adsabs/AstroCLIMB huggingface dataset:
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 Deep Envelope 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.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Prandtl number Pr (left) and magnetic Prandtl number Pm (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 Pr and Pm are input parameters and so 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 Ekman number Ek 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 the Ekman number is an input parameter and does 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 aspect ratio A 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 the aspect ratio is an input parameter and does 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 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 He I 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. Regions with Ra < Racrit are stable to convection and shaded in gray. Note that the two panels appear very similar because He I CZs are so inefficient that they transport almost no flux, so the radiative temperature gradient is very similar to the realized temperature gradient in MLT.
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 I 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 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 I 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 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 H 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 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 H 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.
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 I 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 Prandtl number Pr (left) and magnetic Prandtl number Pm (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 Pr and Pm are input parameters and so 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 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 H 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 against 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 I 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: 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 core 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 stiffness of the outer convective boundary 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. 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: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: An example of the information explored in the quality control process for the galaxy/cube manga-7495-12703. The panels on the left comprise, from the top left to the bottom right: (i) a true color image created using the SDSS u-, g-, and r-band images; (ii) the same image created using images in the same bands synthesized from the MaNGA data cube; (iii) a similar true color image created using the [O III]5007 (blue), Hα (green), and [N II]6584 (red) flux intensity maps, together with the (iv) ﹩{{ \mathcal A }}_{\star ,L}﹩, (v) ﹩{{ \mathcal Z }}_{\star ,L}﹩, and (vi) A V,⋆ maps, all of them derived as part of the pyPipe3D process. The panels on the right show the normalized mass assembly (top) and the metallicity enrichment history (bottom) for this galaxy at different galactocentric distances (indicated with different colors), estimated from the pyPipe3D analysis following the procedures described in Camps-Fariña et al. (2021, 2021). We remark that no S/N mask has been applied to the data, so, therefore, the results corresponding to the outer regions in all panels are highly unreliable (e.g., the apparent increases of ﹩{{ \mathcal A }}_{\star ,L}﹩ and ﹩{{ \mathcal Z }}_{\star ,L}﹩ at the edge of the FOV and/or the metallicity history beyond 2 Re).
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Example of the content of the SSP extension in the Pipe3D FITs file, corresponding to the MaNGA data cube (galaxy) manga-7495-12704. Each panel shows a color image of the property stored in the corresponding channel of the data cube, as listed in Table 3. The index, corresponding property, and units are indicated in each panel with the labels at the bottom right, bottom left, and top right.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: An example of the information explored in the quality control process for the galaxy/cube manga-7495-12703. The top panel shows the central 5″/aperture spectrum of this galaxy (solid black line), together with the best-fitting model (solid yellow line), using the SSP template adopted in the derivation of the nonlinear parameters of the stellar population (Section 4.1 of Lacerda et al. 2022), and the residual of the original spectrum from the subtraction of this model. The gray and blue shaded areas correspond to masked regions along the full fitting process and in the first iteration of the analysis before subtracting the emission lines, respectively. The coefficients of the decomposition in this SSP library, i.e., the fraction of light at the normalization wavelength for each template in the library (w ssp in Equation (1)), are shown in the bottom panel as a heatmap for the four ages and three metallicities of the considered library. The nonlinear parameters (systemic velocity, velocity dispersion, and dust extinction) and the LW and MW age and metallicity are indicated in the legend at the top right.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Distribution of galaxies in the MaNGA sample, in the color–redshift diagram (left panel) and the color–magnitude diagram (right panel). Each solid dot corresponds to one of the analyzed objects, color coded by its Sérsic index. The contours represent the density distribution, encircling 90%, 65%, and 40% of the objects, respectively. Density distributions of the full sample (black lines) and the segregated in bins of Sérsic index (colored lines) as a function of redshift, absolute magnitude, and color are represented at the upper and right edges of the panels. All parameters were extracted from the NSA catalog.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Example of the content of the SFH extension in the Pipe3D FITs file, corresponding to the MaNGA data cube (galaxy) manga-7495-12704. Each panel shows a color image with the fraction of light at the normalization wavelength (w ⋆,L ) for the different age ranges included in the SSP library. The age range is indicated in the bottom left boxes, and the corresponding indices of the coadded channels in the SFH extension are shown in the bottom right legends. For clarity, we do not show the individual w ⋆,L  maps included in the SFH extension.
