adsabs/AstroCLIMB huggingface dataset:
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The comparison between the total percentage of foreign ejecta delivered from main source craters without impact gardening and with the impact gardening of (a) 3.0 Gyr, (b) 2.8 Gyr, (c) 2.6 Gyr, and (d) 2.4 Gyr, respectively, within the top 1 m layer at the CE-6 landing site by one run.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The comparison of our generated craters with observations and production function on mare surface ages of (a) 3.0 Gyr, (b) 2.8 Gyr, (c) 2.6 Gyr, and (d) 2.4 Gyr. The CSFDs of our generated on-grid primary craters, secondary craters, and the combination with uncertainties of 1σ are shown by blue circles, gray triangles, and red diamonds, respectively. The observed crater density distribution within a 1 km circle across the CE-6 landing site (green squares) is derived from Figure C8, and the CSFDs of lunar crater production function (dashed lines) are derived from NPF2001.
Paper: Composition and Provenance of the Chang′e-6 Lunar Samples: Insights from the Simulation of the Impact Gardening Process
Authors: Yanze Su, Luyuan Xu, Meng-Hua Zhu, Xing-Li Cui
Figure caption: The percentage of the foreign materials within the different sampling depths and at different model start times. The final abundances of foreign distal ejecta after 3.0, 2.8, 2.6, and 2.4 Gyr of impact gardening and the averaged percentages of corresponding groups are shown by the blue diamonds, purple circles, red triangles, green squares, and yellow pentagons, respectively, in four groups, corresponding to the sampling depths of 0.5, 1.0, 1.5, and 2.0 m, respectively. The solid vertical lines display the uncertainties of 1σ.
Paper: Triggering the Untriggered: The First Einstein Probe-detected Gamma-Ray Burst 240219A and Its Implications
Authors: Yi-Han Iris Yin, Bin-Bin Zhang, Jun Yang, Hui Sun, Chen Zhang, Yi-Xuan Shao, You-Dong Hu, Zi-Pei Zhu, Dong Xu, Li An, He Gao, Xue-Feng Wu, Bing Zhang, Alberto Javier Castro-Tirado, Shashi B. Pandey, Arne Rau, Weihua Lei, Wei Xie, Giancarlo Ghirlanda, Luigi Piro, Paul O'Brien, Eleonora Troja, Peter Jonker, Yun-Wei Yu, Jie An, Run-Chao Chen, Yi-Jing Chen, Xiao-Fei Dong, Rob Eyles-Ferris, Zhou Fan, Shao-Yu Fu, Johan P. U. Fynbo, Xing Gao, Yong-Feng Huang, Shuai-Qing Jiang, Ya-Hui Jiang, Yashaswi Julakanti, Erik Kuulkers, Qing-Hui Lao, Dongyue Li, Zhi-Xing Ling, Xing Liu, Yuan Liu, Jia-Yu Mou, Xin Pan, Varun, Daming Wei, Qinyu Wu, Muskan Yadav, Yu-Han Yang, Weimin Yuan, Shuang-Nan Zhang
Figure caption: Multiwavelength observations of EP240219a/GRB 240219A. Each wavelength is represented by different colored dots, lines, and blocks. The small dots indicate follow-up observations with candidates, while the lines denote the observing times; lines for follow-up observations are artificially thickened for clarity. The telescopes corresponding to each wavelength are listed in the same row. The top panels display EP source observation, with the EP/WXT position marked with a light blue circle and the Swift/BAT position marked with a white circle and afterglow detections of Candidate 3 with upper limits. An unconstrained afterglow model (with a typical parameter set of E k,iso = 9.85 × 1053 erg, θ v = 8.99 × 10−2 rad, θ c = 2.65 × 10−2 rad, n = 2.69 × 10−2 cm−3, p = 2.94, ϵ e = 0.13, ϵ B = 4.11 × 10−2, v = 0.28 mag, z = 1.5) is adopted for illustration purposes.
