adsabs/AstroCLIMB huggingface dataset:
Paper: Very Bright, Very Blue, and Very Red: JWST CAPERS Analysis of Highly Luminous Galaxies with Extreme Ultraviolet Slopes at z = 10
Authors: Callum T. Donnan, Mark Dickinson, Anthony J. Taylor, Pablo Arrabal Haro, Steven L. Finkelstein, Thomas M. Stanton, Intae Jung, Casey Papovich, Hollis B. Akins, Anton M. Koekemoer, Derek J. McLeod, Lorenzo Napolitano, Ricardo O. Amorín, Ryan Begley, Denis Burgarella, Adam C. Carnall, Caitlin M. Casey, Antonello Calabrò, Fergus Cullen, James S. Dunlop, Richard S. Ellis, Vital Fernández, Mauro Giavalisco, Michaela Hirschmann, Weida Hu, Garth Illingworth, Jeyhan S. Kartaltepe, Dale D. Kocevski, Vasily Kokorev, Ho-Hin Leung, Ray A. Lucas, Alexa M. Morales, Ross McLure, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Struan Stevenson, Jonathan R. Trump, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: A comparison of the UV magnitude and redshift of COSMOS-52185 and COSMOS-300001, individually (green point) and stacked (green star), and EGS-25297 (red point) to the total sample of spectroscopically confirmed galaxies at z > 9 in the literature. The red star shows the intrinsic UV magnitude of EGS-25297 after correction for dust attenuation using standard assumptions. The gray data points show the observed values for other spectroscopically confirmed galaxies at z > 9 (P. Arrabal Haro et al. 2023a, 2023b; A. J. Bunker et al. 2023b; E. Curtis-Lake et al. 2023; S. Fujimoto et al. 2023; A. D. Goulding et al. 2023; G. Roberts-Borsani et al. 2023; M. Stiavelli et al. 2023; B. Wang et al. 2023; H. Williams et al. 2023; K. Boyett et al. 2024; S. Carniani et al. 2024; M. Castellano et al. 2024; M. Curti et al. 2024; F. D’Eugenio et al. 2024; K. N. Hainline et al. 2024; T. Y.-Y. Hsiao et al. 2024; D. Schaerer et al. 2024; M. Tang et al. 2024; H. Yanagisawa et al. 2025; V. Kokorev et al. 2025; R. P. Naidu et al. 2025; L. Napolitano et al. 2025a; A. Runnholm et al. 2025; A. J. Taylor et al. 2025; J. Witstok et al. 2025).
Paper: Very Bright, Very Blue, and Very Red: JWST CAPERS Analysis of Highly Luminous Galaxies with Extreme Ultraviolet Slopes at z = 10
Authors: Callum T. Donnan, Mark Dickinson, Anthony J. Taylor, Pablo Arrabal Haro, Steven L. Finkelstein, Thomas M. Stanton, Intae Jung, Casey Papovich, Hollis B. Akins, Anton M. Koekemoer, Derek J. McLeod, Lorenzo Napolitano, Ricardo O. Amorín, Ryan Begley, Denis Burgarella, Adam C. Carnall, Caitlin M. Casey, Antonello Calabrò, Fergus Cullen, James S. Dunlop, Richard S. Ellis, Vital Fernández, Mauro Giavalisco, Michaela Hirschmann, Weida Hu, Garth Illingworth, Jeyhan S. Kartaltepe, Dale D. Kocevski, Vasily Kokorev, Ho-Hin Leung, Ray A. Lucas, Alexa M. Morales, Ross McLure, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Struan Stevenson, Jonathan R. Trump, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: The 2D (top) and 1D (bottom) optimally extracted spectra of the three sources presented in this work, COSMOS-300001 (top), COSMOS-52185 (middle), and EGS-25297 (bottom). The black data points show the photometry for each galaxy. For each spectrum we highlight the positions of common emission lines (dashed gray line) and plot the best-fitting BAGPIPES SED model assuming a constant (red), double power law (DPL; blue), and continuity-bursty nonparametric (purple) star formation history (SFH) prior. We show 3″ × 3″ cutout images in the F150W filter for each source with the NIRSpec slit overlaid (inset).
