adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Loci. IX. Estimation of Stellar Parameters from CSST-like Photometry
Authors: Xue Lu, Haibo Yuan, Kai Xiao, Bowen Huang, Ruoyi Zhang, Lin Yang, Timothy C. Beers, Shuai Xu
Figure caption: Stellar loci of theoretical CSST colors, color coded by [M/H] and log g shown in the color bars to the right of the upper and lower rows of panels, respectively.
Paper: A Late-time Radio Survey of Type Ia-CSM Supernovae with the Very Large Array
Authors: Olivia Griffith, Grace Showerman, Sumit K. Sarbadhicary, Chelsea E. Harris, Laura Chomiuk, Jesper Sollerman, Peter Lundqvist, Javier Moldón, Miguel Pérez- Torres, Erik C. Kool, Takashi J. Moriya
Figure caption: Predicted 6 GHz radio light curves for SNe Ia-CSM, shown alongside radio observations in this paper and from the literature. Solid curves correspond to the case of Twind = 2.0 × 104 K, and dashed curves to Twind = 105 K. The left panel shows the case of ϵB = 0.1, and the right panel shows ϵB = 0.01 (both panels assume ϵe = 0.1). Light curves span a range of ﹩\dot{M}/{v}_{\mathrm{wind}}﹩ from 3 × 10−5 M⊙ yr−1 (dark blue lines) to 0.1 M⊙ yr−1 (yellow lines), assuming vwind = 100 km s−1. The shaded gray region represents SNe Ia < 1 yr, which are excluded in this study. SNe with 3σ upper limits are plotted as inverted black triangles. The radio detections of SN 2022esa from 2023 to 2024 are shown as red circles connected by a dashed line. Literature measurements of SN 2020eyj from E. C. Kool et al. (2023) and X. Yang et al. (2023) (scaled to 6 GHz) are shown as orange points.
Paper: A Late-time Radio Survey of Type Ia-CSM Supernovae with the Very Large Array
Authors: Olivia Griffith, Grace Showerman, Sumit K. Sarbadhicary, Chelsea E. Harris, Laura Chomiuk, Jesper Sollerman, Peter Lundqvist, Javier Moldón, Miguel Pérez- Torres, Erik C. Kool, Takashi J. Moriya
Figure caption: 6 GHz light curves produced by interaction with shell-like CSM, compared with our radio observations of SNe Ia-CSM. The light curves accounting for absorption are solid, whereas the ones with no absorption are dashed. The left panel shows models for ϵB = 0.1, and the right panel for ϵB = 0.01 (both panels use ϵe = 0.1). Each light curve’s color is specific to the density and mass of the shell, with the dark purple color representing ρcsm = 10−20 g cm−3 and Mshell = 0.147 M⊙, teal corresponding to ρcsm = 10−19 g cm−3 and Mshell = 1.47 M⊙, and yellow depicting ρcsm = 10−18 g cm−3 and Mshell = 14.7 M⊙. We assume Rin = 1017 cm and fR = 1 for this model (see Section 5).
Paper: A Late-time Radio Survey of Type Ia-CSM Supernovae with the Very Large Array
Authors: Olivia Griffith, Grace Showerman, Sumit K. Sarbadhicary, Chelsea E. Harris, Laura Chomiuk, Jesper Sollerman, Peter Lundqvist, Javier Moldón, Miguel Pérez- Torres, Erik C. Kool, Takashi J. Moriya
Figure caption: The range of mass-loss rates ruled out by the radio upper limits for each SN. For each SN, we show ranges for the three models in Table 2 for the parameters ϵB and Twind. See Section 4 for details.
Paper: A Late-time Radio Survey of Type Ia-CSM Supernovae with the Very Large Array
Authors: Olivia Griffith, Grace Showerman, Sumit K. Sarbadhicary, Chelsea E. Harris, Laura Chomiuk, Jesper Sollerman, Peter Lundqvist, Javier Moldón, Miguel Pérez- Torres, Erik C. Kool, Takashi J. Moriya
Figure caption: Illustration of how we use radio upper limits to constrain the range of ruled-out mass-loss rates ﹩\dot{M}/{v}_{\mathrm{wind}}﹩ (green shade). Each light curve (green solid) shows the predicted luminosity for different mass-loss rates at a given SN age (30 days, 1 yr, and 10 yr). The range of mass-loss rates where the predicted luminosity exceeds the measured upper limit (dashed line) are ruled out. Due to the light-curve shape for windlike CSM, later-time observations are more effective at ruling out a greater (and higher) range of mass-loss rates.
