adsabs/AstroCLIMB huggingface dataset:
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Angular distribution of outgoing radiation field (upper panel) and total energy outflow (lower panel) at r = 1024rg measured by the beaming factors (see Equation (16b) for definitions) for selected models. In most cases, both the radiation field and total energy outflow are strongly beamed. In the lower panel, the dashed lines are fitted using Equation (7) from A. Sądowski & R. Narayan (2015b) normalized to match models E88-a3 (red line) and E07-a3-DL (black line), respectively.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Density (top panel) and magnitude of outflow velocity (bottom panel) of a super-Eddington accretion disk on large scales, relevant for interpreting observations of LRDs. The gray lines represent the scattering photosphere. The red, yellow, green, and blue lines represent the isothermal contours of the logarithmic gas temperature in Kelvin, with values of 7.3, 7.0, 6.6, and 6.3, respectively.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Amplitude of luminosity variability (defined as the rms deviation divided by the mean) vs. total output radiation luminosity for all our models. Both quantities are measured at three different radial locations denoted by the blue, orange, and red symbols. The dotted horizontal line marks a 10% variability threshold. Due to the very low radiative efficiencies, even the most super-Eddington accretion flows only emit ≲10LEdd. Models with the double-loop magnetic field geometry produce the highest variability.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Time component of the jet four-velocity. The jet profile is temporally and azimuthally averaged. The four-velocity is spatially averaged using the density weighting along the jet spine.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Ratio of gas temperature to effective temperature of the radiation field along the scattering photosphere for selected models.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Radiation efficiency vs. mass accretion rate for all models. The dashed line shows the trend predicted by analytical models of super-Eddington accretion (e.g., Equation (6) in J. Poutanen et al. 2007), normalized to match our model E9-a3.
Paper: Simulation of the 2010 September 9 Solar Energetic Particle Event by Using a Data-constrained Transport Model
Authors: Xinyi Tao, Fang Shen, Xueshang Feng, Wanyi Lian, Bofeng Tang, Yi Yang
Figure caption: Overview of the SEP event on 2010 September 9. (a): longitudinal configuration of STB (blue filled circle), Earth (green filled circle), and STA (red filled circle) viewed from the north pole of the Sun at 23:26 UT on September 8, plotted in the HEE coordinate; the black curves present the Parker spiral to illustrate the solar rotation and the cyan arrow indicates the position of CME eruption for this event. (b): CME white-light image captured by the SECCHI/COR1 coronagraph of STB at 23:46 UT, colored by the white-light intensity difference in post-eruption compared with pre-eruption periods. (c): energetic proton measurements from STB/LET and STB/HET. (d): CME white-light image captured by the SECCHI/COR1 coronagraph of STA at 23:45 UT. (e): energetic proton measurements from STA/LET and STA/HET. (f): CME white-light image captured by the LASCO/C2 coronagraph of SOHO at 23:48 UT. (g): energetic proton measurements from SOHO/ERNE.
Paper: Simulation of the 2010 September 9 Solar Energetic Particle Event by Using a Data-constrained Transport Model
Authors: Xinyi Tao, Fang Shen, Xueshang Feng, Wanyi Lian, Bofeng Tang, Yi Yang
Figure caption: (a): prediction of solar wind configuration at 23:26 UT on September 8 from the analytical model; the red, green, and blue filled circles respectively refer to the positions of STA, Earth, and STB in the HEE coordinate; the black curves with arrows indicate the magnetic field lines. (b)–(d): hourly measurement data (solid lines) obtained from STA, WIND and STB respectively during the period from 23:00 UT on September 8 to 06:00 UT on September 11 and the predicted results (dashed–dotted lines) from the solar wind model; shown in the panel are, respectively, the radial component of solar wind velocity Vr, solar wind proton number density Np, proton temperature Tp, magnetic field components Br, Bϕ, and magnetic field strength B, while the line segments are discontinuous owing to missing data.