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Dependence on stellar mass M* of (a) bar strength A2/A0 and (b) bar length Rbar. Green dots and error bars represent the mean values and standard deviations from our bar-forming models. Bars within each group have identical stellar masses; data points are slightly offset along the horizontal axis for clarity. In panel (a), the solid line represents the linear fit to the observational data reported by Y. H. Lee et al. (2022), with dotted lines indicating the ﹩1{\sigma }_{{A}_{2}/{A}_{0}}﹩ and ﹩2{\sigma }_{{A}_{2}/{A}_{0}}﹩ deviations from the mean. In panel (b), the solid line represents the mean bar length for S4G galaxies from P. Erwin (2019), with dotted lines indicating the ﹩1{\sigma }_{{R}_{\,\rm{bar}\,}}﹩ and ﹩2{\sigma }_{{R}_{\,\rm{bar}\,}}﹩ deviations.
Paper: Very Bright, Very Blue, and Very Red: JWST CAPERS Analysis of Highly Luminous Galaxies with Extreme Ultraviolet Slopes at z = 10
Authors: Callum T. Donnan, Mark Dickinson, Anthony J. Taylor, Pablo Arrabal Haro, Steven L. Finkelstein, Thomas M. Stanton, Intae Jung, Casey Papovich, Hollis B. Akins, Anton M. Koekemoer, Derek J. McLeod, Lorenzo Napolitano, Ricardo O. Amorín, Ryan Begley, Denis Burgarella, Adam C. Carnall, Caitlin M. Casey, Antonello Calabrò, Fergus Cullen, James S. Dunlop, Richard S. Ellis, Vital Fernández, Mauro Giavalisco, Michaela Hirschmann, Weida Hu, Garth Illingworth, Jeyhan S. Kartaltepe, Dale D. Kocevski, Vasily Kokorev, Ho-Hin Leung, Ray A. Lucas, Alexa M. Morales, Ross McLure, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Struan Stevenson, Jonathan R. Trump, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: The inferred SFHs from the best-fitting BAGPIPES SED model to COSMOS-52185 (left), COSMOS-300001 (middle), and EGS-25297 (right). We show the inferred SFH assuming three different priors for each galaxy with a constant prior in red, a DPL in blue, and the “continuity-bursty” nonparametric prior (S. Tacchella et al. 2022) in purple.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Bar formation time tbar against the disk mass fraction fdisk in our bar-forming models. The symbols have the same meanings as in Figure 16. The solid line indicates the mean relation proposed by M. S. Fujii et al. (2018), while the dashed lines represent the associated uncertainty bounds (see Equation (18)).
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Relationship between the corotation radius RCR and the bar length Rbar for all bar-forming models in our simulations. The dashed and dotted lines correspond to ﹩{ \mathcal R }\equiv {R}_{\rm{CR}\,}/{R}_{\,\rm{bar}}=1.4﹩ and 1.0, respectively. All bars satisfy ﹩{ \mathcal R }\gt 1.4﹩, indicating that they are classified as slow.
Paper: Very Bright, Very Blue, and Very Red: JWST CAPERS Analysis of Highly Luminous Galaxies with Extreme Ultraviolet Slopes at z = 10
Authors: Callum T. Donnan, Mark Dickinson, Anthony J. Taylor, Pablo Arrabal Haro, Steven L. Finkelstein, Thomas M. Stanton, Intae Jung, Casey Papovich, Hollis B. Akins, Anton M. Koekemoer, Derek J. McLeod, Lorenzo Napolitano, Ricardo O. Amorín, Ryan Begley, Denis Burgarella, Adam C. Carnall, Caitlin M. Casey, Antonello Calabrò, Fergus Cullen, James S. Dunlop, Richard S. Ellis, Vital Fernández, Mauro Giavalisco, Michaela Hirschmann, Weida Hu, Garth Illingworth, Jeyhan S. Kartaltepe, Dale D. Kocevski, Vasily Kokorev, Ho-Hin Leung, Ray A. Lucas, Alexa M. Morales, Ross McLure, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Struan Stevenson, Jonathan R. Trump, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Red–green–blue color images of COSMOS-300001 (left panel, upper-right source) and COSMOS-52185 (left panel, lower-left source) and EGS-25297 (right) using the JWST/NIRCam F150W, F200W, and F444W filters. Each cutout is 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 × 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5. The color images illustrate the blue rest-frame UV colors of the COSMOS pair and the red rest-frame UV color of EGS-25297.
