adsabs/AstroCLIMB huggingface dataset:
Paper: Multiphase Gas Nature in the Sub-parsec Region of the Active Galactic Nuclei. III. Eddington Ratio Dependence on the Structures of Dusty and Dust-free Outflows
Authors: Yuki Kudoh, Keiichi Wada, Nozomu Kawakatu, Mariko Nomura
Figure caption: Same as Figure 4, but showing the radial profiles of ﹩\mathrm{log}\,{\gamma }_{\mathrm{Edd}}=0﹩ (black), −1 (red), −2 (blue), and −3 (green). In panel (a), downward arrows indicate the dust sublimation radius, while upward arrows denote the radius where the velocity reaches a minimum at a characteristic radius.
Paper: Multiphase Gas Nature in the Sub-parsec Region of the Active Galactic Nuclei. III. Eddington Ratio Dependence on the Structures of Dusty and Dust-free Outflows
Authors: Yuki Kudoh, Keiichi Wada, Nozomu Kawakatu, Mariko Nomura
Figure caption: Time-averaged column density N as a function of θ. Solid lines denote both the dusty and dust-free components, while dotted lines indicate the dusty component. The colors correspond as ﹩\mathrm{log}({\gamma }_{\mathrm{Edd}})=0﹩ (black), −1 (red), −2 (blue), and −3 (green).
Paper: Multiphase Gas Nature in the Sub-parsec Region of the Active Galactic Nuclei. III. Eddington Ratio Dependence on the Structures of Dusty and Dust-free Outflows
Authors: Yuki Kudoh, Keiichi Wada, Nozomu Kawakatu, Mariko Nomura
Figure caption: Same snapshots as in Figure 2, albeit showing the distribution of the ratio of the radiation force to gas pressure force. Red regions indicate where radiation force dominates, while blue regions indicate the dominance of gas pressure. In the model with ﹩\mathrm{log}\,{\gamma }_{\mathrm{Edd}}=-3﹩, the thermal wind is primarily driven by gas pressure, contrasting with the radiation-driven wind observed in the other three models with larger γ Edd.
Paper: Multiphase Gas Nature in the Sub-parsec Region of the Active Galactic Nuclei. III. Eddington Ratio Dependence on the Structures of Dusty and Dust-free Outflows
Authors: Yuki Kudoh, Keiichi Wada, Nozomu Kawakatu, Mariko Nomura
Figure caption: The time-averaged ionization degrees are arranged from top to bottom in descending order of Eddington ratio. The left panel plots describe the line-of-sight ionization degree for each angle θ = 60°, 40°, and 20°. The right plots describe the spatial distribution of the time-averaged mean ionization degree. For each Eddington ratio, the black regions in the R–z plane represent areas where the column density exceeds 1026 cm−2, i.e., ξ ∼ 0 erg s−1 cm.
Paper: Multiphase Gas Nature in the Sub-parsec Region of the Active Galactic Nuclei. III. Eddington Ratio Dependence on the Structures of Dusty and Dust-free Outflows
Authors: Yuki Kudoh, Keiichi Wada, Nozomu Kawakatu, Mariko Nomura
Figure caption: Comparison between analytical solutions (black dashed and dotted lines) and simulation results (blue solid lines) for the outflow velocity. The blue lines correspond to Figure 4(c). Dotted lines indicate the analytical solution without dust-radiation force, while dashed lines represent the solution with dust-radiation force.
Paper: Distribution and Anisotropy of the Energy Transfer Rate in the Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Liping Yang, Zhigang Yuan
Figure caption: (a) Mean value μ of the fitted normal distribution for the logarithmic energy transfer rate at ﹩{\mathrm{log}}_{10}(\epsilon )\lt 10﹩ as a function of τ. The dashed line denotes the fitted power-law line. (b) Fitted standard deviation σ as a function of τ. (c) Flatness of all the logarithmic energy transfer rates as a function of τ. The red dashed line represents the linear regression in the log–log space. The dashed line denotes F = 3, which corresponds to the normal distribution.
Paper: Distribution and Anisotropy of the Energy Transfer Rate in the Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Liping Yang, Zhigang Yuan
Figure caption: (a) Scaling exponents ξ (red dots) of the magnetic structure functions vs. the order p measured in the radial direction. The green dashed line denotes the prediction of the log-Poisson intermittency model with C = 1 and g = 3.78. (b) Energy transfer rates ﹩\hat{\epsilon }﹩ as a function of τ. (c1) Probability density distributions of the logarithmic energy transfer rate for τ = 12, 51, 96 s. The dashed line denotes the fitted normal distribution for ﹩{\mathrm{log}}_{10}(\epsilon )\lt 10﹩. (c2) The ratio between the observed and fitted probability densities. The blue shadow denotes the region well described by the normal distribution, and the red shadow denotes the region with growing intermittency as τ decreases.
