/spectral type and log L for stellar models with Milky Way metallicity Z = 0.014. Note that for Sun-like stars we predict angular velocities of approximately 10−4 rad s−1, which is ∼50 times faster than the current solar rotation rate.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Rossby number Ro (left) and turnover time t conv (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with He I CZs and Milky Way metallicity Z = 0.014. Note that both Ro and t conv are outputs of a theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray. Note that the turnover time exhibits numerical noise related to the model mesh resolution because the integrand 1/v  c  diverges toward the convective boundaries.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The convection optical depth τ CZ (left) and the optical depth to the surface τ outer (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with He II CZs and Milky Way metallicity Z = 0.014. Note that both of these are input parameters and do not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Rayleigh number Ra (left) and Reynolds number Re (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with He II CZs and Milky Way metallicity Z = 0.014. Note that while the Rayleigh number is an input parameter and does not depend on a specific theory of convection, the Reynolds number is an output of such a theory. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The density ratio D (left) and Mach number Ma (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with He II CZs and Milky Way metallicity Z = 0.014. Note that while the density ratio is an input parameter and does not depend on a specific theory of convection, the Mach number is an output of such a theory. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Péclet number Pe (left) and F conv/F (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with He I CZs and Milky Way metallicity Z = 0.014. Note that both Pe and F conv/F are outputs of a theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Ekman number Ek is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with He I CZs and Milky Way metallicity Z = 0.014. Note that the Ekman number is an input parameter and does not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The radiation pressure ratio β rad is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with He I CZs and Milky Way metallicity Z = 0.014. Note that this ratio is an input parameter and does not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The stiffnesses of the inner (left) and outer (right) convective boundaries are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ and ﹩\mathrm{log}L﹩ for stellar models with He I CZs and Milky Way metallicity Z = 0.014. Note that the stiffness is an output of a theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The aspect ratio A is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with He II CZs and Milky Way metallicity Z = 0.014. Note that the aspect ratio is an input parameter and does not depend on a specific theory of convection. Regions with Ra < Racrit are stable to convection and shaded in gray.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The relations between the number of training features and the mean relative error of the test data set for the six prediction models. Different panels are different machine-learning methods and different color lines are training and test data sets, respectively. The horizontal dashed lines are used to guide our eyes to the stable pattern. Notice that it is the minimum value that is labeled but it is not the final feature we adopt; we choose final features shown in Figure 23 empirically and reasonably.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The comparison between our predicted ages and the true values we use in the catalog. Different panels are different machine-learning methods and the dispersions are labeled in each panel and diagonal lines are used for comparison. The final number of features (corresponding to Figure 2) we adopt to train each model is marked at the top of each panel.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The relative age error of APOGEE and APOKASC-2 along with the age for common stars. We use two catalogs to make the prediction and find that the older the star, the more obvious the difference. The error bars are Poisson noise.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: Comparison of age predictions using two different age catalogs. The x-axis is age trained by APOGEE and the y-axis is trained by APOKASC-2; the figure is colored by star counts.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: Age determination of RC stars for testing, with six empirical stellar parameters shown in the top of each panel. We can see the precision is almost the same.
Paper: Mass and Age Determination of the LAMOST Data with Different Machine-learning Methods
Authors: Qi-Da Li, Hai-Feng Wang, Yang-Ping Luo, Qing Li, Li-Cai Deng, Yuan-Sen Ting
Figure caption: The comparison of common stars between the LS-mass and RC-mass.
Paper: A Blind All-sky Search for Star Clusters in Gaia EDR3: 886 Clusters within 1.2 kpc of the Sun
Authors: Zhihong He, 治宏 何, Kun Wang, 坤 王, Yangping Luo, 杨平 罗, Jing Li, 静 李, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Difference between the number of member stars determined in this study and those found by CG20 and Tarricq22. The dashed line indicates that the two axes have equal values.
Paper: A Blind All-sky Search for Star Clusters in Gaia EDR3: 886 Clusters within 1.2 kpc of the Sun
Authors: Zhihong He, 治宏 何, Kun Wang, 坤 王, Yangping Luo, 杨平 罗, Jing Li, 静 李, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Astrometric and photometric examples for the matched expanding clusters. The upper panel in each subplot presents the spatial distribution of the cluster members and the lower three panels show the parallax statistics, proper-motion distribution, and CMD of the cluster.
Paper: A Blind All-sky Search for Star Clusters in Gaia EDR3: 886 Clusters within 1.2 kpc of the Sun
Authors: Zhihong He, 治宏 何, Kun Wang, 坤 王, Yangping Luo, 杨平 罗, Jing Li, 静 李, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Locations of the new cluster candidates (blue dots) and matched known clusters (red dots) determined by the median positions of member stars in Galactic coordinates (0° to −180° represent 360°–180° in Galactic longitude); the CG20 OCs (ϖ > 0.8 mas) not recovered in this work are also marked (gray crosses).