Paper: Conditions for Bar Formation in Bulgeless Disk Galaxies
Authors: Dajeong Jang, Woong-Tae Kim, Yun Hee Lee
Figure caption: Simulation outcomes in the tOP–ϵELN plane. The symbols have the same meanings as in Figure 16. The vertical dashed line marks ϵELN = 1.1 (see Equation (3)).
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Stellar mass vs. redshift relation computed from the pop-cosmos model draws. Red shaded regions show the 68% and 95% conditional credible intervals, with the solid red line showing the median. The gray shaded region and dashed line correspond to the 99.5th percentile of stellar mass at a given redshift. The black shaded region and dashed line show the estimated mode or “turnover” of the stellar mass distribution as a function of redshift. Purple lines show upper limits on the masses of COSMOS2020 galaxies, estimated from the galaxy-level SED fits presented in Section 4.4.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Stellar mass function (normalized, logarithmic axes) predicted by pop-cosmos (solid red histogram), compared to the stellar masses from Bayesian SED fitting (purple) to COSMOS2020 galaxies selected on Ch. 1 < 26 (see Section 4.4). For the pop-cosmos draws, we consider the most massive 0.5% of galaxies at a given redshift (rightmost gray shaded region) to be an extrapolation due to the rarity of such galaxies in a COSMOS-sized field. The histograms are normalized to integrate to one between the vertical shaded regions. In green we plot the double Schechter mass function from J. Leja et al. (2020), normalized within the same limits.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Normalized redshift distribution for (top) r < 25 and (bottom) Ch. 1 < 26. Shaded regions show the fractional effect of cosmic variance that would be expected for a COSMOS-sized field. The purple histogram shows posterior median redshifts for (top) 146,252 and (bottom) 423,262 COSMOS galaxies that pass each selection cut (see Section 4.3).
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Comparison of stellar mass estimates for the 423,262 COSMOS2020 galaxies with Ch. 1 < 26. The vertical axis shows the posterior median ﹩{\mathrm{log}}_{10}(M/{M}_{\odot })﹩ under the new pop-cosmos prior. The horizontal axis shows (left) the LePhare stellar mass estimates from J. R. Weaver et al. (2022), and (right) the posterior median under the Prospector prior.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Distribution of AGN bolometric luminosity fraction fAGN, for galaxies with Ch. 1 < 26. The filled red histogram shows the prior distribution computed from pop-cosmos model draws. The purple dashed histogram shows the posterior medians for 423,262 COSMOS2020 galaxies, with the cyan histogram showing posterior medians for the subset of 1951 COSMOS2020 galaxies with Chandra X-ray detections.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Stellar mass vs. redshift computed from the pop-cosmos model draws for galaxies with 25 < Ch. 1 < 26 and i > 27.6 (3.5% of the Ch. 1 < 26 mock catalog). The mass completeness limit from Figure 8 is shown as a yellow dashed line and hatched region.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Flux uncertainty vs. (logarithmic) magnitude for the COSMOS broad bands, compared to the flux errors reported in the COSMOS2020 catalog (J. R. Weaver et al. 2022) for Ch. 1 < 26. Note that the pop-cosmos uncertainty predictions are made conditional on the pop-cosmos model magnitudes. Contours enclose the 68% and 95% highest probability density regions.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Comparison of zphot vs. zspec based on zphot (posterior median z) inferred under the new pop-cosmos prior. Each galaxy is weighted by its spectroscopic CL from A. A. Khostovan et al. (2025). Solid and dashed lines show zphot = zspec and ∣Δz∣ = 0.15, respectively.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Broadband colors (logarithmic, A24 band combinations) predicted by the new pop-cosmos generative model, compared to COSMOS2020 (J. R. Weaver et al. 2022) for Ch. 1 < 26. Contours enclose the 68% and 95% highest-density regions.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: SFR vs. mass binned by redshift and shaded by (left) model galaxy count, and (right) median AGN bolometric luminosity fraction, fAGN. Cells are shaded only if they contain >10 model galaxies. The black and gray dashed lines show respectively the mass completeness limit and upper mass limit. Solid yellow lines shows the median from Figure 12, and dashed (dashed–dotted) yellow lines show 68% (95%) intervals.