adsabs/AstroCLIMB huggingface dataset:
Paper: The Potential of Asteroseismology to Resolve the Blue Supergiant Problem
Authors: Earl Patrick Bellinger, Selma E. de Mink, Walter E. van Rossem, Stephen Justham
Figure caption: (Left) Radial and nonradial oscillation mode frequencies for the BSG models shown in Figure 5, plotted as a function of the radial order. By convention, g-dominated modes have n < 0. (Right) Period spacings for the g-mode frequencies of these models from GYRE, shown in comparison with the asymptotic value. Note that most of the dipole modes are mixed modes. The extended MS model has a period spacing of ∼300 min, while the others have period spacings of ∼30 min.
Paper: The Potential of Asteroseismology to Resolve the Blue Supergiant Problem
Authors: Earl Patrick Bellinger, Selma E. de Mink, Walter E. van Rossem, Stephen Justham
Figure caption: The same as Figure 6, now shown in terms of fractional radius. Here contours of constant radius are also shown for 0.1 R ⊙.
Paper: High-resolution Pan-STARRS and SMA Observations of IRAS 23077+6707: A Giant Edge-on Protoplanetary Disk
Authors: Kristina Monsch, Joshua Bennett Lovell, Ciprian T. Berghea, Gordian Edenhofer, Garrett K. Keating, Sean M. Andrews, Ammar Bayyari, Jeremy J. Drake, David J. Wilner
Figure caption: Radial intensity profiles of IRAS 23077+6707 computed along the disk major axis (midplane). Left: PS1 i- (red), r- (orange), and g-band (green) data. Each line was normalized to the peak of the g-band profile. Right: 1.3 mm continuum (gray), 12CO (dark blue), 13CO (mid blue), C18O (light blue). By fitting 1D Gaussian models to each radial profile (with the instrumental FWHMs shown in the upper left), we estimate physical scales on which the disk emission can arise.
Paper: High-resolution Pan-STARRS and SMA Observations of IRAS 23077+6707: A Giant Edge-on Protoplanetary Disk
Authors: Kristina Monsch, Joshua Bennett Lovell, Ciprian T. Berghea, Gordian Edenhofer, Garrett K. Keating, Sean M. Andrews, Ammar Bayyari, Jeremy J. Drake, David J. Wilner
Figure caption: Calculation of IRAS 23077+6707's brightness asymmetries in scattered light. Left: A ∼ 50″ × 50″ cutout (rotated by 22° counterclockwise) of the PS1 g-band filter, where the white box highlights the region in which the intensity profiles were computed. Right: emission profiles for the PS1 i (solid red), r (dashed green) and g (dashed–dotted blue line) filters. Each line corresponds to the mean intensity profiles of the full disk (i.e., averaged along all pixel lanes perpendicular to the disk midplane), which were additionally normalized to their corresponding maximum and subsequently centered on the disk’s midplane (black dotted line). The upper and lower bounds of each shaded region encompass the mean profiles of the southern and northern disk halves, respectively.
Paper: The Potential of Asteroseismology to Resolve the Blue Supergiant Problem
Authors: Earl Patrick Bellinger, Selma E. de Mink, Walter E. van Rossem, Stephen Justham
Figure caption: H-R diagrams for scenarios resulting in BSGs: classical HG stars (top left panel), extended MS stars (top right panel), blue loop stars (bottom left panel) and Case B binary mergers (bottom right panel). The tracks are of 10−20 M⊙ and are computed until core-He exhaustion. The tracks are colored by their “velocity” in the H-R diagram (Equation (1)), which is a proxy for time spent and hence number of expected stars observed (darker means longer lived and more stars). The higher-mass tracks are the more luminous ones, and evolution generally proceeds from hot to cool. The BSG problem is an observed overdensity of stars in the HG (∼10,000–20,000 K as indicated by the dotted blue box) as isolated stars with normal cores (top left panel) should not numerously populate this region.
Paper: The Potential of Asteroseismology to Resolve the Blue Supergiant Problem
Authors: Earl Patrick Bellinger, Selma E. de Mink, Walter E. van Rossem, Stephen Justham
Figure caption: Asteroseismic characteristics of scenarios resulting in BSGs. Lines show the evolution of the period spacing and high-order radial-oscillation frequencies. The binary-merger models are varied in all input parameters (stellar mass, core mass, mass of the gradient region, and envelope helium abundance). Binary mergers and blue loop stars (ΔΠ ∼ 20 min) can be asteroseismically distinguished from MS stars (ΔΠ ∼ 200 min). These groups can also be distinguished from classical HG stars (dν/dt > 10−2 μHz/yr) on the basis of high-order radial-mode frequency modulation; a star in this mass range with high-order radial-mode frequencies that are stable over >10 yr cannot be undergoing classical HG evolution.
