adsabs/AstroCLIMB huggingface dataset:
Paper: Variations of the Vector Magnetic Structures in the Solar Polar Regions Observed by Hinode
Authors: Shuhong Yang, Chunlan Jin, Qiao Song, Yuzong Zhang, Yin Li, Yijun Hou, Ting Li, Guiping Zhou, Yuanyong Deng, Jingxiu Wang
Figure caption: Overview of the north polar region at the solar minimum between solar cycles 24 and 25. (a) Radial magnetic flux density observed by Hinode/SP on 2020 September 6. The plus sign marks the pole. The green dotted curve indicates the 70° latitude, the blue dashed curve outlines the boundary of ±90° longitude, and the region outside this range is not considered. (b) Magnetic patches with magnetic flux density stronger than 10 Mx cm−2 and a size of no less than 3 contiguous pixels. (c) Magnetic inclination angles with respect to the local normal corresponding to the magnetic patches in panel (b).
Paper: Unveil a Peculiar Light-curve Pattern of Magnetar Burst with GECAM Observations of SGR J1935+2154
Authors: Yue Wang, Chen-Wei Wang, Shao-Lin Xiong, Shuo Xiao, Yan-Qiu Zhang, Sheng-Lun Xie, Lin Lin, Yuan-Pei Yang, Hao-Xuan Guo, Ce Cai, Yue Huang, Cheng-Kui Li, Bing Li, Xiao-Bo Li, Jia-Cong Liu, Xiang Ma, Li-Ming Song, Wen-Jun Tan, Ping Wang, Wang-Chen Xue, Shu-Xu Yi, Yun-Wei Yu, Zheng-Hang Yu, Jin-Peng Zhang, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhang, Xiao-Yun Zhao, Chao Zheng, Shi-Jie Zheng
Figure caption: Light curves of some MXBs from SGR J1935+2154 detected by GECAM. The red lines are the fitting results of the ERCOD or FRED model based on the MCMC method. (a) Typical MXBs with ERCOD light-curve pattern. (b) MXBs with ERCOD light-curve pattern and an accompanying initial pulse. The initial pulse is ignored in the fitting. (c) MXBs with FRED light-curve pattern.
Paper: Unveil a Peculiar Light-curve Pattern of Magnetar Burst with GECAM Observations of SGR J1935+2154
Authors: Yue Wang, Chen-Wei Wang, Shao-Lin Xiong, Shuo Xiao, Yan-Qiu Zhang, Sheng-Lun Xie, Lin Lin, Yuan-Pei Yang, Hao-Xuan Guo, Ce Cai, Yue Huang, Cheng-Kui Li, Bing Li, Xiao-Bo Li, Jia-Cong Liu, Xiang Ma, Li-Ming Song, Wen-Jun Tan, Ping Wang, Wang-Chen Xue, Shu-Xu Yi, Yun-Wei Yu, Zheng-Hang Yu, Jin-Peng Zhang, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhang, Xiao-Yun Zhao, Chao Zheng, Shi-Jie Zheng
Figure caption: Spectral properties of ERCOD (orange triangles) and FRED (blue squares) samples. (a) Distribution of BB temperature (kT) and flux (obtained from the BB model). (b) Distribution of Ep and flux (obtained from the CPL (α = 1) model).
Paper: Unveil a Peculiar Light-curve Pattern of Magnetar Burst with GECAM Observations of SGR J1935+2154
Authors: Yue Wang, Chen-Wei Wang, Shao-Lin Xiong, Shuo Xiao, Yan-Qiu Zhang, Sheng-Lun Xie, Lin Lin, Yuan-Pei Yang, Hao-Xuan Guo, Ce Cai, Yue Huang, Cheng-Kui Li, Bing Li, Xiao-Bo Li, Jia-Cong Liu, Xiang Ma, Li-Ming Song, Wen-Jun Tan, Ping Wang, Wang-Chen Xue, Shu-Xu Yi, Yun-Wei Yu, Zheng-Hang Yu, Jin-Peng Zhang, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhang, Xiao-Yun Zhao, Chao Zheng, Shi-Jie Zheng
Figure caption: Distribution of fluence and duration (T90) for MXBs with ERCOD (orange triangles) and FRED (blue squares) patterns. (a) Fluence derived from the BB model. (b) Fluence derived from the CPL (α = 1) model. The red and blue lines represent the fitting results for the ERCOD and FRED samples, respectively.