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: PCs of the broadband colors of the COSMOS2020 catalog with Ch. 1 < 26, showing (upper panel) the eigenvalues, and (lower panel) the principal eigenvectors. The vertical axis in the upper panel shows the fraction of variance explained by each PC, with the annotation showing the cumulative variance explained by each PC and those leftward of it in the plot. The lower panel shows the contribution of each color to the first six PCs, which cumulatively explain >90% of the variance in COSMOS2020.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Histogram of stellar mass vs. redshift for pop-cosmos with Ch. 1 < 26. Redshift binning is based on percentiles of z, so each vertical slice of the histogram contains 20,000 mock galaxies. Red markers show the redshift binned turnover of the mass function (upward pointing triangles), and the 99.5th percentile in stellar mass (downward pointing triangles). Red dashed lines show the fitting functions of the form ﹩{ \mathcal M }(z)﹩ based on the results in Appendices E.1–E.2.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Quantile-based comparison—(left) Q–Q plots and (right) P–P plots—of the model colors and COSMOS colors projected along the first six principal axes (93% of total variance) identified in Figure 25. At the lower right corners of the Q–Q plots, we show the marginal 2-Wasserstein distance ﹩{{ \mathcal W }}_{2}﹩; at the lower right corner of the P–P plots we show the K-S statistic ﹩{{ \mathcal D }}_{\,\rm{KS}\,}﹩.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Same as row 5 of Figure 19, but showing observer-frame IRAC Ch. 1 − Ch. 2 color vs. redshift.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Effective change in predicted emission line strength for pop-cosmos relative to the line strengths inferred in L23 and A24.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Broadband colors (logarithmic, adjacent bands) predicted by the new pop-cosmos generative model, compared to COSMOS2020 (J. R. Weaver et al. 2022) for r < 25.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Effective change in photometric fluxes in the the 26 COSMOS bands, relative to the corrections inferred in L23 and A24.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Broadband magnitudes (logarithmic) predicted by the new pop-cosmos generative model, compared to COSMOS2020 (J. R. Weaver et al. 2022) for r < 25.
Paper: The Accretion Disk Size Problem in AGN Disk Reverberation Mapping Is an Obscuration Effect: A Uniform AGN Sample Study with Swift
Authors: Collin Lewin, Erin Kara, Christos Panagiotou, Edward M. Cackett, Jonathan Gelbord, Juan V. Hernández Santisteban, Keith Horne, Gerard A. Kriss
Figure caption: Swift X-ray spectra for the AGN in our sample. The sources fall into two broad categories based on their spectral shapes, which reflect varying levels of obscuration. Spectra shown in pink correspond to unobscured sources, as shown by smooth, power-law-like continua with relatively minimal spectral features. In contrast, the green spectra exhibit pronounced curvature, particularly between ∼1 and 4 keV, indicative of higher levels of obscuration from neutral and ionized gas along the line of sight. These visually apparent differences are later formalized using a GMM, whose classifications are consistent with this initial inspection. For detailed inspection, per-source spectra are shown in the Appendix (Figure 9).
Paper: The Accretion Disk Size Problem in AGN Disk Reverberation Mapping Is an Obscuration Effect: A Uniform AGN Sample Study with Swift
Authors: Collin Lewin, Erin Kara, Christos Panagiotou, Edward M. Cackett, Jonathan Gelbord, Juan V. Hernández Santisteban, Keith Horne, Gerard A. Kriss
Figure caption: The two Gaussian components of the GMM, corresponding to the obscured and unobscured subgroups. Each distribution was fit by maximizing the likelihood of the observed column density and hardness ratio values, incorporating measurement uncertainties via a Monte Carlo approach. Covariance between the variables is accounted for, producing tilted ellipses, most notable in the obscured subgroup. The overlap between the two components is minimal, resulting in very high cluster assignment probabilities (>99%) for all sources.