Paper: The Potential of Asteroseismology to Resolve the Blue Supergiant Problem
Authors: Earl Patrick Bellinger, Selma E. de Mink, Walter E. van Rossem, Stephen Justham
Figure caption: Asteroseismic diagnostics for the two main classes of long-lived BSG solutions: H-burning and He-burning stars, shown in the asteroseismic Δν–ΔΠ plane. The large frequency separation Δν is sensitive to the mean density of the star, and the period spacing ΔΠ probes internal chemical composition gradients. The figure is split into four panels representing the four free parameters of the binary-merger model: stellar mass (upper left), envelope helium abundance (upper right), mass of the gradient region (lower left), and core mass (lower right; see Section 2.2 for definitions). Across all variations in input parameters, binary mergers have ﹩{\rm{\Delta }}{\rm{\Pi }}\lt 50\,\min ﹩, and H-core burning stars have ﹩{\rm{\Delta }}{\rm{\Pi }}\gt 100\,\min ﹩. Only long-lived phases of evolution are shown. Evolution generally proceeds from high to low Δν (i.e., right to left), and more massive stars have larger period spacings.
Paper: The Potential of Asteroseismology to Resolve the Blue Supergiant Problem
Authors: Earl Patrick Bellinger, Selma E. de Mink, Walter E. van Rossem, Stephen Justham
Figure caption: Anatomy of our schematic merger models. LEFT PANEL. The initial chemical profile consists of a He core (of variable mass) below an outer envelope (of variable He abundance) separated by a gradient (also of variable mass). MIDDLE PANEL. Internal structure of the model shortly after thermal relaxation. RIGHT PANEL. The state after 0.5 Myr. Most of the center in the core has undergone fusion. Notice that despite an initial gradient, the system evolves to a more step-like profile.
Paper: High-resolution Pan-STARRS and SMA Observations of IRAS 23077+6707: A Giant Edge-on Protoplanetary Disk
Authors: Kristina Monsch, Joshua Bennett Lovell, Ciprian T. Berghea, Gordian Edenhofer, Garrett K. Keating, Sean M. Andrews, Ammar Bayyari, Jeremy J. Drake, David J. Wilner
Figure caption: Comparison of optical scattered-light and (sub)millimeter emission of IRAS 23077+6707. Top left: PS1 irg-composite image, showing the optical scattered-light emission at λ mean = 7545, 6215, and 4866 Å, respectively. Top right: SMA 12CO integrated intensity (or “moment 0”) map, overlaid with its respective contours, as well as the 1.3 mm continuum contours, drawn at the 10%, 30%, 50%, 70%, and 90% levels of their corresponding maximum emission. Bottom left: same for 13CO. Bottom right: same for C18O. In the lower right of each panel, we show 14″ scale bars, and we show the effective CO (black) and continuum (orange) beams in the lower left of the SMA image.
Paper: High-resolution Pan-STARRS and SMA Observations of IRAS 23077+6707: A Giant Edge-on Protoplanetary Disk
Authors: Kristina Monsch, Joshua Bennett Lovell, Ciprian T. Berghea, Gordian Edenhofer, Garrett K. Keating, Sean M. Andrews, Ammar Bayyari, Jeremy J. Drake, David J. Wilner
Figure caption: Line spectra of the 12CO, 13CO, and C18O J = 2 − 1 lines. The line profiles were produced with GoFish (Teague 2019) in a field of view spanning 22″ centered on the respective line emission, where we adopted a disk inclination of 80° and a position angle of PA = 342°. The resulting integrated line fluxes are ﹩{F}_{{}^{12}\mathrm{CO}}=35.4\pm 1.8\,\mathrm{Jy}\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩, ﹩{F}_{{}^{13}\mathrm{CO}}=14.0\pm 0.8\,\mathrm{Jy}\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩, and ﹩{F}_{{{\rm{C}}}^{12}{\rm{O}}}=8.6\pm 0.5\,\mathrm{Jy}\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩. The light blue range highlights the velocity range in which the integrated intensity maps shown in Figure 1 were computed.