Paper: Distribution and Anisotropy of the Energy Transfer Rate in the Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Liping Yang, Zhigang Yuan
Figure caption: (a) Mean value μ of the fitted normal distribution for the logarithmic energy transfer rate at ﹩{\mathrm{log}}_{10}(\epsilon )\lt 10﹩ as a function of τ, measured in different ranges of θ RB. The viridis dashed lines denote the fitted power-law lines. The red dashed lines denote μ ∼ τ 0.000 and μ ∼ τ 0.077. (b) Fitted standard deviation σ as a function of τ and θ RB. (c) Flatness of the logarithmic energy transfer rate as a function of τ and θ RB. Colors in the viridis map denote θ RB. The dashed lines represent the linear regressions in the log–log space.
Paper: Distribution and Anisotropy of the Energy Transfer Rate in the Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Liping Yang, Zhigang Yuan
Figure caption: (a) Scaling exponents ξ of the magnetic structure functions vs. the order p measured in different ranges of θ RB. The green dashed lines denote the predictions of the log-Poisson intermittency model with C = 1 but with different values of g for different sampling angles. (b) Energy transfer rate ﹩\hat{\epsilon }﹩ as a function of τ and θ RB. (c) Averaged energy transfer rate ﹩\lt \hat{\epsilon }\gt ﹩ as a function of θ RB. The viridis color map denotes θ RB.
Paper: Distribution and Anisotropy of the Energy Transfer Rate in the Solar Wind Turbulence
Authors: Honghong Wu, Shiyong Huang, Xin Wang, Liping Yang, Zhigang Yuan
Figure caption: Probability density distributions of the logarithmic energy transfer rate for (a1) τ = 12 s, (b1) τ = 51 s, and (c1) τ = 96 s. Colors in the viridis map denote θ RB. The red dashed line denotes the fitted normal distribution for ﹩{\mathrm{log}}_{10}(\epsilon )\lt 10﹩. (a2–c2) The corresponding ratios between the observed and fitted probability densities. The blue shadow denotes the region well described by the normal distribution, and the red shadow denotes the region with growing intermittency as τ decreases.
Paper: Mining for Protoclusters at z ∼ 4 from Photometric Data Sets with Deep Learning
Authors: Yoshihiro Takeda, Nobunari Kashikawa, Kei Ito, Jun Toshikawa, Rieko Momose, Kent Fujiwara, Yongming Liang, Rikako Ishimoto, Takehiro Yoshioka, Junya Arita, Mariko Kubo, Hisakazu Uchiyama
Figure caption: The g-, r-, and i-band magnitude distribution of g-dropout galaxies at z ∼ 4 in the simulation (PCcone; light blue) and the observational (HSC-SSP; yellow) data. The circles and squares represent the Deep and UltraDeep layers, respectively. The error bars of each point indicate Poisson errors.