Paper: SDSS-IV MaNGA: pyPipe3D Analysis Release for 10,000 Galaxies
Authors: S. F. Sánchez, J. K. Barrera-Ballesteros, E. Lacerda, A. Mejía-Narvaez, A. Camps-Fariña, Gustavo Bruzual, C. Espinosa-Ponce, A. Rodríguez-Puebla, A. R. Calette, H. Ibarra-Medel, V. Avila-Reese, H. Hernandez-Toledo, M. A. Bershady, M. Cano-Diaz, A. M. Munguia-Cordova
Figure caption: Similar to Figure 5, showing the w ⋆,L  for the different metallicities included in the adopted SSP library (indicated in the bottom left boxes), corresponding to the channels of the SFH extension indicated in the bottom right legends.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Star formation rate as a function of time for the isolated galaxy simulations given in Table 2. The No-FB run has the highest SFR, and the SNII-thermal run shows weak suppression of SFR. In other runs, SFR is suppressed by the mechanical SN FB efficiently.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Mass (top row), energy (second row), and metal (third row) loading factors vs. the height above the galactic plane. The fourth row depicts outflow velocity vs. the height above the galactic plane. All quantities are measured using cylinders of different heights and a 10 kpc radius and averaged over t = 0.5 − 1.0 Gyr. The lines indicate the average values during this time period, with ±1σ shade for time variation.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Phase diagram of the gas in the isolated galaxies given in Table 2 at t ≃ 1 Gyr. The dense, cold gas (T < 103 K) in the galactic disk is visible on the lower right corner. The hot, tenuous gas heated by feedback adiabatically cools and then joins the hot, gaseous halo in the upper left region with T ∼ 106 K. The hot component is most visible in the SNII-thermal run due to the highest star formation rate and subsequent strong thermal feedback. The hot gas seen in the No-FB run is due to the hot halo implemented in the initial condition.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: The Kennicutt–Schmidt relation of the simulated galaxies given in Table 2 at t ≃ 1 Gyr, calculated with 500 × 500 pc patches. Colored regions depict the observational data of nearby spiral galaxies (blue: Schruba et al. 2011; magenta: Bigiel et al. 2008).
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Same as Figure 18 but measured with spheres of different radii up to 200 kpc, centered at the galactic center and averaged between t = 0.5 − 1.0 Gyr. The lines show the average during this time period with ±1σ shade for the time variation.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Star formation rate as a function of time for the Fiducial and High-reso runs.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Same as Figure 19 but for the Fiducial and High-reso runs.
Paper: Osaka Feedback Model. II. Modeling Supernova Feedback Based on High-resolution Simulations
Authors: Yuri Oku, Kengo Tomida, Kentaro Nagamine, Ikkoh Shimizu, Renyue Cen
Figure caption: Same as Figure 18 but for the Fiducial and High-reso runs.
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 luminosity to the period. Core sample targets are shown in black while nontarget KEBC systems are shown in gray. KICs 3662635 and 5820209 are excluded for clarity. The sharp edge near the lower left corner denotes the short-period limit for a given luminosity. Most of the core sample is clustered near or along this edge.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The Eddington ratio with the full luminosity ΓEdd (upper) and the radiative luminosity (lower) are shown averaged over the outermost pressure scale height (left) and innermost one (right) 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 Rossby number Ro (upper) is shown averaged over the outermost pressure scale height (left) and innermost one (right) 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 numbers were calculated here using the pressure scale height at the relevant boundary rather than the full width of the CZ δr.
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 Deep Envelope CZs and Milky Way metallicity Z = 0.014. Note that both Ro and t conv are outputs of a 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 Prandtl number Pr (upper) and magnetic Prandtl number Pm (lower) are shown averaged over the outermost pressure scale height (left) and innermost one (right) 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 Pr and Pm are input parameters and so 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 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 Deep Envelope CZs and Milky Way metallicity Z = 0.014. Note that both Pe and F conv/F are outputs of a 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 Mach number Ma is shown averaged over the outermost pressure scale height (left) and innermost one (right) 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 the Mach number is an output of a 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 Reynolds number Re is shown averaged over the outermost pressure scale height (left) and innermost one (right) 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 the Reynolds number is an output of a 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 radiation pressure ratio β rad is shown averaged over the outermost pressure scale height (left) and innermost one (right) 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.
Paper: An Atlas of Convection in Main-sequence Stars
Authors: Adam S. Jermyn, Evan H. Anders, Daniel Lecoanet, Matteo Cantiello
Figure caption: The stiffness of the inner convective boundary is shown in terms of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ and ﹩\mathrm{log}L﹩ for stellar models with Deep Envelope CZs and Milky Way metallicity Z = 0.014. Note that the stiffness is an output of a 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 Péclet number Pe (upper) and F conv/F (lower) are shown averaged over the outermost pressure scale height (left) and innermost one (right) 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 these quantities are calculated here using the pressure scale height at the relevant boundary rather than the full width of the CZ δr.
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 H I 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.