adsabs/AstroCLIMB huggingface dataset:
Paper: The Ancient Star Formation History of the Extremely Low-mass Galaxy Leo P: An Emerging Trend of a Post-reionization Pause in Star Formation
Authors: Kristen B. W. McQuinn, Max J. B. Newman, Evan D. Skillman, O. Grace Telford, Alyson Brooks, Elizabeth A. K. Adams, Danielle A. Berg, Martha L. Boyer, John M. Cannon, Andrew E. Dolphin, Anthony J. Pahl, Katherine L. Rhode, John J. Salzer, Roger E. Cohen, Steve R. Goldman
Figure caption: Comparison of the image quality and sensitivity in the three filters using a matched field of view. Immediately apparent is the higher resolution at bluer wavelengths, with some sources that are clearly resolved in F090W becoming blended in the F277W filter. Closer inspection also reveals greater sensitivity as one moves from red to blue filters, which we quantify using artificial star tests (see Table 1).
Paper: “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin
Figure caption: For marginal RWI, the minimum value of κ 2/Ω2 caused by bumps, gaps, and steps (blue, orange, and green curves, respectively) vs. feature width. Solid curves show CSS models for k  y  H = 0.03. Global models of bumps, outer gap edges and jumps (dashed curves) and of inner gap edges and drops (dotted–dashed curves) have m = 1, h = 0.03 (matching mh = k  y  H). Global models break the symmetry between inner and outer gap edges and between jumps and drops.
Paper: Instability in Supernova Fallback Disks and Its Effect on the Formation of Ultralong Period Pulsars
Authors: Hao-Ran Yang, Xiang-Dong Li, Shi-Jie Gao, Kun Xu
Figure caption: The evolution of several radii. The dashes lines represent several radii that may impact the evolution of the outer disk, while the solid lines indicate the inner radius and active outer radii of two models. The initial parameters are fixed to be M d0 = 10−4 M ⊙, R 0 = 102  R s, B 0 = 1015 G, α 0 = 45°, χ 0 = 60°, and P 0 = 0.1 s.
Paper: “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin
Figure caption: Marginal stability curves for the RWI of bumps in the CSS for different values of k  y  H. The incompressible, k  y  H → ∞, limit (dotted yellow curve) and ﹩\min ({\kappa }^{2})=0.6﹩ references (pink line with x’s) are shown. Axes and Rayleigh unstable region are as in Figure 3.
Paper: “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin
Figure caption: RWI growth rates of m = 1 modes in our h = 0.1 global disk for different shapes. Curves for marginal stability (solid), CSS marginal stability (dashed), Rayleigh marginal stability (black dotted–dashed), and marginal dust traps (dotted yellow) are shown.
Paper: “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin
Figure caption: A map of perturbed vorticity, ζ 1, for the RWI in the ISS, vs. x, y position, with arrows for the perturbed velocity  v  1. Rows from top to bottom have growth rates s/Ω ≈ 10−3, 10−2, and 10−1, respectively. Columns from left to right consider enthalpy bumps, gaps, and steps, respectively. Solid vertical lines mark the feature width, x = ±W. Dotted vertical lines locate the minima of the equilibrium vorticity, ζ 0. The enthalpy amplitude ﹩{ \mathcal J }﹩ was chosen to produce the desired growth, with wavenumber k  y  = 0.1/W in all cases.
Paper: “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin
Figure caption: RWI marginal stability curves for bumps in an h = 0.1 global disk with azimuthal mode number m = 1, 2, 3 (solid blue, orange, and green curves, respectively). Dashed curves show shearing-sheet results for comparison. The grayed-out region is Rayleigh unstable. The dotted yellow curve gives the minimum amplitude of dust-trapping bumps.
Paper: “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin
Figure caption: RWI growth rate, s, for bumps in the CSS, mapped vs. scaled bump amplitude, ΔΠ, and bump width relative to disk scale height, W/H. Different values of k  y  H are shown from left to right. Compressible (dashed orange) and incompressible (yellow dotted) marginal stability curves are compared.