Paper: Triggering the Untriggered: The First Einstein Probe-detected Gamma-Ray Burst 240219A and Its Implications
Authors: Yi-Han Iris Yin, Bin-Bin Zhang, Jun Yang, Hui Sun, Chen Zhang, Yi-Xuan Shao, You-Dong Hu, Zi-Pei Zhu, Dong Xu, Li An, He Gao, Xue-Feng Wu, Bing Zhang, Alberto Javier Castro-Tirado, Shashi B. Pandey, Arne Rau, Weihua Lei, Wei Xie, Giancarlo Ghirlanda, Luigi Piro, Paul O'Brien, Eleonora Troja, Peter Jonker, Yun-Wei Yu, Jie An, Run-Chao Chen, Yi-Jing Chen, Xiao-Fei Dong, Rob Eyles-Ferris, Zhou Fan, Shao-Yu Fu, Johan P. U. Fynbo, Xing Gao, Yong-Feng Huang, Shuai-Qing Jiang, Ya-Hui Jiang, Yashaswi Julakanti, Erik Kuulkers, Qing-Hui Lao, Dongyue Li, Zhi-Xing Ling, Xing Liu, Yuan Liu, Jia-Yu Mou, Xin Pan, Varun, Daming Wei, Qinyu Wu, Muskan Yadav, Yu-Han Yang, Weimin Yuan, Shuang-Nan Zhang
Figure caption: Light curves of GRB 240219A as observed by Insight-HXMT/HE, Swift/BAT, Fermi/GBM, and EP/WXT. The top two panels show the light curve of Insight-HXMT/HE in the energy range of 100–1000 keV and Swift/BAT in the energy range of 14–195 keV with a bin size of 10 s. The third panel illustrates the light curve of Fermi/GBM in the energy range of 10–1000 keV, while the bottom panel displays the light curve of EP/WXT in the energy range of 0.5–4.0 keV. The bin size for Fermi/GBM and EP/WXT light curves is uniformly set to 4 s. The blue dashed vertical lines represent the T 90 interval, and the gray dashed vertical lines denote the T 100. All error bars mark the 1σ confidence level.
Paper: Triggering the Untriggered: The First Einstein Probe-detected Gamma-Ray Burst 240219A and Its Implications
Authors: Yi-Han Iris Yin, Bin-Bin Zhang, Jun Yang, Hui Sun, Chen Zhang, Yi-Xuan Shao, You-Dong Hu, Zi-Pei Zhu, Dong Xu, Li An, He Gao, Xue-Feng Wu, Bing Zhang, Alberto Javier Castro-Tirado, Shashi B. Pandey, Arne Rau, Weihua Lei, Wei Xie, Giancarlo Ghirlanda, Luigi Piro, Paul O'Brien, Eleonora Troja, Peter Jonker, Yun-Wei Yu, Jie An, Run-Chao Chen, Yi-Jing Chen, Xiao-Fei Dong, Rob Eyles-Ferris, Zhou Fan, Shao-Yu Fu, Johan P. U. Fynbo, Xing Gao, Yong-Feng Huang, Shuai-Qing Jiang, Ya-Hui Jiang, Yashaswi Julakanti, Erik Kuulkers, Qing-Hui Lao, Dongyue Li, Zhi-Xing Ling, Xing Liu, Yuan Liu, Jia-Yu Mou, Xin Pan, Varun, Daming Wei, Qinyu Wu, Muskan Yadav, Yu-Han Yang, Weimin Yuan, Shuang-Nan Zhang
Figure caption: Calculation of the Poynting luminosity and baryonic luminosity ratio σ. The time-integrated spectrum of GRB 240219A is represented by the black solid curve. Colored dashed curves indicate synthetic blackbody components. Semitransparent thick curves denote components when σ values are zero, while thin curves represent components with the lower limit value of σ, beyond which photosphere emission is not detectable. Colored solid curves show the hybrid model combining the CPL component (black solid line) and blackbody components (colored dashed lines) with the lower limit value of σ. The fireball base radius, R 0, is assumed to be three different values: 108, 1010, and 1012 cm, marked in purple, red, and yellow, respectively. The derived lower limit values of σ for these radii are 7, 60, and 44, respectively.