Paper: Searching for Stellar-feedback-driven Outflow Signatures: A Deep Dive into NGC 3741
Authors: Lexi N. Gault, Liese van Zee, Elizabeth A. K. Adams, James M. Wells, Laura Congreve Hunter, Kristen B. W. McQuinn, Roger E. Cohen, O. Grace Telford
Figure caption: Mass-loading factor as a function of SFR in log space. Comparison galaxies from A. Marasco et al. (2023) are shown in black (circles), and K. B. W. McQuinn et al. (2019) are shown in cyan (diamonds). The blue dashed line shows the best-fit linear relation from A. Marasco et al. (2023), with the blue shaded region showing the intrinsic scatter. LSB Hα emission regions are shown in red (triangles), HSB Hα emission regions are shown in orange (upside-down triangles), SFH regions are shown in green (squares), and the global value for NGC 3741 is shown in pink (star). The SFR(Hα) measurements are lower limits, resulting in higher mass-loading factors when compared to those calculated with more reliable star formation tracers.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Histograms of LAGN, Ldust, Lstellar, and SFR estimates for subsamples of each AGN selection method. Median values of each distribution are shown by the dashed lines. The SFR histograms (bottom right) are the logarithmic Bayesian estimated from X-CIGALE for the SFR averaged over 100 Myr. The mean uncertainties for log LAGN, log Ldust, log Lstellar, and log SFR are 0.85, 0.05 , 0.04, and 0.31, respectively.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: t-SNE clustering with a perplexity of 20, colored by AGN selection method (top) and after rebinning them into clusters (bottom).
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Top: mass distribution of the BPT-selected subsample in comparison to the mass distribution of the remaining objects in the database not selected by that method (gray). Bottom: same plot now separating out the IR-selected subsample from the remaining database.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: SED models for NSA 18993 (top) and NSA 77755 (bottom). NSA 18993 was selected as an AGN via the BPT and [He II] diagrams, as a Seyfert on the [S II] diagram, and from its broad Hα and X-ray emissions. In contrast, NSA 77755 was only selected based on optical variability.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: The cumulative fraction of objects selected as a function of the host galaxy’s stellar mass for each subsample identified in W24.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: H–He ﹩\dot{M}﹩ grids for low and high fluxes—2D linearly interpolated grid of 663 H–He planets located at 0.05 au around a solar-mass, solar-luminosity star. Fluxes correspond to an old star (FXUV ≈ 10−6F*) of 1095 erg s−1 cm−2 (left column) and a younger star (FXUV ≈ 10−4F*) of 109,500 erg s−1 cm−2 (right column). Locations of a Neptune analog and an HD 209458 b analog are plotted as blue and orange points, respectively. The grayed-out region represents where conductive cooling—which we do not model—would be significant. The hatched region represents planets for which Rsp ≤ RHill (see Section 5.2). The top row is color-mapped to the log of the mass-loss rate in g s−1, and the bottom row to the log of the ratio of ﹩\dot{M}﹩ with the tidally corrected energy-limited ﹩\dot{M}({R}_{P})﹩ (Equation (20)) with efficiencies calculated on a point-by-point basis in the grid (low-flux ﹩\left\langle \varepsilon \right\rangle \approx 0.37﹩, high-flux ﹩\left\langle \varepsilon \right\rangle \approx 0.33﹩). See Section 5.1 for a discussion of the bifurcation near 0.1MJ in the high-flux grids.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: H–He ﹩\dot{M}﹩ relative to energy-limited mass-loss rates. (a) Lower flux (1095 erg s−1 cm−2) fractional difference (﹩\dot{M}-{\dot{M}}_{{\rm{tidal}}}({R}_{P}))/{\dot{M}}_{{\rm{tidal}}}({R}_{P})﹩, from tidally corrected energy-limited mass-loss rate computed at RP. We use the same grid as in Figure 9. Orange and blue circles correspond to an HD 209458 b analog and Neptune analog, respectively. Red indicates that ﹩{\dot{M}}_{{\rm{tidal}}}﹩ underestimates the mass-loss rate computed by our model, and blue indicates that ﹩\dot{M}﹩ is less than the energy limit, as is expected. (b) Same color-bar scaling as in panel (a), but here we plot ﹩(\dot{M}-{\dot{M}}_{{\rm{tidal}}}({R}_{{\rm{XUV}}}))/{\dot{M}}_{{\rm{tidal}}}({R}_{{\rm{XUV}}})﹩à. (c) Height of the sonic point above RP in units of RP. All Rsp are below the Hill radii, except at the lowest escape velocity edge (off the left edge of the panel), where the outflow transitions to boil-off or core-powered mass loss—evaluation of our code’s performance in this regime is beyond the scope of this work.