Paper: High-resolution Pan-STARRS and SMA Observations of IRAS 23077+6707: A Giant Edge-on Protoplanetary Disk
Authors: Kristina Monsch, Joshua Bennett Lovell, Ciprian T. Berghea, Gordian Edenhofer, Garrett K. Keating, Sean M. Andrews, Ammar Bayyari, Jeremy J. Drake, David J. Wilner
Figure caption: Position–velocity (PV) diagrams obtained for the three CO J = 2 − 1 lines, with 22″ long and 6″ wide cuts, oriented along a position angle of 342° from the image center, referenced to each of their respective line velocity centers.
Paper: An Early Dark Matter–dominated Phase in the Assembly History of Milky Way–mass Galaxies Suggested by the TNG50 Simulation and JWST Observations
Authors: Anna de Graaff, Annalisa Pillepich, Hans-Walter Rix
Figure caption: Redshift evolution of the dark matter fraction within the stellar half-mass radius (TNG50) and the half-light radius (observations). The dark (light) shaded regions indicate the 16th–84th (5th–95th) percentiles of the evolution of TNG50 galaxies selected at z = 6 with 108 M ⊙ < M * < 109 M ⊙. The thick solid line shows the median evolution of f DM(<r e) of the TNG50 galaxies; to bracket possible systematic differences in the comparison to observations, we also show the median evolution of f DM(<0.5r e) (dotted) and f DM(<1.5r e) (dashed). The median evolutionary tracks and data points from high-redshift observations are color-coded by the total stellar mass. Qualitatively, this suggests a link between observations at different mass and redshift epochs and agreement between the TNG50 simulation and observations.
Paper: Inferring the Interstellar Magnetic Field Direction from Energetic Neutral Atom Observations of the Heliotail
Authors: M. Kornbleuth, M. Opher, M. A. Dayeh, J. M. Sokół, Y. Chen, E. Powell, D. L. Turner, I. Baliukin, K. Dialynas, V. Izmodenov
Figure caption: Same as in Figure 2, but with non-normalized ENA flux in units of (cm2 s sr keV)−1. Cases 5–11 all use the same solar wind profile (1995–2017 averaged) and solar magnetic field strength (B  r,SW = 37.5 μG). For Cases 5–8, we vary α  BV  from 60° to 10°. For Cases 9 and 10 we replicate Case 6, but with a lower (B ISM = 2.9 μG) and higher (B ISM = 4.4 μG) interstellar magnetic field intensity, respectively. For Case 11, we also replicate Case 6, but with a higher interstellar plasma density (n  p,ISM) to investigate the effect of higher ISM ram pressure on the lobes.
Paper: What Is the Black Hole Spin in Cyg X-1?
Authors: Andrzej A. Zdziarski, Swadesh Chand, Srimanta Banerjee, Michał Szanecki, Agnieszka Janiuk, Piotr Lubiński, Andrzej Niedźwiecki, Gulab Dewangan, Ranjeev Misra
Figure caption: The count rates and hardness ratios of NICER and NuSTAR. The top two panels show the NICER 0.5–3.0 keV count rate and the (2–4 keV)/(0.5–2.0 keV) count rate ratio. The bottom two panels show the NuSTAR 3–25 keV count rate and the (8–25 keV)/(3–8 keV) count rate ratio. The blue and red symbols correspond to the NuSTAR A and B units, respectively. The zero time corresponds to MJD 58800.42093.
Paper: What Is the Black Hole Spin in Cyg X-1?
Authors: Andrzej A. Zdziarski, Swadesh Chand, Srimanta Banerjee, Michał Szanecki, Agnieszka Janiuk, Piotr Lubiński, Andrzej Niedźwiecki, Gulab Dewangan, Ranjeev Misra
Figure caption: The NICER (red), NuSTAR (black and blue), and INTEGRAL (magenta) unfolded spectra (top panel) and data-to-model ratios (bottom panel) for (a) Model 1 and (b) Model 4. The spectra are normalized to NuSTAR A. The total model spectrum and the unabsorbed one are shown by the solid black and blue curves, respectively. The unabsorbed disk, scattered, reflected, and narrow Fe Kα components are shown by the magenta, green, red, and cyan curves, respectively. In panel (a) the brown curve shows the disk spectrum scattered by the thermal electron component of the hybrid distribution, and in panel (b) it shows the underlying disk spectrum before going through the Comptonization top layer.