Paper: Triggering the Untriggered: The First Einstein Probe-detected Gamma-Ray Burst 240219A and Its Implications
Authors: Yi-Han Iris Yin, Bin-Bin Zhang, Jun Yang, Hui Sun, Chen Zhang, Yi-Xuan Shao, You-Dong Hu, Zi-Pei Zhu, Dong Xu, Li An, He Gao, Xue-Feng Wu, Bing Zhang, Alberto Javier Castro-Tirado, Shashi B. Pandey, Arne Rau, Weihua Lei, Wei Xie, Giancarlo Ghirlanda, Luigi Piro, Paul O'Brien, Eleonora Troja, Peter Jonker, Yun-Wei Yu, Jie An, Run-Chao Chen, Yi-Jing Chen, Xiao-Fei Dong, Rob Eyles-Ferris, Zhou Fan, Shao-Yu Fu, Johan P. U. Fynbo, Xing Gao, Yong-Feng Huang, Shuai-Qing Jiang, Ya-Hui Jiang, Yashaswi Julakanti, Erik Kuulkers, Qing-Hui Lao, Dongyue Li, Zhi-Xing Ling, Xing Liu, Yuan Liu, Jia-Yu Mou, Xin Pan, Varun, Daming Wei, Qinyu Wu, Muskan Yadav, Yu-Han Yang, Weimin Yuan, Shuang-Nan Zhang
Figure caption: SEDs and their evolution. The left panels present SEDs derived from independent spectral fittings at different time intervals. Solid lines show the best-fit unabsorbed model for each independent fit. The right panels illustrate SEDs obtained from joint spectral fittings using an absorbed single CPL model at different time intervals. The unabsorbed CPL model is presented. Error bars represent the 1σ confidence level.
Paper: Triggering the Untriggered: The First Einstein Probe-detected Gamma-Ray Burst 240219A and Its Implications
Authors: Yi-Han Iris Yin, Bin-Bin Zhang, Jun Yang, Hui Sun, Chen Zhang, Yi-Xuan Shao, You-Dong Hu, Zi-Pei Zhu, Dong Xu, Li An, He Gao, Xue-Feng Wu, Bing Zhang, Alberto Javier Castro-Tirado, Shashi B. Pandey, Arne Rau, Weihua Lei, Wei Xie, Giancarlo Ghirlanda, Luigi Piro, Paul O'Brien, Eleonora Troja, Peter Jonker, Yun-Wei Yu, Jie An, Run-Chao Chen, Yi-Jing Chen, Xiao-Fei Dong, Rob Eyles-Ferris, Zhou Fan, Shao-Yu Fu, Johan P. U. Fynbo, Xing Gao, Yong-Feng Huang, Shuai-Qing Jiang, Ya-Hui Jiang, Yashaswi Julakanti, Erik Kuulkers, Qing-Hui Lao, Dongyue Li, Zhi-Xing Ling, Xing Liu, Yuan Liu, Jia-Yu Mou, Xin Pan, Varun, Daming Wei, Qinyu Wu, Muskan Yadav, Yu-Han Yang, Weimin Yuan, Shuang-Nan Zhang
Figure caption: Fluence ratio distribution in the parameter space of the CPL model. The x- and y-axes represent the photon index and peak energy from the CPL model, respectively, with a color gradient indicating the corresponding fluence ratio. Solid curves delineate boundaries for fluence ratio subclassification criteria (S(25–50 keV)/S(50–100 keV)), while dashed horizontal lines indicate peak energy criteria. The location of GRB 240219A is marked with an orange star, with the error bar representing 1σ confidence level.