Paper: Mining for Protoclusters at z ∼ 4 from Photometric Data Sets with Deep Learning
Authors: Yoshihiro Takeda, Nobunari Kashikawa, Kei Ito, Jun Toshikawa, Rieko Momose, Kent Fujiwara, Yongming Liang, Rikako Ishimoto, Takehiro Yoshioka, Junya Arita, Mariko Kubo, Hisakazu Uchiyama
Figure caption: Number density as a function of redshift for g-dropout galaxies in the simulation data. The right vertical axis represents the normalized density.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: The posterior distribution of the seven parameters (B, incl, Azi, v los, Δλ  D , η 0, and S) of Stokes profiles derived by the NNHMC method. In the seven white background diagonal plots, vertical solid lines represent the 50th percentile of the distribution, indicating the estimated value of the parameters. The dashed lines on either side of the solid line correspond to the 16th and 84th percentiles, representing the lower and upper bounds of the 68% confidence interval, which align with the innermost contour in the six blue background subplots. The specific statistics are displayed in the titles on the seven white background plots. The outermost contour in the blue background subplots represents the range of the 95% confidence interval for the inferred parameters. The blue dashed line in the upper right subfigure represents the actual observed profiles from the Hinode/SP, while the orange curve corresponds to the predicted profiles obtained using the NNHMC method.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: Inferred values of B, incl, Azi, and v los for 10,000 pixels of the NOAA AR 11045. The first and second columns display results from the NNHMC method and MERLIN code, respectively. The third columns show the difference between the parameters of the NNHMC inversion and the parameters of the MERLIN code inversion.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: The comparison between the synthetic Stokes profiles generated by the SynNN and the synthetic Stokes profiles generated by the M-E atmosphere model in a random sample from the test set. The four subfigures in the first row of the figure represent the Stokes I, Q, U, and V profiles, respectively. The blue profiles are one of the test sets generated by the M-E atmosphere model, and the corresponding parameters are B = 787.74 G, incl = 59.°01, Azi = 70.°47, v los = 0 km s−1, Δλ  D  = 17.72 mÅ, a = 0.48, η 0 = 24.69, S = 1.16, and β = 0.27. The orange profiles are generated by inputting the same parameters into the SynNN. The second row of the figure shows the residuals of these two Stokes profiles, with a dashed red line indicating zero residual values.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: Comparison of Stokes profiles for NNHMC inversion approaches in three representative pixels. The first two rows of subplots represent the active region, and the third row of subplots represents the quiet region. The black dotted lines in each subplot represent the actual observed profiles from the Hinode/SP, and the colored curves represent the predicted profiles obtained using the NNHMC method.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: The spatial distribution of map the R 2 between the NNHMC inferred Stokes profiles and the Hinode/SP observed Stokes profiles. The lower R 2 in the region marked “+” in the figure is mainly due to the strong asymmetry observed in the Stokes V profile.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: The Stokes V profile exhibits a strong asymmetry. The blue dashed line represents the actual observed profiles from the Hinode/SP, while the orange curve corresponds to the predicted profiles obtained using the NNHMC method.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: Gaussian kernel density estimate of the difference between the Stokes parameters of the value inferred by the MERLIN code and the NNHMC method, respectively. Panels (a) to (g) illustrate the B  z , B  x , B  y , B, incl, Azi, and v los. The y-axis represents the density of the x-axis values. The closer the values on the x-axis are to zero, the greater the consistency between the two methods. The MAE is also reported in each panel.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: The spatial distribution of parameter uncertainties inferred by the NNHMC method.
Paper: NNHMC: An Efficient Stokes Inversion Method Using a Neural Network (NN) Model Combined with the Hamiltonian Monte Carlo (HMC) Algorithm
Authors: Chong Xu, JinLiang Wang, Hao Li, ZiYao Hu, XianYong Bai, JiaBen Lin, Hui Liu, ZhenYu Jin, KaiFan Ji
Figure caption: Inferred values of B  z , B  x , and B  y  for 10,000 pixels of the NOAA AR 11045. The first and second columns display results from the NNHMC method and the MERLIN code, respectively. The third columns show the difference between the parameters of the NNHMC inversion and the parameters of the MERLIN code inversion.
Paper: Multiple Components of the Outflow in the Protostellar System HH 212: Outer Outflow Shell, Rotating Wind, Shocked Wind, and Jet
Authors: J. A. López-Vázquez, Chin-Fei Lee, Hsien Shang, Sylvie Cabrit, Ruben Krasnopolsky, Claudio Codella, Chun-Fan Liu, Linda Podio, Somnath Dutta, A. Murphy, Jennifer Wiseman
Figure caption: The PV diagram along the jet axis of the CO, SiO, and SO molecular line emission. (a) Comparison between the three molecular lines. (b) Comparison between CO and SiO emission. (c) Comparison between CO and SO emission. The color codes for the labels remain consistent across all panels. Magenta curves are included to guide readers for the parabolic PV structure. In all panels, the contours start from 3σ in steps of 3σ, 6σ, 9σ, and 12σ where σ = 2.11 mJy beam−1 km s−1, σ = 0.96 mJy beam−1 km s−1, and σ = 0.92 mJy beam−1 km s−1 for the CO, SiO, and SO, respectively. The bars in the left lower corner represent of each panel represent the angular resolution and the channel width used for the PV cut.