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: Hot Jupiter, Neptune, and mini-Neptune H–He outflows—wind structure of H–He (0.8:0.2 mass fraction) atmospheres for a 0.7MJ, 1.4RJ (222.6 M⊕, 15.7 R⊕) planet (orange) with escape velocity at RP of vesc = 4.6 × 106 cm s−1; a Neptune-sized 17 M⊕, 3.9 R⊕ planet (blue) with vesc = 2.4 × 106 cm s−1; and a mini-Neptune with 5 M⊕, 2 R⊕ (green), and vesc = 1.77 × 106 cm s−2. All three are located at 0.05 au around a 1 M⊙ and 1 L⊙ star, with total flux at 0.05 au of Ftot = 1095 erg s−1 cm−2 (13.6–2000 eV). All are plotted in terms of their RP, but all have different RP values. The super-Earth’s small thermal inversion below the wind (where larger planets have an isotherm) is the result of bolometric heating/cooling naturally falling off before photoionization heating becomes significant and the wind launches.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: Metals WASP-121b (C. Huang et al. 2023)—WASP-121b: 1.18MJ, 1.77RJ, 0.03 au, 1.35 M⊙, 2.6 L⊙, Ftot = 6.66 × 104  erg s−1 cm−2. Case B (C. Huang et al. 2023, Figure 20) with solar abundances of H I, He I, C I, N I, O I, S I, Mg II, Si II, Ca II, Fe II, K I, and Na I is reproduced in black. Wind-AE models for solar abundances of all of the above species except Fe II, K I, and Na I using our lower BCs (green) and matching BCs (blue) of ﹩{R}_{{\rm{\min }}}=1.24﹩ and ﹩\rho ({R}_{{\rm{\min }}})=1.39\times 1{0}^{-11}﹩ g cm−3 are plotted. Both also have the same input stellar spectrum as the black solution does.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: HD 209458 b H–He comparisons with ATES and p-winds—Wind-AE H–He (black), ATES H–He (blue, A. Caldiroli et al. 2022), and p-winds pure-H (orange; L. A. Dos Santos et al. 2022) profiles for HD 209458 b. Inputs to p-winds are T = 8616 and ﹩\dot{M}=1.57\times 1{0}^{10}﹩ g s−1 (the ﹩\dot{{M}_{/4}}﹩ computed by Wind-AE). Sonic points are plotted as dashed vertical lines, and the Hill radius is plotted as a dotted vertical line. All three employ different approximations to solar spectra.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: Profiles for planets in the high X-ray flux limit—reproduction of Figure 4 in J. E. Owen & A. P. Jackson (2012; black), a model that does not contain PdV or Lyα cooling. Density, velocity, and temperature results are given for a 1MJ, 1.73RJ (dark) and 5RJ (light) planet at 0.1 au irradiated by a 1 M⊙ star with X-ray luminosity LX = 1030 erg s−1 cm−2. Wind-AE profiles are plotted for planets with physical BCs (green) and BCs that match the BCs of the black solution (cyan). To match LX = 1030 ergs cm−2, our planets are irradiated by a scaled solar spectrum of total flux 13.6–2000 eV of 3.57 × 105 erg s−1 cm−2. Sonic points are plotted as dashed vertical lines.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: HD 209458 b pure H (A. García Muñoz 2007). We reproduce the SP solution of Figures 3–4 in A. García Muñoz (2007) for an EUV-irradiated pure-H atmosphere (black). The Wind-AE solution plotted (cyan) is for a pure-H atmosphere with no Lyα cooling, a similar if not identical high-activity solar spectrum (Ftot = 2474 erg s−1 cm−2 integrated over 13.6–165 eV, which loosely simulates H3+ cooling), and BCs matched to those of the black solution (﹩{R}_{{\rm{\min }}}﹩ = 1.03 RP, T = 730 K, ρ = 5.82 × 10−13 g cm−3). Sonic points are dashed lines, and the solid gray region is the Coriolis radius past which our model is not valid.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: H–He GJ 1214 b CHAIN and TPCI models—GJ 1214 b: 6.36 M⊕, 2.69 R⊕, 0.014 au, 0.18 M⊙, 3.51 × 10−3L⊙, 886 erg s−1 cm−2. The D. Kubyshkina & L. Fossati (2022) CHAIN solar spectrum solution (cyan) and M. Salz et al. (2016) TPCI solution (magenta) are reproduced here.
Paper: Wind-AE: A Fast, Open-source 1D Photoevaporation Code with Metal and Multifrequency X-Ray Capabilities
Authors: Madelyn I. Broome, Ruth Murray-Clay, John R. McCann, James E. Owen
Figure caption: Pure-H HD 209458 b TPCI model (M. Salz et al. 2016; TPCI, magenta), with lower BCs of ﹩T({R}_{{\rm{\min }}})=1000﹩ K, ﹩{R}_{{\rm{\min }}}\sim 1.05{R}_{P}﹩, ﹩\rho ({R}_{\min })\sim 1.6\times 1{0}^{-9}\,{\rm{g}}\,{\mathrm{cm}}^{-3}﹩. We have confirmed that these boundary conditions are not the source of the profile differences.