Paper: A Late-time Radio Survey of Type Ia-CSM Supernovae with the Very Large Array
Authors: Olivia Griffith, Grace Showerman, Sumit K. Sarbadhicary, Chelsea E. Harris, Laura Chomiuk, Jesper Sollerman, Peter Lundqvist, Javier Moldón, Miguel Pérez- Torres, Erik C. Kool, Takashi J. Moriya
Figure caption: Comparison of light curves produced by the different models. The solid lines make use of the dynamics from TC17, while the dashed lines represent the models of L. Chomiuk et al. (2016), which do not include the transition to the ST phase. The left panel shows models for ϵB = 0.1, and the right panel for ϵB = 0.01. Different color lines represent different values of ﹩\dot{M}/{v}_{\mathrm{wind}}﹩, according to the color bar at right.
Paper: A Late-time Radio Survey of Type Ia-CSM Supernovae with the Very Large Array
Authors: Olivia Griffith, Grace Showerman, Sumit K. Sarbadhicary, Chelsea E. Harris, Laura Chomiuk, Jesper Sollerman, Peter Lundqvist, Javier Moldón, Miguel Pérez- Torres, Erik C. Kool, Takashi J. Moriya
Figure caption: Comparing the TC17 model (green) with the older, ED light-curve models (blue). Each panel represents the parameter value combinations from Table 2. See the Appendix for details. This figure does not include data for SN 2022esa.
Paper: A Late-time Radio Survey of Type Ia-CSM Supernovae with the Very Large Array
Authors: Olivia Griffith, Grace Showerman, Sumit K. Sarbadhicary, Chelsea E. Harris, Laura Chomiuk, Jesper Sollerman, Peter Lundqvist, Javier Moldón, Miguel Pérez- Torres, Erik C. Kool, Takashi J. Moriya
Figure caption: The time evolution of the forward shock radius (left panel) and velocity (right panel) from the TC17 model (Section 3.2) for the case of E51 = 1.0, Mej = 1.44 M⊙, and ﹩\dot{M}/{v}_{\mathrm{wind}}﹩ = 0.1 M⊙ yr−1 (100 km s−1)−1. The vertical blue shaded section represents the time range at which our radio observations were obtained. Dashed lines represent the asymptotic solutions for the ED (n = 10 density profile) and ST cases.
Paper: Thermonuclear X-Ray Bursts of 4U 0614+09: The Evidence for the Retreat of the Disk away from the Neutron Star
Authors: Yu-Peng Chen, Long Ji, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Persistent spectrum of 4U 0614+09 as observed from NICER. The best-fitting model consists of an absorbed convolution thermal-Comptonization model (with an input seed photon spectrum of the accretion disk and NS surface emission), i.e., vphabs*thcomp*(diskbb+bboday).
Paper: Thermonuclear X-Ray Bursts of 4U 0614+09: The Evidence for the Retreat of the Disk away from the Neutron Star
Authors: Yu-Peng Chen, Long Ji, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Lightcurves of the first X-ray burst detected in the NICER observation of 4U 0614+09 with time bin 0.5 s (left) and 0.01 s (right) in the NICER full energy band.
Paper: Thermonuclear X-Ray Bursts of 4U 0614+09: The Evidence for the Retreat of the Disk away from the Neutron Star
Authors: Yu-Peng Chen, Long Ji, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: The bolometric flux relation between the persistent emission (including the disk and the corona emission) Ftotal and the inner disk radius Rdisk of 4U 0614+09 based on NICER observations. The yellow stars represent the two bursts detected by NICER.