Paper: Triggering the Untriggered: The First Einstein Probe-detected Gamma-Ray Burst 240219A and Its Implications
Authors: Yi-Han Iris Yin, Bin-Bin Zhang, Jun Yang, Hui Sun, Chen Zhang, Yi-Xuan Shao, You-Dong Hu, Zi-Pei Zhu, Dong Xu, Li An, He Gao, Xue-Feng Wu, Bing Zhang, Alberto Javier Castro-Tirado, Shashi B. Pandey, Arne Rau, Weihua Lei, Wei Xie, Giancarlo Ghirlanda, Luigi Piro, Paul O'Brien, Eleonora Troja, Peter Jonker, Yun-Wei Yu, Jie An, Run-Chao Chen, Yi-Jing Chen, Xiao-Fei Dong, Rob Eyles-Ferris, Zhou Fan, Shao-Yu Fu, Johan P. U. Fynbo, Xing Gao, Yong-Feng Huang, Shuai-Qing Jiang, Ya-Hui Jiang, Yashaswi Julakanti, Erik Kuulkers, Qing-Hui Lao, Dongyue Li, Zhi-Xing Ling, Xing Liu, Yuan Liu, Jia-Yu Mou, Xin Pan, Varun, Daming Wei, Qinyu Wu, Muskan Yadav, Yu-Han Yang, Weimin Yuan, Shuang-Nan Zhang
Figure caption: The observed light curves of GRB 240219A and its spectral evolution based on the best-fit parameters of the CPL model for Fermi/GBM spectra, the PL model for EP/WXT spectra, and the CPL model for Fermi/GBM-EP/WXT spectra. Same time slices are highlighted in same colors across all panels. All error bars on data points represent the 1σ confidence level.
Paper: Triggering the Untriggered: The First Einstein Probe-detected Gamma-Ray Burst 240219A and Its Implications
Authors: Yi-Han Iris Yin, Bin-Bin Zhang, Jun Yang, Hui Sun, Chen Zhang, Yi-Xuan Shao, You-Dong Hu, Zi-Pei Zhu, Dong Xu, Li An, He Gao, Xue-Feng Wu, Bing Zhang, Alberto Javier Castro-Tirado, Shashi B. Pandey, Arne Rau, Weihua Lei, Wei Xie, Giancarlo Ghirlanda, Luigi Piro, Paul O'Brien, Eleonora Troja, Peter Jonker, Yun-Wei Yu, Jie An, Run-Chao Chen, Yi-Jing Chen, Xiao-Fei Dong, Rob Eyles-Ferris, Zhou Fan, Shao-Yu Fu, Johan P. U. Fynbo, Xing Gao, Yong-Feng Huang, Shuai-Qing Jiang, Ya-Hui Jiang, Yashaswi Julakanti, Erik Kuulkers, Qing-Hui Lao, Dongyue Li, Zhi-Xing Ling, Xing Liu, Yuan Liu, Jia-Yu Mou, Xin Pan, Varun, Daming Wei, Qinyu Wu, Muskan Yadav, Yu-Han Yang, Weimin Yuan, Shuang-Nan Zhang
Figure caption: The E p,z–E iso diagram. The blue, gray, and red solid lines represent the best-fit correlations for Type-I, Type-II, and magnetar giant flare populations, respectively. The purple dashed line indicates the position of GRB 240219A at various redshifts, with specific redshifts marked by dots. Error bars on data points represent the 1σ confidence level.
Paper: Triggering the Untriggered: The First Einstein Probe-detected Gamma-Ray Burst 240219A and Its Implications
Authors: Yi-Han Iris Yin, Bin-Bin Zhang, Jun Yang, Hui Sun, Chen Zhang, Yi-Xuan Shao, You-Dong Hu, Zi-Pei Zhu, Dong Xu, Li An, He Gao, Xue-Feng Wu, Bing Zhang, Alberto Javier Castro-Tirado, Shashi B. Pandey, Arne Rau, Weihua Lei, Wei Xie, Giancarlo Ghirlanda, Luigi Piro, Paul O'Brien, Eleonora Troja, Peter Jonker, Yun-Wei Yu, Jie An, Run-Chao Chen, Yi-Jing Chen, Xiao-Fei Dong, Rob Eyles-Ferris, Zhou Fan, Shao-Yu Fu, Johan P. U. Fynbo, Xing Gao, Yong-Feng Huang, Shuai-Qing Jiang, Ya-Hui Jiang, Yashaswi Julakanti, Erik Kuulkers, Qing-Hui Lao, Dongyue Li, Zhi-Xing Ling, Xing Liu, Yuan Liu, Jia-Yu Mou, Xin Pan, Varun, Daming Wei, Qinyu Wu, Muskan Yadav, Yu-Han Yang, Weimin Yuan, Shuang-Nan Zhang
Figure caption: Fluence ratio and E p distribution of Fermi/GBM-detected GRB samples. The red dashed vertical lines denote boundaries of GRB subclasses, labeled accordingly. Yellow vertical lines indicate the location of GRB 240219A on the plot.