Paper: Variations of the Vector Magnetic Structures in the Solar Polar Regions Observed by Hinode
Authors: Shuhong Yang, Chunlan Jin, Qiao Song, Yuzong Zhang, Yin Li, Yijun Hou, Ting Li, Guiping Zhou, Yuanyong Deng, Jingxiu Wang
Figure caption: Distribution function of the polar radial magnetic fields observed by Hinode/SP. The green solid curve shows the Gaussian fit to the distribution function in the range of ±50 Mx cm−2. The horizontal dotted line marks the FWHM, i.e., 2σ.
Paper: Unveil a Peculiar Light-curve Pattern of Magnetar Burst with GECAM Observations of SGR J1935+2154
Authors: Yue Wang, Chen-Wei Wang, Shao-Lin Xiong, Shuo Xiao, Yan-Qiu Zhang, Sheng-Lun Xie, Lin Lin, Yuan-Pei Yang, Hao-Xuan Guo, Ce Cai, Yue Huang, Cheng-Kui Li, Bing Li, Xiao-Bo Li, Jia-Cong Liu, Xiang Ma, Li-Ming Song, Wen-Jun Tan, Ping Wang, Wang-Chen Xue, Shu-Xu Yi, Yun-Wei Yu, Zheng-Hang Yu, Jin-Peng Zhang, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhang, Xiao-Yun Zhao, Chao Zheng, Shi-Jie Zheng
Figure caption: The distribution of trise and tdecay for MXBs with ERCOD (orange triangles) and FRED (blue squares) patterns. The black lines are the fitting results to the data separately. The gray dotted lines indicate the ratio between trise and tdecay.
Paper: Unveil a Peculiar Light-curve Pattern of Magnetar Burst with GECAM Observations of SGR J1935+2154
Authors: Yue Wang, Chen-Wei Wang, Shao-Lin Xiong, Shuo Xiao, Yan-Qiu Zhang, Sheng-Lun Xie, Lin Lin, Yuan-Pei Yang, Hao-Xuan Guo, Ce Cai, Yue Huang, Cheng-Kui Li, Bing Li, Xiao-Bo Li, Jia-Cong Liu, Xiang Ma, Li-Ming Song, Wen-Jun Tan, Ping Wang, Wang-Chen Xue, Shu-Xu Yi, Yun-Wei Yu, Zheng-Hang Yu, Jin-Peng Zhang, Peng Zhang, Shuang-Nan Zhang, Wen-Long Zhang, Zhen Zhang, Xiao-Yun Zhao, Chao Zheng, Shi-Jie Zheng
Figure caption: Fitting of normalized light curves. The FRED (dashed line) and ERCOD (solid line) shapes are plotted over the normalized light curves. (a) Normalized light curves of MXBs with the FRED light-curve pattern. (b): Normalized light curves of MXBs with the ERCOD light-curve pattern.
Paper: Variations of the Vector Magnetic Structures in the Solar Polar Regions Observed by Hinode
Authors: Shuhong Yang, Chunlan Jin, Qiao Song, Yuzong Zhang, Yin Li, Yijun Hou, Ting Li, Guiping Zhou, Yuanyong Deng, Jingxiu Wang
Figure caption: Magnetic inclination with respect to the local normal. (a) Long-term variations of the average inclination angles of the positive (indicated by asterisks) and negative (indicated by diamonds) magnetic fields in the north polar region. (b) Variations of the inclination angles of the positive (red curve) and negative (blue curve) fields vs. the thresholds of unsigned radial flux density in the north polar region in 2019 (marked by the vertical line in panel (a)). (c) Similar to panel (a), but for the magnetic inclination in the south polar region. (d) Similar to panel (b), but for the south polar region in 2018 (marked by the vertical line in panel (c)). In this figure, the values of magnetic inclination of the negative fields are shown as 180°–γ, where γ is the inclination angle with respect to the local normal. The horizontal lines in panels (a) and (c) indicate the values around which the inclination angles of nondominant polarity fluctuate.