Paper: What Is the Black Hole Spin in Cyg X-1?
Authors: Andrzej A. Zdziarski, Swadesh Chand, Srimanta Banerjee, Michał Szanecki, Agnieszka Janiuk, Piotr Lubiński, Andrzej Niedźwiecki, Gulab Dewangan, Ranjeev Misra
Figure caption: (a) Monitoring daily light curves around the studied observation normalized to the hard-state averages (dotted line). The magenta bars show the durations of the NICER/NuSTAR and INTEGRAL observations. The blue, red, and black symbols show the fluxes from MAXI (2–20 keV, 〈F〉 = 1.0 cm−2 s−1), BAT (15–50 keV, 〈F〉 = 0.17 cm−2 s−1), and AMI-LA (15 GHz, 〈F〉 = 12.7 mJy), respectively. (b) The 2–10 keV photon spectral index estimated from the MAXI count rates.
Paper: What Is the Black Hole Spin in Cyg X-1?
Authors: Andrzej A. Zdziarski, Swadesh Chand, Srimanta Banerjee, Michał Szanecki, Agnieszka Janiuk, Piotr Lubiński, Andrzej Niedźwiecki, Gulab Dewangan, Ranjeev Misra
Figure caption: Correlations between selected parameters obtained by MCMC for Model 1 (left) and Model 4 (right). We show the median values by the middle dashed lines in the distribution panels, and the surrounding dashed lines correspond to the 90% uncertainty. The corresponding numerical values are given above the posterior distributions (and may be different from those in Table 3, which give the values based on χ 2).
Paper: What Is the Black Hole Spin in Cyg X-1?
Authors: Andrzej A. Zdziarski, Swadesh Chand, Srimanta Banerjee, Michał Szanecki, Agnieszka Janiuk, Piotr Lubiński, Andrzej Niedźwiecki, Gulab Dewangan, Ranjeev Misra
Figure caption: The rms vs. photon energy for the frequency range of 0.01–1 Hz. The lower values for NuSTAR (red) than for NICER (magenta) in the overlapping energy range are due to the dead time of NuSTAR.
Paper: What Is the Black Hole Spin in Cyg X-1?
Authors: Andrzej A. Zdziarski, Swadesh Chand, Srimanta Banerjee, Michał Szanecki, Agnieszka Janiuk, Piotr Lubiński, Andrzej Niedźwiecki, Gulab Dewangan, Ranjeev Misra
Figure caption: The power spectra from NICER, 0.34–2.0 keV (magenta circles), and the co-spectra from NuSTAR, 5–30 keV (red circles).
Paper: What Is the Black Hole Spin in Cyg X-1?
Authors: Andrzej A. Zdziarski, Swadesh Chand, Srimanta Banerjee, Michał Szanecki, Agnieszka Janiuk, Piotr Lubiński, Andrzej Niedźwiecki, Gulab Dewangan, Ranjeev Misra
Figure caption: The residuals to the fit with absorbed relativistic disk and a Comptonization tail (modeled by simpl) to the NICER (red), NuSTAR (black and blue), and INTEGRAL (magenta) data. Canonical reflection features are seen.
Paper: Resonance of Low-frequency Electromagnetic and Ion-sound Modes in the Solar Wind
Authors: I. Y. Vasko, F. S. Mozer, T. Bowen, J. Verniero, X. An, A. V. Artemyev, S. D. Bale, J. W. Bonnell, J. Halekas, I. V. Kuzichev
Figure caption: Panels (a) and (b) present linear dispersion curves of fast, intermediate, and slow modes obtained using Hall-MHD approximation for the case of oblique propagation at the wave normal angle of θ = 5° in a warm plasma with β  e  = β  i  = 1, and polytrope indexes of electrons and ions of γ  e  = 1 and γ  i  = 3. Both panels also demonstrate dispersion curves of fast magnetosonic and Alfvén ion-cyclotron modes in cold plasma. Panel (c) presents the coordinate system XYZ used for PSP observations in Section 1: the Z-axis is directed radially toward the Sun and basically parallel to the background magnetic field (Figure 1). Panel (c) also presents the coordinate system xyz used for numerical simulations in Section 4: the z-axis is along the propagation direction ﹩\hat{{\boldsymbol{k}}}﹩ of the low-frequency electromagnetic fluctuations. The magenta dots in panel (b) correspond to fast magnetosonic waves, whose nonlinear evolution is demonstrated in Figure 5.