Paper: A Blind All-sky Search for Star Clusters in Gaia EDR3: 886 Clusters within 1.2 kpc of the Sun
Authors: Zhihong He, 治宏 何, Kun Wang, 坤 王, Yangping Luo, 杨平 罗, Jing Li, 静 李, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Same as Figure 4, but for the examples of comparison of our results (in red) with CG20 (in blue), and Tarricq22 (in green).
Paper: A Blind All-sky Search for Star Clusters in Gaia EDR3: 886 Clusters within 1.2 kpc of the Sun
Authors: Zhihong He, 治宏 何, Kun Wang, 坤 王, Yangping Luo, 杨平 罗, Jing Li, 静 李, Xiaochen Liu, 效臣 刘, Qingquan Jiang, 青权 蒋
Figure caption: Examples of comparison of our results (in red) with CG20 (in blue). The four subplots show the spatial distribution, parallax statistics, proper-motion distribution, and CMD of the cluster members.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Averaged light curve of KIC 5282464 showing the O’Connell effect. The maximum following the primary eclipse (indicated with the upper dashed line) is noticeably brighter than the maximum preceding it (indicated by the lower dashed line).
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Histogram showing the OES distribution for the KEBC. The central peak at an OES of 0.00 rises to a value of 1367 systems and is truncated for clarity. There are 26 additional systems with ∣OES∣ > 0.03 not included in this figure for clarity. The dashed lines indicate the ∣OES∣ = 0.01 cutoff defining our sample.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Kepler light curve of KIC 9777984 showing three fits to the system: the KEBC’s original polyfit (green), the KEBC’s reconvolved polyfit (blue) that corrects for Kepler's nonzero integration time, and our fit using the Savitzky–Golay filter (red). The Savitzky–Golay curve better fits KIC 9777984's light curve and provides a more accurate measure of the eclipse depth for this system.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Averaged light curve of KIC 11347875 showing two Fourier series approximations of the system: the 50-term series used in this paper (solid red) and a 12-term series (dashed blue) similar to one Akiba et al. (2019) would use. The 50-term series follows the averaged data more closely than the 12-term series while not capturing the statistical scatter.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Histogram comparing the implied distances for the 212 core sample targets (solid red) and 2860 of 2862 entries in the KEBC (dashed gray) with Gaia EDR3 parallaxes (excluding two systems with d > 9000 pc). Our core sample’s distances range from 210 (KIC 7671594) to 7743 pc (KIC 4474637). The two distributions are similar.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Histogram comparing the luminosities for the 212 core sample targets (solid red) and all 2862 entries in the KEBC (dashed gray) with Gaia EDR3 parallaxes. Note the logarithmic scale of the x-axis. Our core sample’s calculated luminosities range from 0.02 (KIC 7671594) to 50.25 L ⊙ (KIC 5820209). Systems in our sample are less luminous on average than other KEBC systems.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Kepler short-cadence (left) and long-cadence (right) light curves of KIC 7667885. The system displays a negative O’Connell effect and at least one significant flare event.
Paper: Characteristics of Kepler Eclipsing Binaries Displaying a Significant O’Connell Effect
Authors: Matthew F. Knote, Saida M. Caballero-Nieves, Vayujeet Gokhale, Kyle B. Johnston, Eric S. Perlman
Figure caption: Histogram comparing the ratio ∣OES∣/primary eclipse depth for our core sample (solid red) and all entries in the KEBC (dashed gray). Systems with a ratio above 1 are not displayed. Core sample systems have a larger ratio on average than other KEBC systems.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The difference between the Prandtl number computed by averaging ν and χ radially and that computed by radially averaging ν/χ is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ and ﹩\mathrm{log}L﹩ for stellar models with core CZs and Milky Way metallicity Z = 0.014. Different panels show different CZs. For all but the Deep Envelope CZs the differences are small ( ≲ 2 × ), but for the Deep Envelope zones we see differences of up to 105.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Eddington ratios with the full luminosity ΓEdd (left) and the radiative luminosity (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with Deep Envelope CZs and Milky Way metallicity Z = 0.014. Note that while ΓEdd is an input parameter and does not depend on a specific theory of convection, ﹩{{\rm{\Gamma }}}_{\mathrm{Edd}}^{\mathrm{rad}}﹩ is an output of such a theory.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The convection optical depth τ CZ (left) and the optical depth to the surface τ outer (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with Deep Envelope CZs and Milky Way metallicity Z = 0.014. Note that both of these are input parameters and do not depend on a specific theory of convection.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The density ratio D (left) and Mach number Ma (right) are shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with Deep Envelope CZs and Milky Way metallicity Z = 0.014. Note that while the density ratio is an input parameter and does not depend on a specific theory of convection, the Mach number is an output of such a theory.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The radiation pressure ratio β rad is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩/spectral type and ﹩\mathrm{log}L﹩ for stellar models with Deep Envelope CZs and Milky Way metallicity Z = 0.014. Note that β rad does not depend on the steady-state convective velocity or temperature gradient, so it is not sensitive to the choice of convection theory.