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: Distribution of r-band apparent magnitude (ro, top) and stellar mass (﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })﹩, bottom) as a function of spectroscopic redshift (zspec) for SAGA Gold satellites (purple, circles), SAGAbg environmentally averaged galaxies (orange, triangles), and SDSS/NSA isolated galaxies (green, stars). Luminosity distance is shown for reference as the upper x-axis. The black dashed and dotted–dashed lines in both panels represent magnitude limits of ro = 20.7 and ro = 17.77, indicating approximate spectroscopic limits for the SAGA and SDSS surveys, respectively. The vertical dotted lines highlight the redshift criteria for the SAGAbg and SDSS/NSA isolated samples. We employ a redshift cutoff of z < 0.025 for the SAGAbg sample (orange dotted line) and z < 0.01 for SDSS/NSA isolated galaxies (green dotted line). These redshift ranges are selected such that the samples are stellar mass matched to our SAGA satellite sample (above ﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })=7.5﹩).
Paper: Thermonuclear X-Ray Bursts of 4U 0614+09: The Evidence for the Retreat of the Disk away from the Neutron Star
Authors: Yu-Peng Chen, Long Ji, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: The spectral fitting results of the burst using the variable persistent flux model (red; left panel) and convolution thermal-Comptonization model (red; right panel), and using a pure blackbody model (black) at the burst tail phase. This includes the time evolution of the blackbody bolometric flux Fbb, the temperature kTbb, the observed radius R of the NS surface at 3 kpc fa, the inner disk radius Rdisk, and the goodness of fit ﹩{\chi }_{v}^{2}﹩. The bolometric flux of the blackbody model Fbb is in units of 10−8 erg cm–2 s−1. The black data indicate the fitting results by the absorbed blackbody model at the burst tail. The blue data points indicate the fitting results of the time evolution of Fbb at the decay phase using the revised power-law function, i.e., ﹩{F}_{{\rm{bb}}}={F}_{{\rm{0}}}{t}^{\alpha }-{F}_{{\rm{pre}}}﹩.
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: Half-light size (Rr,eff, top), ellipticity (e, middle), and Sérsic index (n, bottom) distributions of SAGA satellites. Left panels show the binned medians as a function of stellar mass, with shaded regions indicating the 16th–84th percentile ranges. Right panels show the normalized distributions for satellites in the mass range of ﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })\gt 7.5﹩. Gaussian KDE density functions are included to illustrate the overall shape of each distribution. In all panels, distributions show the completeness-corrected satellite population, split by star-forming (SAGA SF, blue) and quenched satellites (SAGA Q, maroon).
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: The size–mass relation for SAGA satellite galaxies. Star-forming (blue circles) and quenched (maroon squares) populations are both shown and fit independently. Open symbols correspond to unconfirmed candidates with a high probability of being satellites (psat > 0.5), with open blue circles and maroon squares indicating predicted star-forming and quenched candidates, respectively. Vertical dashed lines indicate the SAGA Silver (﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })=6.75﹩) and SAGA Gold (﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })=7.5﹩) mass thresholds. The black line shows our completeness-corrected size–mass relation for all SAGA satellites above ﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })=7.5﹩, and the relations for star-forming and quenched satellites are shown by the blue dashed and maroon dotted–dashed lines, respectively.
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: Stellar mass distributions for the observed and completeness-corrected samples of SAGA satellites (first panel, purple), SAGAbg galaxies (second panel, orange), and SDSS/NSA isolated galaxies (third panel, green). The hatched histograms represent the observed (uncorrected) distributions, while the solid filled histograms show the completeness-corrected distributions. Dotted lines indicate Gaussian KDEs for the observed distributions, and solid lines indicate KDEs for the completeness-corrected distributions. Given the large completeness correction required for the SDSS/NSA sample, we verify in Section 4.5 that incompleteness cannot fully account for our results.
Paper: The SAGA Survey. VI. The Size–Mass Relation for Low-mass Galaxies Across Environments
Authors: Yasmeen Asali, Marla Geha, Erin Kado-Fong, Yao-Yuan Mao, Risa H. Wechsler, Mithi A. C. de los Reyes, Imad Pasha, Nitya Kallivayalil, Ethan O. Nadler, Erik J. Tollerud, Yunchong Wang, Benjamin Weiner, John F. Wu
Figure caption: Example galaxy in Legacy Survey imaging. The axes in each panel correspond to physical distances in kiloparsecs relative to the center of the galaxy. First panel: optical color image (g, r, and z bands) with Sérsic model ellipses corresponding to Reff, R80, and 3 × Reff. Second panel: masked r-band image. Third panel: best-fit pysersic model to r-band image. Fourth panel: residual between the pysersic model image and the r-band image.