Paper: Resonance of Low-frequency Electromagnetic and Ion-sound Modes in the Solar Wind
Authors: I. Y. Vasko, F. S. Mozer, T. Bowen, J. Verniero, X. An, A. V. Artemyev, S. D. Bale, J. W. Bonnell, J. Halekas, I. V. Kuzichev
Figure caption: The results of Hall-MHD simulations of the nonlinear evolution of initially monochromatic fast magnetosonic waves, propagating at θ = 5° to the background magnetic field in a warm plasma with β  e  = β  i  = 1. The initial wavenumbers of the fast magnetosonic waves are indicated in the panels as well as in Figure 4. For each simulation run the panels demonstrate evolution (in the frame of the wave) of the plasma density N/N 0, compressible component V ∣∣/v  A  of the plasma flow velocity, electrostatic field E ∣∣/v  A  B 0 parallel to the propagation direction, and the magnetic field  B /B 0.
Paper: Cannibals in PARADISE: The Effect of Merging Interplanetary Shocks on Solar Energetic Particle Events
Authors: Antonio Niemela, Nicolas Wijsen, Angels Aran, Luciano Rodriguez, Jasmina Magdalenic, Stefaan Poedts
Figure caption: PARADISE simulation results for the three EUHFORIA simulations (different rows) at 0.3 au (panels (a), (d), and (g)), 0.7 au (panels (b), (e), and (h)), and 1 au (panels (c), (f), and (i)). Each panel consists of omnidirectional intensity–time profiles (top) and first-order parallel anisotropy–time profiles (bottom). Low-, mid-, and high-energy anisotropy–time profiles are calculated using the lowest four, middle four, and highest four energy channels, respectively. Vertical shaded areas correspond to a time window of ±30 minutes around the modeled shock.
Paper: Cannibals in PARADISE: The Effect of Merging Interplanetary Shocks on Solar Energetic Particle Events
Authors: Antonio Niemela, Nicolas Wijsen, Angels Aran, Luciano Rodriguez, Jasmina Magdalenic, Stefaan Poedts
Figure caption: PARADISE complementary simulation results using the background solar wind with both CMEs injected. Panels (a) (at 0.3 au), (b) (at 0.7 au), and (c) (at 1 au) show the resulting intensity– and anisotropy–time profiles when injecting only at the slower CME-driven shock position. Panels (d) (at 0.3 au), (e) (at 0.7 au), and (f) (at 1 au) show the results when injecting only at the faster CME-driven shock position. Each panel consists of omnidirectional intensity–time profiles (top panel) and first-order parallel anisotropy–time profiles (bottom panel). Low-, mid-, and high-energy anisotropy–time profiles are calculated using the lowest four, middle four, and highest four energy channels, respectively. Vertical shaded areas correspond to a time window of ±30 minutes centered at the time of the switch in the low-energy anisotropy sign, which, approximately, represents the time of the shock passage.
Paper: Cannibals in PARADISE: The Effect of Merging Interplanetary Shocks on Solar Energetic Particle Events
Authors: Antonio Niemela, Nicolas Wijsen, Angels Aran, Luciano Rodriguez, Jasmina Magdalenic, Stefaan Poedts
Figure caption: Visualization of the position of the shocks detected by the automatic shock-tracing algorithm, corresponding to panel (c) of Figure 1. The position of the Earth (not to scale) is marked with a green sphere, while the Sun is represented with a gray sphere. The gray sphere represents the inner boundary of EUHFORIA. (a) Rear view. (b) Front view.
Paper: The Dependence of Gamma-Ray Burst Jet Collimation on Black Hole Spin
Authors: Valeria U. Hurtado, Nicole M. Lloyd-Ronning, Jonah M. Miller
Figure caption: Plots of 3D simulation sigma (σ) analysis at different times of the simulation. Each plot is a snapshot in time of σ for the case of five different BH spins. The navy curve corresponds to the BH of spin 0.4, the teal to a BH of spin 0.5, the yellow curve to the BH of spin 0.7, the brown to a BH of spin 0.85, and the purple line to the BH of spin 0.99. The top-left plot is at the earliest time, and the bottom-right is at a later time in the simulation. This plot indicates the trend that a more highly spinning BH leads to a narrower jet opening angle and vice versa.