Paper: “Halfway to Rayleigh” and Other Insights into the Rossby Wave Instability
Authors: Eonho Chang, Andrew N. Youdin
Figure caption: Same as Figure 3, except incompressible growth rates are scaled by a characteristic rate ﹩{({\rm{\Omega }}{k}_{y}^{2}{\rm{\Delta }}{\rm{\Pi }})}^{1/3}﹩. Away from the stability boundary, these scaled rates vary only moderately.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Edge-on disk slices within the central 10−3 pc. The color palette shows the magnetic field strength, and the arrows display the direction of the total magnetic field—here dominated by the toroidal field. The left panel taken at earlier times shows a turbulent disk with two dominant vortices (upper left and lower right) that are oriented at random angles with respect to the disk rotation. The middle panel displays a growing toroidal field with inverted polarity at the midplane, which experiences a minimum around the equatorial plane. The right panel taken at the end of the run, t = 2.5 kyr, shows a buckling toroidal field being expelled from the disk. The orientation of the slices is exactly the same as in Figure 4.
Paper: GTC Optical/Near-infrared Upper Limits and NICER X-Ray Analysis of SGR J1935+2154 for the Outburst in 2022
Authors: Yi-Xuan Shao, Ping Zhou, Xiang-Dong Li, Bin-Bin Zhang, Alberto Javier Castro-Tirado, Pei Wang, Di Li, Zeng-Hua Zhang, Zi-Jian Zhang, You-Dong Hu, Shashi B. Pandey
Figure caption: Distribution of spectral fit results of bursts from SGR J1935+2154. Each data point in the lower panels represents one burst. Left panel: BB radius vs. flux in 0.3–10 keV, with the color representing the BB temperature. The upper panel shows the distribution of the flux, which cannot be fitted by a log-normal function (green), but follows a power law with N ∝ F −0.76±0.10 (purple dots and solid line) for flux ≳2.6 × 10−9 erg cm−2 s−1. Middle panel: flux vs. BB temperature, with the color representing the BB radius. The upper panel shows the distribution of BB temperature fitted with a log-normal function with a mean of 1.63 keV and 1σ range of 1.13–2.36 keV. Right panel: BB temperature vs. BB radius, with the color representing the flux. The upper panel shows the distribution of BB radius fitted with a log-normal function with a mean of 4.35 km and 1σ range of 3.00–6.30 km). The vertical dashed lines show the mean value and 1σ range of the parameter.
Paper: GTC Optical/Near-infrared Upper Limits and NICER X-Ray Analysis of SGR J1935+2154 for the Outburst in 2022
Authors: Yi-Xuan Shao, Ping Zhou, Xiang-Dong Li, Bin-Bin Zhang, Alberto Javier Castro-Tirado, Pei Wang, Di Li, Zeng-Hua Zhang, Zi-Jian Zhang, You-Dong Hu, Shashi B. Pandey
Figure caption: GTC optical/NIR images of SGR J1935+2154. The three panels show the ﹩r^{\prime} ﹩ band image with an exposure of 900 s, the first observation in ﹩z^{\prime} ﹩ band with an exposure of 1350 s, and the second observation in ﹩z^{\prime} ﹩ band with an exposure of 2700 s, respectively. The cyan and red circles denote the 90% uncertainties of the magnetar’s position as determined by the Chandra X-ray observation and HST NIR observations, respectively.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Top panel: dominant acceleration profiles, along the polar axis of the accretion disk starting with t = 0.5 kyr and for t = 0.5 kyr increments—gravitational acceleration, a grav, acceleration based on the thermal pressure gradient, a th, and acceleration based on the gradient of magnetic pressure, a  B . Bottom panel: thermal (P th), magnetic (P  B ), and turbulent (P turb) pressure profiles along the polar axis of the accretion disk at the same times. All the variables have been measured at r = 0.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Evolution of magnetic field profiles along the polar axis−z (i.e., the lower hemisphere shown in Figure 4) of the accretion disk: β, toroidal field B  ϕ , vertical poloidal B  z  field, and the ratio B  ϕ /B  z  at four characteristic times. The measurements have been taken at r = 0.