Paper: Formation and Eruption of a Hot Channel Magnetic Flux Rope in a Nested Double Null Magnetic System
Authors: Surui Yao, Yuandeng Shen, Chengrui Zhou, Dongxu Liu, Xinping Zhou
Figure caption: The reconstructed three-dimensional magnetic topology of the source region and relevant QSLs and J/B distribution. Panel (a) is the top view of the inner magnetic null point system and has the same range as the black box in Figure 1(e). The green and yellow curves denote the observed two filaments. The enlarged plot in panel (a) shows the observed hot channel and displays the same region as the white box in panel (a). The red, orange, yellow, and green boxes in panel (a) correspond to the colored boxes in Figure 4(b). Panel (b) shows the photospheric horizontal velocity map, determined by the FLCT method, overlaid with the extrapolated field lines. The enlarged plot in panel (b) is the XRT Al_Poly image at 02:22:38 UT, which contains a hot loop. Panels (e) and (f) show the distribution of the J/B and QSLs along the dashed black line in panel (a), crossing the position where the inner null point exists at 02:12 UT on 2014 September 28. The dashed white lines in panels (e) and (f) indicate the height of the X-type distribution. Panel (c) is the HMI image at 00:00:33 UT on 2014 September 27, overlaid with red (300 G; positive) and blue (−300 G; negative) contours at 02:22:20 UT on 2014 September 28. Panel (d) is the temporal evolution of the positive (red) and negative (blue) magnetic fluxes calculated over the same range as panel (b) from 01:20 UT to 02:30 UT on 2014 September 28.
Paper: Formation and Eruption of a Hot Channel Magnetic Flux Rope in a Nested Double Null Magnetic System
Authors: Surui Yao, Yuandeng Shen, Chengrui Zhou, Dongxu Liu, Xinping Zhou
Figure caption: Overview of this event on 2014 September 28. Panel (a) is the AIA 171 Å image overlaid by HMI magnetogram contours (±300 G; red = positive, blue = negative). Two filaments (F1 and F2; indicated by the green and yellow arrows, respectively) exist under a large-scale fan–spine magnetic flux system within a null point, noted by a white arrow. Panel (b) is the AIA 304 Å image and displays the eruption signatures of the source region. The white rectangle in panel (b) indicates the FOV of panels (c) and (d). Panel (c) presents the locations of the two filaments (F1 and F2; indicated by the green and yellow lines) on the HMI magnetogram. In panel (d), the Hα image acquired by NVST shows that the filaments were stable during the entire process, which is overlaid with the RHESSI images for 6–12 (red) and 25–50 (blue) keV for 20%, 45%, 75%, and 95% of the maximum emission. The white arrows in panel (d) indicate the two flare ribbons. Panel (e) is the reconstructed three-dimensional magnetic topology of the source region revealed by NLFFF extrapolation at 02:12 UT on 2014 September 28. The gray and red curves indicate the outer fan–spine magnetic system. The black box in panel (e) indicates the FOV of panels (f) and (g) and has the same range as the white box in panel (b). Panel (f) shows the side view of the inner magnetic null point system (indicated by the black, pink, cyan, and orange curves), containing an inner null point (17.4 Mm above the photosphere). Panel (g) is the top view of the inner magnetic null point system. The green and yellow curves in the extrapolation results indicate the two observed filaments.