Paper: Variations of the Vector Magnetic Structures in the Solar Polar Regions Observed by Hinode
Authors: Shuhong Yang, Chunlan Jin, Qiao Song, Yuzong Zhang, Yin Li, Yijun Hou, Ting Li, Guiping Zhou, Yuanyong Deng, Jingxiu Wang
Figure caption: Proportions of the positive and negative magnetic flux in the total flux in polar regions. (a) Long-term variations of the proportion of the positive flux (indicated by asterisks) and negative flux (indicated by diamonds) in the total flux in the north polar region. (b) Variations of the proportion of the positive flux (red curve) and negative flux (blue curve) in the total flux vs. the thresholds of unsigned radial magnetic flux density in the north polar region in 2019 (marked by the vertical line in panel (a)). (c) Similar to panel (a), but for the flux proportions in the south polar region. (d) Similar to panel (b), but for the south polar region in 2017 (marked by the vertical line in panel (c)). The horizontal lines in panels (a) and (c) indicate the values at which the positive flux and negative flux are balanced.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: Surface density Σ plotted against dimensionless radius R/rg at late times. The solid curves are the numerical solutions of the disk diffusion equation, while the dashed curves are the self-similar solutions (Equation (12)). The masses of the SMBH and the disrupted star are M• = 106M⊙ and M⋆ = 0.3M⊙, respectively, and α = 0.1. The self-similar solutions provide a good match to numerical integration of the disk diffusion equation at late times and large radii.
Paper: Variations of the Vector Magnetic Structures in the Solar Polar Regions Observed by Hinode
Authors: Shuhong Yang, Chunlan Jin, Qiao Song, Yuzong Zhang, Yin Li, Yijun Hou, Ting Li, Guiping Zhou, Yuanyong Deng, Jingxiu Wang
Figure caption: Variations of the magnetic flux and magnetic flux density in the polar regions above 70° latitude from 2012 to 2021. (a) Positive flux (indicated by asterisks), negative flux (indicated by diamonds), total flux (black solid curve), and net flux (dotted curve) in the north polar region. (b) Similar to panel (a) but for the south polar region.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: A comparison between the Gaussian initial condition (solid) to the source function (dashed). The top panel shows the surface density as a function of radius at different times, while the bottom panel presents the light curves at different wavelengths (NUV: λ = 250 nm; FUV: λ = 150 nm; and X-ray: hf  = 300 eV). The masses of the SMBH and the disrupted star are M• = 106 M⊙ and M⋆ = 0.3 M⊙, respectively, and α = 0.1.
Paper: Variations of the Vector Magnetic Structures in the Solar Polar Regions Observed by Hinode
Authors: Shuhong Yang, Chunlan Jin, Qiao Song, Yuzong Zhang, Yin Li, Yijun Hou, Ting Li, Guiping Zhou, Yuanyong Deng, Jingxiu Wang
Figure caption: Long-term variations of the average inclination angles of the “horizontal” magnetic fields. (a) and (b) Similar to Figures 5(a) and (c), respectively.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: Late-time UV light-curve observations from Swift/UVOT for various TDEs (A. Mummery et al. 2024). Data are presented for the uvw2 filter. The light curves have been binned and averaged over 20 days intervals, with the error bars representing (asymmetric) 1σ uncertainties. The observations generally show smoothly evolving late-time emission, without the dramatic instabilities predicted by unmagnetized α-disk models (R.-F. Shen & C. D. Matzner 2014; A. L. Piro & B. Mockler 2025; with the possible exception of AT2018dyb).