Paper: GTC Optical/Near-infrared Upper Limits and NICER X-Ray Analysis of SGR J1935+2154 for the Outburst in 2022
Authors: Yi-Xuan Shao, Ping Zhou, Xiang-Dong Li, Bin-Bin Zhang, Alberto Javier Castro-Tirado, Pei Wang, Di Li, Zeng-Hua Zhang, Zi-Jian Zhang, You-Dong Hu, Shashi B. Pandey
Figure caption: Left panel: distribution of burst waiting time fit with the log-normal function with a mean of 59.94 s and 1σ range of 22.48–159.80 s. Middle panel: distribution of T 90 and the best-fit log-normal function with a mean of 0.20s and 1σ  range of 0.07–0.53 s. Right panel: distribution of burst counts rate and the best-fit log-normal function, with a mean of 142.41 s−1 and 1σ range of 73.36–276.47 s−1. The green line shows the best-fit log-normal distribution and the vertical dashed lines show the mean value and 1σ range of the parameter.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: Evolution of the profiles of (radial) poloidal field B  p , ratio B  ϕ /B  p , ratio P  B /P turb, and β as a function of cylindrical radius r in the accumulating accretion disk within r ∼ 0.1 pc, at different times. All the variables have been averaged over the disk thickness, h, and azimuthally.
Paper: Direct Collapse Accretion Disks within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion
Authors: Yang Luo, Isaac Shlosman
Figure caption: The spin parameter ﹩\lambda =J/{J}_{\max }﹩ within three representative radii, including the core radius of ∼2 × 10−4 pc, as a function of time.
Paper: Occurrence of Gravitational Collapse in the Accreting Neutron Stars of Binary-driven Hypernovae
Authors: L. M. Becerra, F. Cipolletta, C. L. Fryer, Débora P. Menezes, Constança Providência, J. A. Rueda, R. Ruffini
Figure caption: Time to collapse, defined as the time it takes the stars to leave the stability zone, as a function of the star’s initial angular momentum, for different values of the angular momentum efficiency, χ. The upper panels show the results assuming the eL3ω ρ parameterization for the EOS, while for the lower panels, we use the NL3ω ρ one. Black lines correspond to matter with nucleons, and blue lines correspond to matter with nucleons mixed with hyperons. The initial binary is the same as in Figure 4.
Paper: On the Formation of Super-Alfvénic Flows Downstream of Collisionless Shocks
Authors: Adnane Osmane, Savvas Raptis
Figure caption: Kinetic energy density normalized by the magnetic field energy density as a function of normalized time τ = ∣U  b ∣t/L 0 for a compressible flow. Curves are plotted for β ∥(0) varying between 0.02 and 0.1. Larger kinetic energy densities are reached for lower initial β ∥ values. The case study presented by B. Lavraud et al. (2007) corresponds to such instance of kinetic energy density enhancement for low β ∥ ≪ 1. This figure indicates that the resulting flow can become super-Alfvénic with values on the order of 2–3 times the Alfvén speed.
Paper: Occurrence of Gravitational Collapse in the Accreting Neutron Stars of Binary-driven Hypernovae
Authors: L. M. Becerra, F. Cipolletta, C. L. Fryer, Débora P. Menezes, Constança Providência, J. A. Rueda, R. Ruffini
Figure caption: Top: pressure–energy density relation for the cold NS EOS with the matter with nucleons only (solid line) and nucleons and hyperons (dotted line). Middle: mass–radius relation for nonrotating NSs. The color bands represent observational constraints given by the pulsar mass of PSR J0348+0432 (J. Antoniadis et al. 2013); on mass and radius from NICER measurements for pulsars PSR J0030+0451 (M. C. Miller et al. 2019; T. E. Riley et al. 2019) and PSR J0740+662 (M. C. Miller et al. 2021; T. E. Riley et al. 2021); and the mass of the secondary compact object of the GW190814 event (R. Abbott et al. 2020). The dashed gray line corresponds to the fastest observed radio pulsar, PSR J1748–2446ad (J. W. T. Hessels et al. 2006). Bottom: same as middle panel but adding the hot NS EOS with nucleons mixed with hyperons for two constant entropy per baryon values, s  B /n  B  = 1 and 2.