Paper: Thermonuclear X-Ray Bursts of 4U 0614+09: The Evidence for the Retreat of the Disk away from the Neutron Star
Authors: Yu-Peng Chen, Long Ji, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Spectral fits to burst peak (left panel: fitted with the variable persistent flux model—vpabs*(bb+fa*persistent); right panel: fitted with the convolution thermal-Comptonization model with variable inner disk radius—vpabs*thcomp*(bbody+diskbb).
Paper: Thermonuclear X-Ray Bursts of 4U 0614+09: The Evidence for the Retreat of the Disk away from the Neutron Star
Authors: Yu-Peng Chen, Long Ji, Shu Zhang, Shuang-Nan Zhang, Hua Feng, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Burst flux (in units of 10−8 erg cm–2 s−1) versus the value of fa. The two flux values normalized to the Eddington luminosity, i.e., γbb and γfa, are also labeled. The red line represents the fit with ﹩{f}_{a}\propto {F}_{{\rm{bb}}}^{1/2}﹩.
Paper: Hot, Cold, and Multicomponent Accretion Flows around Supermassive Black Hole Binaries
Authors: Christopher Tiede, Daniel J. D'Orazio
Figure caption: Same as Figure 6, but for a reference period of 10 days. Systems in the gray region are disallowed because they would have merged.
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: Distribution of the effective radius of bulge (Re_bulge) and disk (Re_disk) across F150W, F200W, F277W, F356W, F410M, and F444W, with the red and dark blue dotted vertical lines indicating the median of the effective radius of the bulge and the disk, respectively.
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: Gini–M20 relation for both the SMGs and the field galaxies in the PRIMER-COSMOS field, with the dashed line indicating the boundary of the galaxies with merger signatures and those nonmergers, with a detailed description in J. M. Lotz et al. (2008).
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: Simple assumptive sketch based on previous studies summarizing the bulge formations in submillimeter galaxies presented in this paper, in which the classical bulge and ellipticals (kinematically hot, high B/T, high Sérsic) are the products of mergers whereas the pseodobulges and the bulgeless galaxies (kinematically cold, low B/T, low Sérsic) are fabricated by degrees in the secular evolution.
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: The distribution of different types of bulges based on the classification scheme using the Sérsic index and bulge-to-total luminosity ratio on band F277W after the removal of the strongly disturbed SMGs, with the big star symbols showing the median of each group.
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: Example of SMGs with different bulge types (165″ × 165″), including merger-built bulge, clump-sinking bulge, pseudobulge, and unclassified bulge, with the white horizontal line in each individual plot standing for the scale of 1″ (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩03 pixel−1).
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: The distribution of the bulge Sérsic index across six bands (F150W, F200W, F277W, F356W, F410M, and F444W), divided by three B/T bins (B/T < 0.2, 0.2 < B/T < 0.5, and B/T > 0.5).
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: Photometric redshift vs. stellar mass for 125 selected SMGs (orange), and the field sample (gray) in the PRIMER-COSMOS field.
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: An example of bar identification via ellipse isophotal fitting of source ID: 614294 via ellipse-fitting techniques as an example. The blue cross marks the shared center of isophotes (red).
Paper: Disclosing Submillimeter Galaxy Formation: Mergers or Secular Evolution?
Authors: Siu-Wang Chan, 瀟弘 陳, Yiping Ao, Qing-hua Tan
Figure caption: The distribution of bulge Sérsic indices across three B/T bins (B/T < 0.2, 0.2 ≤ B/T ≤ 0.5, B/T > 0.5) in band F200W.
Paper: The Shape of the Solar Tachocline
Authors: Sarbani Basu, Sylvain G. Korzennik
Figure caption: The position of the tachocline plotted as a function of latitude for all the datasets. The solid gray horizontal line shows the position of the convection-zone base, with the gray dotted lines showing the 1σ uncertainty. Panel (a) shows the results for the 32 × 72-day sets, while panel (b) shows the results for the 64 × 72-day sets. In each panel the solid lines show the results for the three-term case, while the dotted–dashed lines are the results when using the two-term latitudinal model. Note how they agree at low latitudes. We show the 1σ error limit only for the GONG Set 1 and the HMI (Project) results for the sake of clarity. These are marked as dotted lines for the two-term case and dashed lines for the three-term one. The uncertainties are similar for the three other datasets obtained with the SGK pipeline. It should be noted that the results close to the pole are essentially an extrapolation, since the data do not have sensitivity there. Also note that the results from the HMI project’s pipeline and the SGK pipeline agree well within 1σ uncertainties.
