adsabs/AstroCLIMB huggingface dataset:
Paper: Io’s SO2 and NaCl Wind Fields from ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Martin A. Cordiner, Imke de Pater, Arielle Moullet, Statia Luszcz-Cook
Figure caption: Retrieved SO2 and NaCl LOS velocity maps for pixels with spectral SNR ≥ 10 used to derive Io's wind field shown in Figure 4. The color bar corresponds to approaching (blue) and receding (red) LOS velocities. SO2 velocities on Io's sub-Jovian hemisphere pre- and posteclipse from observations in 2018 are shown in panels (A)–(C); SO2 velocities at Jupiter's eastern and western elongations are shown in panels (D) and (G) for observations in 2021 and (E) and (H) for observations in 2022; and NaCl velocities from both Jovian elongations observed in 2022 are shown in panels (F) and (I). Each panel corresponds to those in Figure 4 before the subtraction of Io's solid-body rotation. Io's solid-body radius, latitude, and longitude lines are denoted by the gray grid, with latitude and longitude contours increasing in increments of 22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 and 30°, respectively. The subobserver central longitude is shown in the lower right of each panel, and the ALMA beam (FWHM of the PSF) for each observation is shown as a hashed ellipse in the lower left of each panel.
Paper: Io’s SO2 and NaCl Wind Fields from ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Martin A. Cordiner, Imke de Pater, Arielle Moullet, Statia Luszcz-Cook
Figure caption: Comparison of the retrieved wind map of the SO2 (﹩{J}_{{K}_{a},{K}_{c}}=1{9}_{1,19}-1{8}_{0,18}﹩) spectral line at 346.7 GHz (A) with solid-body rotation models ((B)–(D)) and the final derived wind maps ((E)–(G)) following the subtraction of the models from the data. Different rotation models were tested: a pure solid-body rotation model (B), the solid-body rotation model convolved with the ALMA beam (C), and solid-body rotation extending off the surface of Io to the ALMA beamwidth and subsequently convolved with the beam shape (D). The wind fields ((E)–(G)) result from the velocity field (A) subtracted by the corresponding model in the panel above (e.g., velocities A – model B = winds E).
Paper: Formation Rate of Quasiperiodic Eruptions in Galactic Nuclei Containing Single and Dual Supermassive Black Holes
Authors: Chunyang Cao, F. K. Liu, Xian Chen, Shuo Li
Figure caption: Rate of QPEs (Γ) produced by Hills-captured stars with periods shorter than P when the SMBH is of 106M⊙ (left panel) and 107M⊙ (right panel). The gray lines show the rates in a single-SMBH system where stellar binaries are scattered to the SMBH by two-body relaxation in the galactic nucleus of cored (γ = 1, squared), cuspy (γ = 1.75, circle), and extremely cuspy (γ = 2.6, triangle) density profiles. The black lines show the rates in a dual-SMBH system consisting of two equal-mass SMBHs separated by 2ri, and the contributions from four subgroups of progenitor stellar binaries are separately shown: MS-MS (red dashdot), WD-MS (blue loosely dashed), NS-MS (purple densely dashed), and sBH-MS (green dotted).
Paper: Io’s SO2 and NaCl Wind Fields from ALMA
Authors: Alexander E. Thelen, Katherine de Kleer, Martin A. Cordiner, Imke de Pater, Arielle Moullet, Statia Luszcz-Cook
Figure caption: Retrieved velocity error maps corresponding to the velocity maps shown in Figure 6. Velocity errors are shown where the gas emission is ≥10× the spectral rms noise and within an ALMA beamwidth (shown in the lower left) of Io's surface. Io's solid-body radius, latitude (22﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 increments), and longitude (30° increments) lines are represented by the grid in gray.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: Left: stellar age vs. C2H2 to water flux ratio for the mid-to-late M disk sample, using the same target labeling as Figure 5. The size of the symbol corresponds to the disk flux at 0.9 mm (scaled to 150 pc). Right: the distribution of millimeter fluxes for mid-to-late M-star disks from Lupus (M. Ansdell et al. 2016), Cha I (I. Pascucci et al. 2016), Upper Sco (S. A. Barenfeld et al. 2016), and other older systems (K. Flaherty et al. 2019; P. F. Cronin-Coltsmann et al. 2023; this work). Values for young disks are taken from the compiled table in C. F. Manara et al. (2023), and only >3σ detections are included. The width in each “violin” reflects the density of data points along the y-axis.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: Left: the 17.22 μm water line luminosity vs. C2H2 Q-branch line luminosity for a mixed sample from JWST and Spitzer. Right: the 17.22 μm water line luminosity vs. C2H2 to water flux ratio. The M star sample refers to stars with spectral type later than M3 and is labeled with the target name: 1, this work; 2, A. M. Arabhavi et al. (2024); 3, B. Tabone et al. (2023); 4, C. Xie et al. (2023); 5–11, I. Pascucci et al. (2013); 12 and all T Tauri disks, A. Banzatti et al. (2020). The 3σ upper limits are indicated with arrows. Targets with upper limits for both lines are excluded in the right panel for flux ratios.