Paper: Multiple Components of the Outflow in the Protostellar System HH 212: Outer Outflow Shell, Rotating Wind, Shocked Wind, and Jet
Authors: J. A. López-Vázquez, Chin-Fei Lee, Hsien Shang, Sylvie Cabrit, Ruben Krasnopolsky, Claudio Codella, Chun-Fan Liu, Linda Podio, Somnath Dutta, A. Murphy, Jennifer Wiseman
Figure caption: ALMA first moment or intensity-weighted velocity of the CO molecular line emission overlaid in black contours the CO total intensity map. (a) Map of the extended emission. (b) Zoom-in of the central region. Red and blue contours represent the blueshifted and redshifted, respectively, of the intensity map of SO (LV) molecular line emission adopted from C.-F. Lee et al. (2021), while the black contours depicted the 358 GHz continuum map of the disk adopted from C.-F. Lee et al. (2017c). Black contour levels start from 3σ in steps of 3σ in steps of 2σ, 4σ, 6σ, 8σ, 10σ, 12σ, and 14σ, where σ = 13.92 mJy beam−1 km s−1. The contours of the continuum emission contours start from 3σ in steps of 3σ, 6σ, 9σ, and 12σ, where σ = 1.24 mJy beam−1. The synthesized beams are shown in the lower left corner of both panels.
Paper: Multiple Components of the Outflow in the Protostellar System HH 212: Outer Outflow Shell, Rotating Wind, Shocked Wind, and Jet
Authors: J. A. López-Vázquez, Chin-Fei Lee, Hsien Shang, Sylvie Cabrit, Ruben Krasnopolsky, Claudio Codella, Chun-Fan Liu, Linda Podio, Somnath Dutta, A. Murphy, Jennifer Wiseman
Figure caption: PV diagrams perpendicular to the jet axis of the molecular line emission from the CO (gray scale), SiO (green), and SO (blue) at different heights from z = ±50 au to z = ±200 au with an interval of 30 au. The ellipses in all panels represent the best fit for the SO and CO emission limit at 2σ. The red ellipses exclude the high-velocity components, and the dashed brown ellipses trace the high-velocity portion of the data. The description is the same as Figure 7.
Paper: Multiple Components of the Outflow in the Protostellar System HH 212: Outer Outflow Shell, Rotating Wind, Shocked Wind, and Jet
Authors: J. A. López-Vázquez, Chin-Fei Lee, Hsien Shang, Sylvie Cabrit, Ruben Krasnopolsky, Claudio Codella, Chun-Fan Liu, Linda Podio, Somnath Dutta, A. Murphy, Jennifer Wiseman
Figure caption: PV diagrams perpendicular to the jet axis of the molecular line emission from the CO (gray scale), SiO (green), and SO (blue) are presented at various heights from z = ±300 au to z = ±400 au with an interval of 50 au. The black, green, and blue bars represent the angular resolution and the channel width. The contour labels start at 2σ in steps of 3σ, 6σ, 9σ, and 12σ, where σ = 2.11 mJy beam−1 km s−1, σ = 0.96 mJy beam−1 km s−1, and σ = 0.92 mJy beam−1 km s−1 for the CO, SiO, and SO, respectively. The horizontal dashed line represents the position of the jet axis, and the vertical dashed line indicates V off. The red ellipses in all panels represent the best fit of the emission of the bright outer CO shell.
Paper: Multiple Components of the Outflow in the Protostellar System HH 212: Outer Outflow Shell, Rotating Wind, Shocked Wind, and Jet
Authors: J. A. López-Vázquez, Chin-Fei Lee, Hsien Shang, Sylvie Cabrit, Ruben Krasnopolsky, Claudio Codella, Chun-Fan Liu, Linda Podio, Somnath Dutta, A. Murphy, Jennifer Wiseman
Figure caption: The kinematical properties of the CO outflow of HH 212 as a function of the height with respect to the disk midplane z = 0. Top left: cylindrical radius R. Top right: radial expansion velocity V exp. Bottom left: rotation velocity V rot. Bottom right: specific angular momentum j obs. The error bars represent the uncertainties in the measurements of these kinematical properties. The brown points with error bars are derived from those dashed ellipses in Figure 8, for the three different heights at 50, 80, and 110 au from the midplane.
Paper: Multiple Components of the Outflow in the Protostellar System HH 212: Outer Outflow Shell, Rotating Wind, Shocked Wind, and Jet
Authors: J. A. López-Vázquez, Chin-Fei Lee, Hsien Shang, Sylvie Cabrit, Ruben Krasnopolsky, Claudio Codella, Chun-Fan Liu, Linda Podio, Somnath Dutta, A. Murphy, Jennifer Wiseman
Figure caption: The specific angular momentum as a function of the poloidal velocity, both normalized to ﹩\sqrt{{M}_{* }}﹩. The black and brown symbols represent the estimated values for the HH 212 CO wide-angle MHD disk winds, while the curves depict the expected relation from self-similar cold magnetocentrifugal disk winds with launching radii r 0 from 1 to 15 au (solid lines) and magnetic lever arm parameter λ from 1.5 to 5 (dashed lines). Figure adapted from J. Ferreira et al. (2006).