Paper: Occurrence of Gravitational Collapse in the Accreting Neutron Stars of Binary-driven Hypernovae
Authors: L. M. Becerra, F. Cipolletta, C. L. Fryer, Débora P. Menezes, Constança Providência, J. A. Rueda, R. Ruffini
Figure caption: Evolution of the NS (orange lines) and the νNS (green lines) in the ρ  c −M NS plane for different initial values of the angular momentum, J. Each panel corresponds to each EOS summarized in Table 2. We set the strength of the magnetic field to B ns = 1013 G and the angular momentum transfer efficiency χ = 0.5. The initial binary system is formed by a 1.9 M ⊙ NS and a CO star, whose progenitor is a star with M ZAMS = 30 M ⊙, and the orbital period is P orb = 5.77 minutes. The stability zone is delimited by the static (red solid line), Keplerian (red dashed line), and secular instability sequences (red dotted line).
Paper: Occurrence of Gravitational Collapse in the Accreting Neutron Stars of Binary-driven Hypernovae
Authors: L. M. Becerra, F. Cipolletta, C. L. Fryer, Débora P. Menezes, Constança Providência, J. A. Rueda, R. Ruffini
Figure caption: Same as Figure 5 but using an EOS with the eL3ω ρ parameterization with hyperons. The initial binary system is formed by a 1.9 M ⊙ NS and a CO star, whose progenitor is a star with M ZAMS = 30 M ⊙. The initial binary period is about 5.7 minutes for the black lines, 10.2 minutes for the blue ones, and 31 minutes for the red ones.
Paper: Occurrence of Gravitational Collapse in the Accreting Neutron Stars of Binary-driven Hypernovae
Authors: L. M. Becerra, F. Cipolletta, C. L. Fryer, Débora P. Menezes, Constança Providência, J. A. Rueda, R. Ruffini
Figure caption: Time to the secular instability limit by magnetic-dipole braking as a function of the initial angular momentum of the νNS and the NS companion, which do not collapse to a BH in the BdHN event but reach a mass greater than ﹩{M}_{\mathrm{TOV}}^{\max }﹩. The EOS is the eL3ω ρ parameterization with hyperons. The star’s initial mass is about 2.1 M ⊙, and its radius is between 13 and 16 km, depending on its angular momentum. The star reaches secular instability when ﹩J={J}_{\sec }\approx 3{{GM}}_{\odot }^{2}/c﹩.
Paper: Occurrence of Gravitational Collapse in the Accreting Neutron Stars of Binary-driven Hypernovae
Authors: L. M. Becerra, F. Cipolletta, C. L. Fryer, Débora P. Menezes, Constança Providência, J. A. Rueda, R. Ruffini
Figure caption: Same as Figure 5 but for a hot NS using the eL3ω ρ and NL3ω ρ parameterizations with hyperons for the EOS. The black lines correspond to the cold EOS, the blue ones for an EOS with constant entropy S1(s  B /n  B  = 1), and the red ones for an EOS with constant entropy S2(s  B /n  B  = 2) > S1. The initial binary system is formed by a 1.9 M ⊙ NS and a CO star, whose progenitor is a star with M ZAMS = 30 M ⊙ in an initial binary period of about 5.7 minutes.
Paper: Occurrence of Gravitational Collapse in the Accreting Neutron Stars of Binary-driven Hypernovae
Authors: L. M. Becerra, F. Cipolletta, C. L. Fryer, Débora P. Menezes, Constança Providência, J. A. Rueda, R. Ruffini
Figure caption: Scheme of the BdHN I, II, and III scenarios, depending upon the pre-SN CO–NS orbital period. We recall that ﹩{P}_{\mathrm{orb},\max }﹩ is the maximum orbital period for the NS companion to reach an instability point of BH formation, given CO and NS masses and SN kinetic energy.
Paper: SOFIA/EXES Observations of Warm H2 at High Spectral Resolution. II. IC 443C, NGC 2071, and 3C 391
Authors: David A. Neufeld, Curtis DeWitt, Pierre Lesaffre, Sylvie Cabrit, Antoine Gusdorf, Le Ngoc Tram, William T. Reach
Figure caption: Spectra obtained toward IC 443C. The average intensity within the 1.″9 × 3.″0 extraction region is plotted in units of erg cm−2 s−1 sr−1/cm−1. Solid curves show the two-Gaussian fits to each line. The dotted green lines show the H2 S(5) line profile, scaled and overplotted in the other panels for comparison. Vertical black lines indicate the velocity centroids for the Gaussian components, with horizontal bars at the bottom indicating the standard errors. The LSR velocity of the source is indicated by the dotted black vertical line.