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: Left: the input gas C/O ratio vs. the output column density ratio of C2H2 and CO2 from J. R. Najita et al. (2011) chemical models (connected gray dots). The observed values/ranges of the JWST mid-to-late M-star disk sample are highlighted in colors, except for Sz 28, for which the derived column densities are highly uncertain (J. Kanwar et al. 2024b). Three disks with derived column densities from Spitzer/IRS data (I. Pascucci et al. 2013) are indicated as gray dotted lines. Right: stellar age vs. the derived C/O ratio from model grids. The lower limit is marked for J155829, as CO2 was not detected with the Spitzer data.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: Left: zoomed-in spectra around molecular hydrogen pure rotational lines. Fitted Gaussian profiles are overplotted for detected lines. H2 S(2), S(4), and S(5) are blended with hydrocarbon emissions, for which the slab models are indicated in blue with the original data spectra shown in gray. The vertical dashed lines mark the line center for nondetection. Right: the detection of [Ne II] at 12.814 μm and [Ar II] at 6.985 μm.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: Left: the SED of J0446A including the JWST MIRI/MRS spectrum in blue (the noisy long-wavelength range is marked with a lighter color). The gray curve shows a stellar photospheric model with Teff = 3100 K. The VISTA J-band flux of J0446A might be problematic, as this flux is comparable to that of J0446B, while J0446A is consistently fainter in all other bands. Right: the comparison of the Gaia XP spectra of J0446B to the XP spectra of objects in the TW Hya association with varying spectral types. The molecular absorption bands are consistent with a spectral type of M4.5.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: Top: the MIRI/MRS spectrum (black) of the disk of J0446B and the estimated continuum emission (orange). The shorter wavelength affected by stellar absorption and the wavelength range longer than 18 μm with worse data quality and no lines of interest are cut out. The identified molecules are marked out. Bottom: the continuum-subtracted spectrum (gray), where the regions with pseudo-continuum emission from the optically thick C2H2 component are highlighted.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: The comparison of data and model spectra. Top panels: the continuum-subtracted data spectrum (black) with a model spectrum (orange shaded region) composed of all fitted species. The optically thick emission of C2H2 is highlighted in light blue. Bottom panels: model spectra for individual molecules in each wavelength segment. The inset plot highlights the marginal detection of H2O, and the possible detection of emission lines around 17.62 μm remains unidentified.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: The modeled time evolution of the gas-phase C/O ratio using chemcomp (A. D. Schneider & B. Bitsch 2021) in a disk around a very low-mass star, with stellar properties consistent with J0446B. The line styles represent different α viscosity, and the line colors represent different initial disk masses.
Paper: The First JWST View of a 30-Myr-old Protoplanetary Disk Reveals a Late-stage Carbon-rich Phase
Authors: Feng Long, 凤 龙, Ilaria Pascucci, Adrien Houge, Andrea Banzatti, Klaus M. Pontoppidan, Joan Najita, Sebastiaan Krijt, Chengyan Xie, Joe Williams, Gregory J. Herczeg, 雷歌 沈, Sean M. Andrews, Edwin Bergin, Geoffrey A. Blake, María José Colmenares, Daniel Harsono, Carlos E. Romero-Mirza, Rixin Li, 日新 李, Cicero X. Lu, Paola Pinilla, David J. Wilner, Miguel Vioque, Ke Zhang
Figure caption: The observed spectrum of J0446B (black) in comparison with CO (orange) and H2O (blue) models (scaled) with an emitting temperature of 3100 K.
Paper: Fire and Ice in the Whirlpool: Spatially Resolved Scaling Relations between X-Ray-emitting Hot Gas and Cold Molecular Gas in M51
Authors: Chunyi Zhang, Junfeng Wang, Tian-Wen Cao
Figure caption: Correlations between the emission of hot gas and the total infrared luminosity across the entire galaxy at the kiloparsec scale. The red points represent regions within the central 2 kpc, and the gray points are regions located in the disk. The blue points show the binned trend for the X-ray luminosities across the disk. Each total infrared luminosity bin spacing is 0.08 dex. The solid and dashed lines are the best fit of the ﹩{L}_{0.5-2\,{\rm{keV}}}^{{\rm{gas}}}﹩–LIR relations for the center and the mean X-ray luminosities. The purple box includes almost 80% of the disk regions, which presents a more gradual trend.