Paper: The Dependence of Gamma-Ray Burst Jet Collimation on Black Hole Spin
Authors: Valeria U. Hurtado, Nicole M. Lloyd-Ronning, Jonah M. Miller
Figure caption: 3D simulations of the BH–accretion disk jet system, all at times 5500 MBH out of 10,000 MBH. On the top is a BH with spin 0.5 (lower spin fraction), in the middle is a BH of spin 0.7, and on the bottom is a BH of spin 0.99 (highest spin fraction). β > 1 indicates material dominated by gas pressure (accretion disk in yellow/orange) and β < 1 indicated material dominated by magnetic field energy (jet, pink/purple).
Paper: The Dependence of Gamma-Ray Burst Jet Collimation on Black Hole Spin
Authors: Valeria U. Hurtado, Nicole M. Lloyd-Ronning, Jonah M. Miller
Figure caption: 3D simulations showing a plot of density for three simulation runs, all at time 5500 MBH out of 10,000 MBH. On the top is the simulation corresponding to a BH of spin 0.5, in the middle is a BH of spin 0.7, and on the bottom a BH of spin 0.99. All simulations show a frontal view of the black hole–accretion disk jet (bhadj) system. The blue and purple hues correspond to the least dense material (jet) in the system, while green and yellow hues to the densest (accretion disk).
Paper: A Relativistic Formula for the Multiple Scattering of Photons
Authors: Rohta Takahashi, Masayuki Umemura, Ken Ohsuga, Yuta Asahina, Rintaro Takeda, Mikiya M. Takahashi, Norita Kawanaka, Kohkichi Konno, Tomoaki Nagasawa
Figure caption: The probability density function P(t *, r *) of scattering photons in the laboratory frame of a relativistic flow with Γβ = 0.0 (the first column), 0.1 (the second column), and 1.0 (the third column) at the time t * = 0.001, 1.0, 10.0, 100.0, and 1000.0 (from left to right). In each plot, the abscissa and the ordinate represent x *-axis and z *-axis, respectively, and the outermost circle (dotted circle) shows the location of r * = t *. The symbols (F, B, I, D, D2) at the bottom-right corner of each plot represents the state of the scattering photons (see the text). The maximum and minimum values, ﹩{P}_{\max }﹩ and ﹩{P}_{\min }﹩, of the color bar are set to show the distribution of the probability density function. The circle with the radius of ﹩\sqrt{{t}_{* }}﹩ and the center at (x *, z *) = (0, β t *) are shown at the time t * = 10.0, 100.0, and 1000.0 (white dotted circle).
Paper: A Relativistic Formula for the Multiple Scattering of Photons
Authors: Rohta Takahashi, Masayuki Umemura, Ken Ohsuga, Yuta Asahina, Rintaro Takeda, Mikiya M. Takahashi, Norita Kawanaka, Kohkichi Konno, Tomoaki Nagasawa
Figure caption: The time evolution of the mean radial distance ﹩{\overline{r}}_{* }﹩ of the probability distribution of the scattering photons in the laboratory frame of the fluid with Γβ = 0.0, 10−4, 10−3, 10−2, 0.1, 1.0, and 10 (from top to bottom). The results of the formula (solid line) and the MC simulations (blank circle) are shown. The formula representing the state of the scattering photons are shown: ﹩{\overline{r}}_{* }\sim {t}_{* }﹩ (isotropic free-streaming or anisotropic ballistic motion), ﹩{\overline{r}}_{* }\propto \sqrt{{t}_{* }}﹩ (diffusion, i.e., diffusive expansion), and ﹩{\overline{r}}_{* }\sim \beta {t}_{* }+﹩const. (dynamic diffusion, i.e., boosted diffusion).
Paper: A Relativistic Formula for the Multiple Scattering of Photons
Authors: Rohta Takahashi, Masayuki Umemura, Ken Ohsuga, Yuta Asahina, Rintaro Takeda, Mikiya M. Takahashi, Norita Kawanaka, Kohkichi Konno, Tomoaki Nagasawa
Figure caption: The probability density function P(t *, r *) of scattering photons in a static medium at the time t * = 10−3, 10−2.5, 10−2, 10−1.5, 10−1, 10−0.5, 1, 100.5, 10, 101.5, 102, 102.5, 103, 103.5, 104, 104.5, 105, 105.5, 106, 106.5, and 107 (from top to bottom). The results of the formula (solid line) and the Monte Carlo simulations (blank circle) are shown.