Paper: Formation and Eruption of a Hot Channel Magnetic Flux Rope in a Nested Double Null Magnetic System
Authors: Surui Yao, Yuandeng Shen, Chengrui Zhou, Dongxu Liu, Xinping Zhou
Figure caption: Temporal evolution of the hot channel and synchronous fluxes. Panel (a) shows a time–distance diagram of AIA 131 Å images made along the white line in Figure 2(b) (i.e., the white line in Figure 4(b)) enhanced by the multiscale Gaussian normalization method (H. Morgan & M. Druckmüller 2014). The slow rise and impulsive acceleration phase of the hot channel (indicated by a dashed white curve) have been observed in this time–distance diagram. Panel (b) shows GOES SXR fluxes in 1–8 Å (indicated by the black curve), the normalized light curve of AIA 131 Å (denoted by the blue curve) obtained by integrating the region in the white box in Figure 2(b), and RHESSI X-ray fluxes at different energies in different colored curves. The speed (blue) and acceleration (red) of the hot channel in panel (c) were measured along the dashed white curve in panel (a). The left and right dashed vertical lines in panels (a) and (b) indicate the start time of the slow rise and the impulsive acceleration phase of the hot channel, respectively.
Paper: 2019 UO14: A Transient Trojan of Saturn
Authors: Man-To Hui, 文韜 許, Paul A. Wiegert, Robert Weryk, Marco Micheli, David J. Tholen, Sam Deen, Andrew J. Walker, Richard Wainscoat
Figure caption: Apparent magnitude of 2019 UO14 as a function of time (a) and its absolute magnitude vs. true anomaly (b). The horizontal dotted lines in panel (b) represent weighted means of absolute magnitude in the corresponding bands, which are distinguished by colors. As the legends indicate, data points from different telescopes are plotted as different symbols. To improve visual clarity, measurements with uncertainties ≤0.3 mag are plotted in bolder font.
Paper: 2019 UO14: A Transient Trojan of Saturn
Authors: Man-To Hui, 文韜 許, Paul A. Wiegert, Robert Weryk, Marco Micheli, David J. Tholen, Sam Deen, Andrew J. Walker, Richard Wainscoat
Figure caption: Comparison of the normalized radial surface brightness profile of 2019 UO14 (open dots) with that of the PSF (black dashed curve) and models of varying activity levels (solid curves in various colors, as indicated in the legends) on (a) 2017 July 19, (b) 2018 October 2, and (c) 2019 November 7. Despite these examples having the best S/N if compared to other observations, the signal from 2019 UO14 becomes dominated by the sky background beyond ∼1″ from the optocenter. Taking the scatter into consideration, no obvious differences can be discerned in the radial brightness profiles between the object and the PSF.
Paper: 2019 UO14: A Transient Trojan of Saturn
Authors: Man-To Hui, 文韜 許, Paul A. Wiegert, Robert Weryk, Marco Micheli, David J. Tholen, Sam Deen, Andrew J. Walker, Richard Wainscoat
Figure caption: The color of 2019 UO14 (plotted as the star in magenta) in comparison to that of miscellaneous populations of small solar system bodies (C. L. Dandy et al. 2003; G. M. Szabó et al. 2007; M. Solontoi et al. 2012; D. Jewitt 2015; L. Markwardt et al. 2023, and citations therein) and the Sun (C. N. A. Willmer 2018) in the SDSS g − r and r − i regimes. Open circles with letters labeled mark typical colors of main-belt asteroid taxonomic classes. We followed K. Jordi et al. (2006) and applied transformations for reported color indices not in the SDSS system. The gray dashed curve represents the locus of bodies with linear reflectivity spectra in the investigated space. We notice that the measured color of 2019 UO14 is in line with that of Jupiter and Neptune Trojans and that it is less similar to that of Centaurs, yet not beyond the 3σ level.