Paper: Fire and Ice in the Whirlpool: Spatially Resolved Scaling Relations between X-Ray-emitting Hot Gas and Cold Molecular Gas in M51
Authors: Chunyi Zhang, Junfeng Wang, Tian-Wen Cao
Figure caption: Correlations between the hot gas emission and the four molecular line luminosities. The symbols (points and lines) are as in Figure 4. The parameters a and b of the best fit for ﹩{\rm{log}}﹩ ﹩{L}_{0.5-2\,{\rm{keV}}}^{{\rm{gas}}}﹩ = a﹩{\rm{log}}﹩ ﹩{L}_{{\rm{gas}}}^{{\prime} }﹩ + b are shown in the lower right corner of each panel.
Paper: Fire and Ice in the Whirlpool: Spatially Resolved Scaling Relations between X-Ray-emitting Hot Gas and Cold Molecular Gas in M51
Authors: Chunyi Zhang, Junfeng Wang, Tian-Wen Cao
Figure caption: Maps of the total infrared, diffuse X-ray luminosity, and LIR/﹩{L}_{0.5-2\,{\rm{keV}}}^{{\rm{gas}}}﹩ ratios along the galactic radius. The units are given above each panel and all maps are logarithmic. Left: the infrared luminosity is convolved to 33″ resolution. The black lines indicate contour levels of logLIR = 8.4, 8.9, and 9.3L⊙. Middle: the contour levels of log﹩{L}_{0.5-2\,{\rm{keV}}}^{{\rm{gas}}}﹩ = 4.5, 4.9, 5.2, and 5.8L⊙. Right: the red dashed line represents the average LIR/﹩{L}_{0.5-2\,{\rm{keV}}}^{{\rm{gas}}}﹩ ratio across the galaxy. The white crosses indicate the central position of the galaxy.
Paper: Fire and Ice in the Whirlpool: Spatially Resolved Scaling Relations between X-Ray-emitting Hot Gas and Cold Molecular Gas in M51
Authors: Chunyi Zhang, Junfeng Wang, Tian-Wen Cao
Figure caption: Radial distribution of hot gas luminosity and surface brightness (0.5–2.0 keV). Top panel: radial profile of luminosity. The gray points denote regions matched to the millimeter data, and the red points are average values of the X-ray luminosities within the intervals r = n  ×  0.4 kpc + 0.2 kpc  ± 0.2 kpc, where n = 0,1...19. The error bars are the statistical uncertainty of the average X-ray luminosities. Bottom panel: surface brightness profile of hot gas. The surface brightness profile is constructed in concentric annuli across the entire galaxy. The dashed line shows the radius of 2 kpc (50″) to distinguish the galactic center and the outer disk.
Paper: Fire and Ice in the Whirlpool: Spatially Resolved Scaling Relations between X-Ray-emitting Hot Gas and Cold Molecular Gas in M51
Authors: Chunyi Zhang, Junfeng Wang, Tian-Wen Cao
Figure caption: Correlations between X-ray radiation efficiency and star formation rate surface density at the kiloparsec scale. The color code represents the distance from the galactic center. The purple- and black-bordered points correspond to regions within 0.6 and 2 kpc of M51, respectively. The blue and gray curves are the derived relationships between η and ΣSFR for the center and the disk.
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Spot, penumbral, and umbral contrasts for the G2 dwarfs. The curves in the top row are the absolute contrasts computed, using Equation (1), from the 3D MHD simulations and using radiative-equilibrium models with the same Teff as the MHD case (﹩{T}_{{\rm{eff}}}^{{\rm{MHD}}}-{T}_{{\rm{eff}}}^{{\rm{RE}}}={\rm{\Delta }}{T}_{{\rm{eff}}}=0﹩, red lines). The relative contrasts, computed using Equation (2), for the respective cases are plotted on a logarithmic scale in the middle row. To simplify the comparison of the wavelength dependencies returned by MHD and 1D RE calculations we normalize both relative and absolute contrasts by their integrals over the wavelength domain we show. In other words, the areas under all shown curves for absolute and relative contrasts are equal to unity. In the bottom row are the relative differences, defined in Equation (3), between the MHD contrasts and RE contrasts, shown here for different RE models, including those with ΔTeff = ±50 and ±100 K (see legend). The relative differences are computed from the absolute contrasts but without the normalization. See Section 5.1 for more details.
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Disk center intensity images of the spots for G2, K0, and M0 dwarfs at four representative wavelengths computed with the MPS-ATLAS code. The yellow and cyan contours indicate the masks that were used to select the penumbral and umbral regions in each case. All images have been normalized to their respective spatially averaged quiet region intensities. The gray scale indicates relative intensities between 0 (black) and 1.2 (white) as indicated by the color bar.