Paper: SOFIA/EXES Observations of Warm H2 at High Spectral Resolution. II. IC 443C, NGC 2071, and 3C 391
Authors: David A. Neufeld, Curtis DeWitt, Pierre Lesaffre, Sylvie Cabrit, Antoine Gusdorf, Le Ngoc Tram, William T. Reach
Figure caption: Results obtained for IC 443C. Top two panels: T  XY , the temperature derived from the relative populations in the H2 J = X and Y states. Next two panels: OPR XYZ , the ortho-to-para ratio derived from the relative populations in the H2 J = X, Y, and Z states. Bottom panels: scaled spectra, rebinned to 2 km s−1 resolution, with the same color coding as in Figures 4–6.
Paper: Constraints on Interacting Dark Energy Models from the DESI Baryon Acoustic Oscillation and DES Supernovae Data
Authors: Tian-Nuo Li, Peng-Ju Wu, Guo-Hong Du, Shang-Jie Jin, Hai-Li Li, Jing-Fei Zhang, Xin Zhang
Figure caption: Best-fit predictions for distance–redshift relations for ΛCDM (solid line), IΛCDM1 (dotted–dashed line), and IΛCDM2 (dashed line) obtained from the analysis of CMB+DESI data. For visual clarity and to compress the dynamic range of the plot, we applied an arbitrary scaling. The error bars represent ±1σ uncertainties.
Paper: SOFIA/EXES Observations of Warm H2 at High Spectral Resolution. II. IC 443C, NGC 2071, and 3C 391
Authors: David A. Neufeld, Curtis DeWitt, Pierre Lesaffre, Sylvie Cabrit, Antoine Gusdorf, Le Ngoc Tram, William T. Reach
Figure caption: Same as Figure 4, but for 3C 391.
Paper: SOFIA/EXES Observations of Warm H2 at High Spectral Resolution. II. IC 443C, NGC 2071, and 3C 391
Authors: David A. Neufeld, Curtis DeWitt, Pierre Lesaffre, Sylvie Cabrit, Antoine Gusdorf, Le Ngoc Tram, William T. Reach
Figure caption: Slit positions for IC 443C. Grayscale: map of H2 S(5) intensity from Spitzer/IRS (D. A. Neufeld et al. 2007). Colored rectangles: location and orientation of the extracted apertures for SOFIA/EXES observations of H2 S(4) (red), S(5) (green), S(6) (blue), and S(7) (magenta).
Paper: SOFIA/EXES Observations of Warm H2 at High Spectral Resolution. II. IC 443C, NGC 2071, and 3C 391
Authors: David A. Neufeld, Curtis DeWitt, Pierre Lesaffre, Sylvie Cabrit, Antoine Gusdorf, Le Ngoc Tram, William T. Reach
Figure caption: Slit positions for 3C 391. Grayscale: map of H2 S(5) intensity from Spitzer/IRS (D. A. Neufeld et al. 2007). Colored rectangles: location and orientation of the extracted apertures for SOFIA/EXES observations of S(5) (green), S(6) (blue), and S(7) (magenta).
Paper: SOFIA/EXES Observations of Warm H2 at High Spectral Resolution. II. IC 443C, NGC 2071, and 3C 391
Authors: David A. Neufeld, Curtis DeWitt, Pierre Lesaffre, Sylvie Cabrit, Antoine Gusdorf, Le Ngoc Tram, William T. Reach
Figure caption: Slit positions for NGC 2071. Grayscale: map of H2 S(5) intensity from Spitzer/IRS (D. A. Neufeld et al. 2009). Colored rectangles: location and orientation of the extracted apertures for SOFIA/EXES observations of H2 S(4) (red), S(5) (green), S(6) (blue), and S(7) (magenta).