Paper: 2019 UO14: A Transient Trojan of Saturn
Authors: Man-To Hui, 文韜 許, Paul A. Wiegert, Robert Weryk, Marco Micheli, David J. Tholen, Sam Deen, Andrew J. Walker, Richard Wainscoat
Figure caption: The mean longitude of 2019 UO14 (black) relative to Saturn along with 100 clones (blue) generated from the orbital covariance matrix.
Paper: 2019 UO14: A Transient Trojan of Saturn
Authors: Man-To Hui, 文韜 許, Paul A. Wiegert, Robert Weryk, Marco Micheli, David J. Tholen, Sam Deen, Andrew J. Walker, Richard Wainscoat
Figure caption: The time evolution of the semimajor axis a, perihelion distance q, and eccentricity e of the nominal orbit of 2019 UO14 (black) and 100 clones (blue).
Paper: 2019 UO14: A Transient Trojan of Saturn
Authors: Man-To Hui, 文韜 許, Paul A. Wiegert, Robert Weryk, Marco Micheli, David J. Tholen, Sam Deen, Andrew J. Walker, Richard Wainscoat
Figure caption: Selected images of 2019 UO14. All but the HSC image were coadded from individual exposures taken on the same nights. Each panel is annotated with the date of observation formatted as YYYYMMDD in the upper-left corner and the used telescope/camera in the upper-right corner. A horizontal white scale bar in the lower-left corner represents an apparent length of 10″. The images are oriented such that the J2000 equatorial north is upwards and east is to the left.
Paper: From Coasting to Energy-conserving: New Self-similar Solutions to the Interaction Phase of Strong Explosions
Authors: Eric R. Coughlin
Figure caption: The density (top left), velocity (top right), and pressure (bottom left) profiles for a wind-driven explosion (m = 2; left) in a constant-density (n = 0) ambient medium and γ = 5/3. The black dashed curves give the predictions from the self-similar solution, while the orange curves are from a FLASH hydrodynamical simulation. The bottom right panel shows the RS shell width, Δr, as a function of the radius of the CD, both from FLASH (orange) and as predicted by the self-similar solution (black dashed).
Paper: From Coasting to Energy-conserving: New Self-similar Solutions to the Interaction Phase of Strong Explosions
Authors: Eric R. Coughlin
Figure caption: Left: β (the leading nonzero power-law index of the pressure) as a function of n for γ = 5/3 (blue) and γ = 4/3 (orange) and m = 3. Since β > 0, the pressure converges near the CD, but the rate of convergence is extremely slow as n → 3. Right: the self-similar pressure in the RS shell, h r, as a function of −η on a logarithmic scale. The numerical accuracy needs to be extremely high, with the functions resolved at ∣η∣ ≤ 10−11 for n = 2 and ∣η∣ ≤ 10−16 for n = 2.5, to correctly determine the pressure at the CD and thus the eigenvalues controlling the expansion of the RS shell and the deceleration of the CD.
Paper: From Coasting to Energy-conserving: New Self-similar Solutions to the Interaction Phase of Strong Explosions
Authors: Eric R. Coughlin
Figure caption: Same as Figure 4 but for homologously expanding ejecta (m = 3) impacting a wind-like medium (n = 2).
Paper: From Coasting to Energy-conserving: New Self-similar Solutions to the Interaction Phase of Strong Explosions
Authors: Eric R. Coughlin
Figure caption: Analogous to Figure 2, but here we are plotting the corrections to the FS density g 1, velocity f 1, and pressure h 1.
Paper: Intense Star Cluster Formation: Stellar Masses, the Mass Function, and the Fundamental Mass Scale
Authors: Christopher D. Matzner
Figure caption: A toy model for star cluster formation, in which Σ is held fixed at either 3 (left) or 20 (right) and the stellar population evolves under the influence of its own radiation while the upper mass slope evolves according to the hypothetical relation (Equation (26)). Curves are plotted as dashed lines once the Eddington factor Γ exceeds 0.8, as this is likely to imply disruption by radiation pressure gradients. In the right panel, the kink in the lines arises from the change in the opacity law at T = 150 K. See Section 8.2 for additional details.