Paper: Variations of the Vector Magnetic Structures in the Solar Polar Regions Observed by Hinode
Authors: Shuhong Yang, Chunlan Jin, Qiao Song, Yuzong Zhang, Yin Li, Yijun Hou, Ting Li, Guiping Zhou, Yuanyong Deng, Jingxiu Wang
Figure caption: Similar to Figure 5, but only for the “vertical” magnetic fields.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: Cumulative distribution functions showing the number of ULTRASAT-observable fossil TDEs as a function of their age (top), their comoving distance and redshift (middle), and SMBH mass (bottom). The limiting NUV AB magnitude in these estimations is mAB = 22.5. The results are shown for a 3σ detection threshold for the minimum detectable luminosity change over 1 yr and with two different photometric stability limits: ΔL = 1% (blue and orange) and ΔL = 5% (green and pink). The predicted numbers of ULTRASAT fossils are presented for two different estimates of the disk effective viscosity: α = 0.01 (orange and pink) and α = 0.1 (blue and green). In these calculations, we consider both the empirical TDE rate from the ZTF sample of TDEs (lower curves; Y. Yao et al. 2023) and the dynamically predicted rate from loss-cone theory (higher curves; N. C. Stone & B. D. Metzger 2016). Under our most pessimistic assumptions (low event rate, low α, and poor photometric stability), ULTRASAT will find ∼few TDE fossils; under our most optimistic assumptions (high event rate, high α, and good photometric stability), ∼210.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: Light curves (top panels) and RUV (bottom panels) for the magnetized α-disk, plotted as functions of time, and calculated for various M• values at an NUV wavelength (λ = 250 nm). The left panels correspond to α = 0.1, while the right panels use α = 0.01. Numerical solutions are shown in darker colors, while self-similar solutions are represented with lighter colors (the relative errors between the numerical and the self-similar solutions are calculated in Appendix B). The curves transition to dashed lines when the disks become optically thin and are truncated when RUV shrinks to the ISCO. A gray reference line, scaled as Lm,UV ∝ t−5/6 (Equation (15)), is included for comparison. The light curves remain UV-bright for many years before eventually turning off.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: Surface densities plotted against radius at different times, for the magnetized viscosity (solid) and the linear viscosity (dashed). The power laws of the linear viscosity are μl = {3/2, 5/9, 0, −3/2} from the top panel to the bottom panel. The normalization factor of the linear parameterization ν0,l is determined by equating the outer radius of the two disks after 1 yr. The choices of M•, M⋆, and α are the same as in Figure 3. The best match between the surface densities occurs for μl = 5/9 in the inner regions of the disk and μl = 0 in the outer regions.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: Light curves for the NUV, FUV, and X-ray bands (top panel to bottom panel), with Gaussian initial conditions for magnetized viscosity solutions (solid red) and linear viscosity solutions (dashed), with μl = {3/2, 5/9, 0, −3/2} (green, black, blue, and brown, respectively). The normalization factor of the linear parameterization ν0,l is determined by equating the outer radius of the disk after 1 yr. The choices of M•, M⋆, and α are the same as in Figure 3. The light curves of the linear and magnetized viscosity models appear very similar for μl = 0 but quite distinct for other values of μl.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: The time it takes for the QPEs to turn on after the TDE burst as a function of the SMBH mass (top) and recurrence time (bottom). The secondary object is a BH in a circular orbit with mass m•. The default parameters are m• = 10M⊙, trec = 48.4 hr, α = 0.1, M• = 106M⊙, and M⋆ = 0.3M⊙. Chandra observed the beginning of the QPEs ∼1500 days after AT2019qiz was first detected, around an SMBH with ﹩{\mathrm{log}}_{10}{M}_{\bullet }/{M}_{\odot }=6.{3}_{-0.2}^{+0.3}﹩, with a mean recurrence time between peaks of 48.4 ± 0.3 hr (M. Nicholl et al. 2024). The observed time to exhibit QPEs of AT2019qiz is longer than the expected time from our model.