Paper: Multiple Components of the Outflow in the Protostellar System HH 212: Outer Outflow Shell, Rotating Wind, Shocked Wind, and Jet
Authors: J. A. López-Vázquez, Chin-Fei Lee, Hsien Shang, Sylvie Cabrit, Ruben Krasnopolsky, Claudio Codella, Chun-Fan Liu, Linda Podio, Somnath Dutta, A. Murphy, Jennifer Wiseman
Figure caption: Schematic diagram illustrating the components of the protostellar system of HH 212. The right panels depict PV diagrams perpendicular to the jet axis, showcasing various components of the system, including the ambient medium, envelope, cavity wall, an outer outflow shell, rotating wind, SiO shell, X-wind, and jet. The illustration is not to scale.
Paper: Multiple Components of the Outflow in the Protostellar System HH 212: Outer Outflow Shell, Rotating Wind, Shocked Wind, and Jet
Authors: J. A. López-Vázquez, Chin-Fei Lee, Hsien Shang, Sylvie Cabrit, Ruben Krasnopolsky, Claudio Codella, Chun-Fan Liu, Linda Podio, Somnath Dutta, A. Murphy, Jennifer Wiseman
Figure caption: The launching radii of the HH 212 CO wide-angle MHD disk winds as a function of the height with respect to the disk midplane z = 0. The radii are estimated using Anderson’s relation (J. M. Anderson et al. 2003), and the error bars represent the uncertainties in our estimations.
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption: The left column is multiwavelength afterglow light curves of GRB 170817A with the best-fit curves in our afterglow model. Different colors are used to represent different bands. The RS light curves are depicted as dotted lines, while the FS light curves are represented by dashed–dotted lines. The shaded region represents the variability from scintillation. The right column is the proper motion of GRB 170817A relative to an 8 day Hubble Space Telescope (HST) measurement. The blue line represents the result obtained from our model, based on the best-fitting parameters. The proper motion measured between 8–75, 8–206, and 8–230 days is 2.41 ± 0.38, 4.09 ± 0.42, and 5.07 ± 0.40 mas, respectively (K. P. Mooley et al. 2022).
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption:  R-band and 1 keV afterglow light curves for different jet models viewed at 20°. Jets have an isotropic energy E iso,c = 2 × 1052 erg and bulk Lorentz Γ0,c = 300 in the jet core. The CBM density is n 1 = 0.1 cm−3 (k = 0). The model values used in each case are θ c = θ j = 3° for a homogeneous (top-hat) jet; θ c = 6°, θ j = 15° for a two-component jet with an isotropic energy E iso,w = 1051 erg and bulk Lorentz factor Γ0,w = 10 in a wide jet; θ c = 3°, θ j = 10° and angular slope a = b = 2.5 for a power-law jet; and (bottom right) θ c = 3° for a Gaussian jet with an opening angle θ j = 5.°2 to keep the relativistic jet. In each subplot, the gray solid lines denote the total flux, and the red and blue solid lines denote the RS and FS synchrotron light curves. The red and blue dashed lines denote the SSC radiation from RS and FS. The red and blue dotted lines represent the IC emissions of scatterings of forward shock photons on reverse shocked electrons and reverse shock photons on forward shocked electrons.
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption:  R-band afterglow light curves for power-law jets viewed from 10° and 20°. The red lines illustrate the contributions from the RS, while the blue lines represent the FS light curves. Dotted lines indicate the jet core components, whereas dashed lines denote the power-law wing components, with gray solid lines reflecting the total flux. The dots on the plot are the approximated locations of FS and RS peaks from the jet core and power-law wings. The model parameters employed in these calculations include a half-opening angle θ c = 3° for the core and θ j = 10° for the power-law wings. The isotropic energy of the core is E iso,c = 2 × 1052 erg, with an initial bulk Lorentz factor Γ0,c = 300. The angular slopes are set to a = b = 2.5, and CBM density is n 1 = 0.1 cm−3 (k = 0).
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption: Same as Figure 6, but for the mixed jet model.
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption: Corner plot of the parameters derived from fitting the multiwavelength light curves of GRB 170817A with the two-component model. Our best-fitting parameters and corresponding 1σ uncertainties are shown with the black dashed lines in the histograms on the diagonal.