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: CLV of the spatially averaged intensities from the quiet region, spot, penumbra, and umbra for the G2, K0, and M0 dwarfs. The penumbral and umbral regions were selected using the contours shown in Figure 1. The spot spectra were computed by spatially averaging over the combined penumbral and umbral regions. Similarly, the quiet region spectra were taken from two narrow horizontal bands at the top and bottom of the intensity images, away from the spot.
Paper: Equation of State Independent Determination on the Radius of a 1.4 M⊙ Neutron Star Using Mass–Radius Measurements
Authors: Chun Huang
Figure caption: The posterior of R1 and R2 in Scenario 2 under different hotspot configuration choices of J0030 after applying the condition that all the sources are 1.4 M⊙ stars. The numbers reported above each 1D marginal distribution refer to the ST+PDT result. Lime green is the ST+PST choice of J0030 plus J0437 resulted posterior, blue is the one from PDT-U, and the red posterior is the result from ST+PDT. The contour levels in the corner plot, going from deep to light colors, correspond to the 68%, 84%, and 98.9% levels. The dashed line in the 1D corner plots represents the 68% credible interval, and the title of this plot indicates the median of the distribution as well as the range of the 68% credible interval.
Paper: Equation of State Independent Determination on the Radius of a 1.4 M⊙ Neutron Star Using Mass–Radius Measurements
Authors: Chun Huang
Figure caption: The 1D distribution of 1.4 M⊙ star radius R1.4 from joint J0030 and J0437 inference results, with mass–radius measurements of J0030 resulting from (a) ST+PST model, (b) ST+PDT model, and (c) PDT-U model. The dashed lines represent the quantiles of each distribution at 16%, 50%, and 84%. The density function is computed using KDE estimation.
Paper: Equation of State Independent Determination on the Radius of a 1.4 M⊙ Neutron Star Using Mass–Radius Measurements
Authors: Chun Huang
Figure caption: The joint posterior distribution of R1.4 under different hotspot configuration choices of J0030 after applying the condition that all the sources are 1.4 M⊙ stars. Lime green is the ST+PST choice of J0030 plus J0437 resulted posterior, blue is the one from PDT-U, and the red posterior is the result from ST+PDT. The dashed line with same color as the distribution plots represents the corresponding 95% credible interval.
Paper: Equation of State Independent Determination on the Radius of a 1.4 M⊙ Neutron Star Using Mass–Radius Measurements
Authors: Chun Huang
Figure caption: The 1D distribution of 1.4 M⊙ star radius R1.4 from injected data set: (1) NL3ωρ and (2) TM1-2ωρ. The injected R1.4 value from the chosen EOS is shown by the black dashed line. The red dashed lines represent the quantiles of each distribution at 16%, 50%, and 84%. The density function is computed using KDE estimation.
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Same as Figure 3 but for M dwarfs. Unlike for the G and K dwarfs, the difference in Teff between the quiet region and the penumbra in the MHD simulations is less than 100 K, hence we present a comparison with RE models only for ΔTeff = ±50 K.
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Effects of horizontal inhomogeneities on the contrasts. Comparison between the spatially averaged penumbral and umbral contrasts (Equation (2)) from the 3D MHD cube for an M0V dwarf and the contrasts computed from the “1D MHD” atmospheres obtained by spatially averaging the atmospheres over the respective yellow boxes in panel (a).
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Relative difference between RE and MHD contrasts (see Equation (3)) for the spot, penumbra, and umbra for the three spectral types (given on the right-hand side of the figure) and three values of the cosine of the heliocentric angle (i.e., angle between the line of sight and the local stellar surface normal) μ: 1 (disk center, black curve), 0.6 (intermediate disk position, orange curves), and 0.3 (near the limb, maroon curves).
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Relative contrasts for the M0 star from the spatially averaged 1D MHD atmosphere computed without the opacities from H2O molecules (panels (a1) and (a2)), without the opacities from the TiO molecules (panels (b1) and (b2)), and without the opacities from the diatomic molecules (panels (c1) and (c2)). The top row shows the penumbral contrasts, while the umbral contrasts are plotted in the bottom row.
Paper: First Calculations of Starspot Spectra Based on 3D Radiative Magnetohydrodynamics Simulations
Authors: H. N. Smitha, Alexander I. Shapiro, Veronika Witzke, Nadiia M. Kostogryz, Yvonne C. Unruh, Tanayveer S. Bhatia, Robert Cameron, Sara Seager, Sami K. Solanki
Figure caption: Same as Figure 3 but for K dwarfs.