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: A scatter plot of the viscosity power-law values. Exact solutions for the Emden–Fowler equation are shown as blue lines (continuous solutions) and blue dots (discrete solutions). The red dots represent astrophysically interesting values, corresponding to all permutations of ﹩P\in \left\{{P}_{{\rm{gas}}},{P}_{{\rm{rad}}},{P}_{{\rm{mag}}}\right\}﹩ and ﹩\kappa \in \left\{{\kappa }_{{\rm{es}}},{\kappa }_{{\rm{Kr}}},{\kappa }_{{\rm{dust}}}\right\}﹩. The magnetized viscosity with κes, which is the focus of this study, is highlighted as a bold red dot. All solutions above the black line are stable, while those below the line are unstable. Currently, no exact solutions exist for the astrophysically interesting values.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: Surface densities plotted against radius at different times for the magnetized α-viscosity (solid) and the linear viscosity (dashed), similar to Figure 4. The first case (top) assumes a Gaussian initial condition, with the normalization factor of the linear viscosity parameterization, ν0,l, chosen to match the magnetized viscosity at the start time. The second case (bottom) includes a source term in the diffusion equation (Equation (1)) instead of a Gaussian initial condition.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: The relative error between the UV light curves from the numerical solution and the self-similar solution is shown as a function of the SMBH mass and stellar mass. The error is plotted for different α prefactor values (α = 0.1 and α = 0.01) and for different ages of the TDE (t = 10 yr and t = 100 yr). The white region corresponds to SMBH masses exceeding the Hills mass. The relative error is larger for masses near the Hills mass, while for other regions, the error remains below an order of magnitude.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: Light curves for NUV, FUV, and X-ray bands (left to right) with the magnetized α-viscosity (red) and the linear viscosity (dashed black, blue, and brown), similar to Figure 5. The first case (top) assumes a Gaussian initial condition, with the normalization factor of the linear viscosity parameterization, ν0,l, chosen to match the magnetized viscosity at the initial condition. The second case (bottom) includes a source term in the diffusion equation (Equation (1)) instead of a Gaussian initial condition.
Paper: Electrons in the Collisionally Young Solar Wind: Parker Solar Probe Observations
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. L. Stevens, R. Livi, S. D. Bale
Figure caption: Electron VDFs measured by the PSP SPAN-E sensors on Encounter 22. The top row shows distribution function vs. velocity in the plasma frame for 154 individual SPAN-E pixels, colored by pitch angle (velocities shown as negative for pitch angles >90°). Solid and dashed black lines show parallel and perpendicular cuts through bi-Maxwellian core fits. The second row shows the same VDFs binned into 12° × 15° pitch-angle bins, again colored by pitch angle, and plotted vs. energy. Dashed lines show corresponding cuts through the same fits. The third row shows aggregate VDFs accumulated over 20 minute intervals surrounding the center times above, and binned into 24° × 7﹩\mathop{.}\limits^{^\circ }﹩5 pitch-angle bins. Dashed lines again show corresponding cuts through the bi-Maxwellian fits. The fourth row shows 2D contour plots of the same aggregate VDFs.
Paper: Electrons in the Collisionally Young Solar Wind: Parker Solar Probe Observations
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. L. Stevens, R. Livi, S. D. Bale
Figure caption: Observations from PSP’s Encounter 22. The top panel shows the electron core density from bi-Maxwellian fits. The second panel shows the local flow speed measured by SPAN-I, and the inferred maximum asymptotic speed consistent with local energy flux measurements. The third panel shows the electron core parallel temperature and strahl parallel temperature from fits. The fourth panel shows the fitted core anisotropy T⊥/T∥. The fifth panel shows an estimated electron collisional age Ae. The sixth panel shows an estimate of the Knudsen number. Blue lines indicate the times of VDFs shown in Figure 1, and green lines and letters indicate the times of VDFs shown in Figure 3.