Paper: The Shape of the Solar Tachocline
Authors: Sarbani Basu, Sylvain G. Korzennik
Figure caption: As in Figure 5 we show the position of the tachocline obtained by fitting the 1D model as points with error bars; the fit is to the HMI 64 × 72-day set. The red dotted–dashed line is the result of the two-term 2D fit; 1σ uncertainties are shown as the red dotted line. The blue solid line is the result of the three-term 2D fit, with the blue dashed line marking 1σ uncertainties. The new, four-term 2D fit is shown with large black dashes, with the large-dashed–dotted black lines marking the 1σ uncertainties.
Paper: The Shape of the Solar Tachocline
Authors: Sarbani Basu, Sylvain G. Korzennik
Figure caption: Top: a sigmoid fitted to the c3 splitting coefficient for the HMI 64 × 72-day set. Bottom: a sigmoid fitted to the c5 splitting coefficient of the same set. The background cyan points with error bars are the observed coefficients plotted as a function of their lower turning point. The red points show the coefficients resulting from our best-fit sigmoid model. The c5 component of the 32 × 72-day sets can also be fitted with a sigmoid. This splitting coefficient is very noisy in shorter sets.
Paper: The Shape of the Solar Tachocline
Authors: Sarbani Basu, Sylvain G. Korzennik
Figure caption: The position of the tachocline obtained by fitting the 1D model shown in Equation (7) to the HMI 64 × 72-day set is plotted as points with 1σ error bars; the points below and above 25° have been connected separately with a dotted line to guide the eye. The red dotted–dashed line is the result of the two-term 2D fit; 1σ uncertainties are shown as the red dotted line. The blue solid line is the result of the three-term 2D fit, with the blue dashed line marking 1σ uncertainties.
Paper: The Shape of the Solar Tachocline
Authors: Sarbani Basu, Sylvain G. Korzennik
Figure caption: Plot showing the position of the tachocline obtained with the HMI 64 × 72-day dataset. The red curve is the result from the two-term fit, the blue curve is that from the three-term fit, and the black is from the four-term fit. Dotted lines of the corresponding colors show 1σ uncertainties. The points with error bars are results of the 1D fits. The position of the convection-zone base is shown in gray.
Paper: The Shape of the Solar Tachocline
Authors: Sarbani Basu, Sylvain G. Korzennik
Figure caption: The extent of the tachocline, defined as the region between rd − wd and rd + wd, as obtained with the HMI 64 × 72-day set. The region between the red dotted–dashed lines shows the result of the two-term case, with the dotted lines indicating 1σ uncertainties. The region between the blue solid lines shows the results of the three-term case, with the dashed lines showing 1σ uncertainties.
Paper: Radiation Hydrodynamics of Self-gravitating Protoplanetary Disks. I. Direct Formation of Gas Giants via Disk Fragmentation
Authors: Yang Ni, 阳 倪, Hongping Deng, 洪 平 邓, Xue-Ning Bai, 雪 宁 白
Figure caption: Temporal evolution of the clump mass mclump (left column) and virial parameter αvir (right column) in m15k1, m17k1, m20k1, m17k5, and m20k5. Labels in the upper left of all rows indicate the names of the five simulation runs. Each line demonstrates the evolution of an individual clump. Solid lines represent the fragments among all the clumps, and dotted lines represent all other clumps.
Paper: Radiation Hydrodynamics of Self-gravitating Protoplanetary Disks. I. Direct Formation of Gas Giants via Disk Fragmentation
Authors: Yang Ni, 阳 倪, Hongping Deng, 洪 平 邓, Xue-Ning Bai, 雪 宁 白
Figure caption: Two examples of clumps undergoing disruption or collapse following collisions with spiral arms, taken from simulation m17k5, are shown in the top and bottom rows of panels, respectively. Each row presents a time sequence of midplane density slices centered on the clump’s center of mass at different epochs. Streamlines are overplotted in the local Keplerian orbital frame to illustrate the gas motion relative to the background flow. Each slice spans a physical size of 15 au × 15 au.