Paper: Simulating Propagation of a Coronal Mass Ejection from Solar Corona to 1 au with the Alfvén Wave Solar Atmosphere Model and Fitting of Gibson–Low
Authors: Xinghua Dai
Figure caption: Simulation of ICME in IH domain at 07:39 UT on 2011 March 9, 35 hr after the CME insertion. Top row: plasma velocity. Second row: proton density. Third row: proton temperature. Bottom row: magnetic field. Left column: solar equatorial view (xy plane) at 07:39 UT. Middle column: solar meridional view (xz plane) at 07:39 UT. Right column: simulations (red lines) and in situ measurements from STA (black lines) of the ICME, where the time at 07:39 UT is marked by four vertical dashed red lines.
Paper: Simulating Propagation of a Coronal Mass Ejection from Solar Corona to 1 au with the Alfvén Wave Solar Atmosphere Model and Fitting of Gibson–Low
Authors: Xinghua Dai
Figure caption: Simulation of ICME in IH domain at 11:39 UT on 2011 March 8, 15 hr after the CME insertion. Top row: plasma velocity. Second row: proton density. Third row: proton temperature. Bottom row: magnetic field. Left column: solar equatorial view (xy plane) at 11:39 UT. Middle column: solar meridional view (xz plane) at 11:39 UT. Right column: simulations (red lines) and in situ measurements from STA (black lines) of the ICME, where the time at 11:39 UT is marked by four vertical dashed red lines.
Paper: Simulating Propagation of a Coronal Mass Ejection from Solar Corona to 1 au with the Alfvén Wave Solar Atmosphere Model and Fitting of Gibson–Low
Authors: Xinghua Dai
Figure caption: Simulation of solar wind of CR2107 in IH domain. Top row: plasma velocity; Second row: proton density; Third row: proton temperature. Bottom row: magnetic field. Left column: solar equatorial view (xy plane) at 20:30 UT on 2011 March 7. Middle column: solar meridional view (xz plane) at 20:30 UT. Right column: simulations (red lines) and in situ measurements from STA (black lines) of the complete CR2107, where the time at 20:30 UT is marked by four vertical dashed red lines. Locations of the Sun and STA are labeled in the left and middle columns.
Paper: Simulating Propagation of a Coronal Mass Ejection from Solar Corona to 1 au with the Alfvén Wave Solar Atmosphere Model and Fitting of Gibson–Low
Authors: Xinghua Dai
Figure caption: Top row: GONG synoptic magnetogram of CR2107; Middle row: synthesized EUV images of SDO/AIA (211 Å), STA/EUVI (195 Å), and STB/EUVI (284 Å). Bottom row: observed EUV images of SDO/AIA (211 Å) at 20:38, STA/EUVI (195 Å) at 20:35, and STB/EUVI (284 Å) at 20:36 on 2011 March 07. The NOAA numbers of active regions are marked on these images, and a coronal hole is also labeled by CH on the 195 Å images.
Paper: Simulating Propagation of a Coronal Mass Ejection from Solar Corona to 1 au with the Alfvén Wave Solar Atmosphere Model and Fitting of Gibson–Low
Authors: Xinghua Dai
Figure caption: Self-similar velocity (top row), magnetic field (second row), plasma density (third row), and plasma pressure (bottom row) of the reconstructed CME on planes of ﹩y^{\prime} {z}^{{\prime} }﹩ (left column), ﹩y^{\prime} {x}^{{\prime} }﹩ (middle column), and ﹩z^{\prime} {x}^{{\prime} }﹩ (right column).
Paper: Simulating Propagation of a Coronal Mass Ejection from Solar Corona to 1 au with the Alfvén Wave Solar Atmosphere Model and Fitting of Gibson–Low
Authors: Xinghua Dai
Figure caption: Simulation (red lines) and in situ measurements from STA (black lines) of plasma velocity (left column) and magnetic field (right column) of the complete CR2107. Top row: total values. Second row: radial components. Third row: tangent components. Bottom row: normal components.