Paper: The Calibrations of the DAMPE γ-Ray Effective Area
Authors: Zhao-Qiang Shen, Wen-Hao Li, Kai-Kai Duan, Wei Jiang, Zun-Lei Xu, Chuan Yue, Xiang Li
Figure caption: Upper panel: the relative rate of change in the HET photon effective area with respect to the reconstructed inclination angle θ (blue points) derived with the data below 5 GeV. The black dotted line is the rate of change only corrected with the energy-dependent factor f(E). Lower panel: the relative rate of change in the HET effective area divided by the relative rate from the factor f(E). The green points and dashed line represent the enhancement correction factor g(E, θ) derived from the simulated photon data between 1.6 and 5 GeV.
Paper: The Calibrations of the DAMPE γ-Ray Effective Area
Authors: Zhao-Qiang Shen, Wen-Hao Li, Kai-Kai Duan, Wei Jiang, Zun-Lei Xu, Chuan Yue, Xiang Li
Figure caption: The relative rate of change in the HET photon effective area (blue points) concerning the reconstructed energy. The red dashed line shows the power-law (PL) model fitted with the points whose reconstructed energies are ≲8 GeV (shaded region). The orange and green points are the expected change rates of HET efficiencies of electron (W.-H. Li et al. 2024) and photon in simulation, respectively.
Paper: The Calibrations of the DAMPE γ-Ray Effective Area
Authors: Zhao-Qiang Shen, Wen-Hao Li, Kai-Kai Duan, Wei Jiang, Zun-Lei Xu, Chuan Yue, Xiang Li
Figure caption: The ratios of the observed high-energy trigger (HET) photon counts to the reference counts in different time bins. The ratios are normalized to 1.0 at the first bin. Different colors represent different energy bins. The dashed lines present the linear models that fit the variations best.
Paper: Gamma-Ray Burst Interaction with the Circumburst Medium: The CBM Phase Following the Prompt Phase in GRBs
Authors: Asaf Pe'er, Felix Ryde
Figure caption: Similar to Figure 1, now showing the density profile after the blast wave crosses the contact discontinuity (CD). Region (1) was not yet reached by the newly formed forward shock, and is thus identical to previous region (c). Region (2) is composed of material from region (c), shocked by the newly formed forward shock. Region (3) is composed of wind material from the progenitor, first shocked by the wind termination shock (region (b) above), then by the GRB blast wave, and a third time by the newly formed reverse shock, hence is denoted by “shocked3 wind.” Region (4) is composed of the same material before being reached by the newly formed reverse shock.
Paper: The Calibrations of the DAMPE γ-Ray Effective Area
Authors: Zhao-Qiang Shen, Wen-Hao Li, Kai-Kai Duan, Wei Jiang, Zun-Lei Xu, Chuan Yue, Xiang Li
Figure caption: The relative rate of change in the HvLET photon effective area (trigger logic ﹩\mathrm{LET}\& \& \bar{\mathrm{HET}}﹩) with respect to the reconstructed energy. The blue points are derived from the observed events. Shown in orange is the expected contribution of the HET photons that do not satisfy the HET logic due to the increasing HET threshold energy. The dotted–dashed line and the color band correspond to the best-fit values and the 1σ uncertainties of the relative decrease rates of the HET effective area, respectively.
Paper: Gamma-Ray Burst Interaction with the Circumburst Medium: The CBM Phase Following the Prompt Phase in GRBs
Authors: Asaf Pe'er, Felix Ryde
Figure caption: Cartoon showing the density profile of a wind bubble as a function of the distance, R, from the central star. The four distinct regimes, marked (a)–(d) are separated by the forward and reverse shocks (FS and RS), as well as the contact discontinuity (CD).
Paper: Gamma-Ray Burst Interaction with the Circumburst Medium: The CBM Phase Following the Prompt Phase in GRBs
Authors: Asaf Pe'er, Felix Ryde
Figure caption: Similar to Figure 1, now showing the density profile after the blast wave crosses the wind’s original reverse shock (RS in Figure 1). Behind the GRB blast wave, is material that was shocked twice: first, by the wind termination shock, and second by the GRB blast wave itself. Hence, it is denoted in the cartoon as the “shocked2 wind.”