Paper: Electrons in the Collisionally Young Solar Wind: Parker Solar Probe Observations
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. L. Stevens, R. Livi, S. D. Bale
Figure caption: Six example electron VDFs measured by the PSP SPAN-E instruments on Encounter 22, in the same format as the top row of Figure 1, at the times indicated by green lines in Figure 2.
Paper: Electrons in the Collisionally Young Solar Wind: Parker Solar Probe Observations
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. L. Stevens, R. Livi, S. D. Bale
Figure caption: Six example electron VDFs measured by the PSP SPAN-E instruments on Encounter 23, in the same format as the top row of Figure 1, at the times indicated by green lines in Figure 4.
Paper: Electrons in the Collisionally Young Solar Wind: Parker Solar Probe Observations
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. L. Stevens, R. Livi, S. D. Bale
Figure caption: The median ratio of the core parallel temperature to the strahl parallel temperature (top) and the median core anisotropy (bottom), both derived from PSP SPAN-E measurements on Encounters 4–23, separated into six equally populated bins by the approximately conserved quantity nur2. Error bars show quartile ranges around median values.
Paper: Electrons in the Collisionally Young Solar Wind: Parker Solar Probe Observations
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. L. Stevens, R. Livi, S. D. Bale
Figure caption: Observations from PSP’s Encounter 23, in the same format as Figure 2. Green lines and letters indicate the times of VDFs shown in Figure 5.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: The effective temperature Teff vs. radius at different times for the magnetized viscosity (solid) and the linear viscosity (dashed). The first case (left) assumes a Gaussian initial condition, where the normalization factor for the linear parameterization ν0,l is determined by matching the disk’s outer radius after 1 yr. The second case (right) also assumes a Gaussian initial condition, but the normalization factor is chosen to match the magnetized viscosity at the initial condition.
Paper: Late-time Evolution of Magnetized Disks in Tidal Disruption Events
Authors: Yael Alush, Nicholas C. Stone
Figure caption: The same as Figure 13 but including a source term in the diffusion equation (Equation (1)) instead of using a Gaussian initial condition.
Paper: Electrons in the Collisionally Young Solar Wind: Parker Solar Probe Observations
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. L. Stevens, R. Livi, S. D. Bale
Figure caption: Non-self-consistent estimate of the number of Coulomb collisions experienced by electrons following orbits that conserve energy and magnetic moment in a diverging magnetic field and potential structure consistent with the solar wind. Both cases assume an isotropic Maxwellian with a temperature of kTe = 100 eV for the initial electron distribution. The top row shows results at three different radii for a source density of 4 × 104 cm−3 at 5R⊙, and the bottom row shows results for a source density of 4 × 103 cm−3 at 5R⊙.
Paper: Electrons in the Collisionally Young Solar Wind: Parker Solar Probe Observations
Authors: J. S. Halekas, P. Whittlesey, D. E. Larson, M. L. Stevens, R. Livi, S. D. Bale
Figure caption: Frequency distributions of PSP measurements from Encounters 4–23 in terms of core anisotropy (top row) and core-to-strahl parallel temperature ratio (bottom row) vs. collisional age (left column) and the inferred maximum asymptotic speed (right column). Black lines show average values of core anisotropy and temperature ratio.
Paper: The Optical to X-Ray Luminosity and Spectrum of Supernova Wind Breakouts
Authors: Tal Wasserman, Nir Sapir, Peter Szabo, Eli Waxman
Figure caption: Solid lines show the numeric radiation spectral energy density at ﹩{\tilde{r}}_{{\rm{sh}}}﹩, er,ε ≡ ∂εer, as a function of photon energy, ε, normalized to the bolometric energy density er, Equation (18), for different shock radii, R14 = 1 and v9 = 0.5, 1, and 2. Analytic approximations for various regimes are shown in dashed lines (corresponding to shock radii of their adjacent solid lines): Comptonized Wien (black, Equation (20)), unsaturated Comptonization (red, Equation (31)), thermal radiation originating from the dense shell (brown, Equation (23)), and bremsstrahlung cooling (magenta, Equation (28)).