Paper: Measurement and Modeling of Electron Temperature in Laboratory Photoionized Plasmas Relevant to Astrophysics
Authors: J. J. Rowland, R. C. Mancini, G. S. Jaar, D. C. Mayes, H. Scott, I. E. Golovkin, M. Chatzikos, G. Ferland, G. P. Loisel, J. E. Bailey
Figure caption: Electron temperature as a function of time modeled with steady-state Cloudy (black dot trace) and time-dependent Cloudy (orange solid trace) for neon atom densities of (a) 2.5 × 1017 cm−3, (b) 5 × 1017 cm−3, and (c) 1018 cm−3, and associated ionization parameter values of ξ = 37.1 ± 7.0 erg cm s−1, ξ = 19.1 ± 2.8 erg cm s−1, ξ = 9.5 ± 1.2 erg cm s−1, respectively (D. C. Mayes et al. 2021). The shaded region represents ±1 standard deviation of time-dependent Cloudy calculations performed for different spectral energy distributions of the X-ray flux, but all with the same photon-energy integrated time history. Experimental measurements are displayed as well. Also shown is the time history of the photon-energy integrated X-ray flux (blue dotted–dashed trace), which is the same for all neon density cases.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Poloidal slices of the mass density in radiation-dominated disks with the same black hole spin but different mass accretion rates. The left column corresponds to a model with ﹩{\dot{M}}_{3}=88{\dot{M}}_{{\rm{Edd}}}﹩ (E88-a3), the middle column ﹩{\dot{M}}_{3}=0.8{\dot{M}}_{{\rm{Edd}}}﹩ (E08-a3), and the right column ﹩{\dot{M}}_{3}=0.1{\dot{M}}_{{\rm{Edd}}}﹩ (E01-a3). The bottom row is a zoom-in to the inner regions. Each model is shown at t = 60000rg/c once a steady state has been reached. The blue contour marks regions within the photosphere where the magnetic pressure is twice the thermal pressure, indicating magnetically dominated zones.
Paper: Measurement and Modeling of Electron Temperature in Laboratory Photoionized Plasmas Relevant to Astrophysics
Authors: J. J. Rowland, R. C. Mancini, G. S. Jaar, D. C. Mayes, H. Scott, I. E. Golovkin, M. Chatzikos, G. Ferland, G. P. Loisel, J. E. Bailey
Figure caption: Electron temperature as a function of time modeled with time-dependent Cloudy (orange solid trace, same as in Figure 4) for neon atom densities of (a) 2.5 × 1017 cm−3, (b) 5 × 1017 cm−3, and (c) 1018 cm−3. The shaded region represents ±1 standard deviation of time-dependent Cloudy calculations performed for different spectral energy distributions, but all with the same photon-energy integrated time history. Also shown are the results from HeliosCR radiation-hydrodynamics (red solid trace) and time-dependent Cretin (purple solid trace, same as in Figure 5). Experimental measurements are displayed as well.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Disk, wind, and jet regions that emerge in our radiation-dominated disk models. The upper panels illustrate the super-Eddington case ﹩{\dot{M}}_{3}=88{\dot{M}}_{{\rm{Edd}}}﹩ (E88-a3), while the lower panels show a near-Eddington case ﹩{\dot{M}}_{3}=0.8{\dot{M}}_{{\rm{Edd}}}﹩ (E08-a3). Colors show the local flux-mean optical depth per gravitational radius. The blue streamlines show the gas velocity. The cyan dashed lines mark the contour of zero Bernoulli parameter: regions inside this contour are gravitationally bound. The orange dashed lines outline the jet zone, defined by the outermost velocity streamline that originates from the strongly magnetized inner region where magnetic energy equals rest-mass energy.
Paper: Measurement and Modeling of Electron Temperature in Laboratory Photoionized Plasmas Relevant to Astrophysics
Authors: J. J. Rowland, R. C. Mancini, G. S. Jaar, D. C. Mayes, H. Scott, I. E. Golovkin, M. Chatzikos, G. Ferland, G. P. Loisel, J. E. Bailey
Figure caption: Electron temperature as a function of time modeled with steady-state Cretin (black dot trace) and time-dependent Cretin (purple solid trace) for neon atom densities of (a) 2.5 × 1017 cm−3, (b) 5 × 1017 cm−3, and (c) 1018 cm−3. Experimental measurements are displayed as well. Also shown is the time history of the photon-energy integrated X-ray flux (blue dotted–dashed trace, same as in Figure 4), which is the same for all neon density cases.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Time evolution of mass accretion rate and normalized magnetic flux at r = 3rg (see Equation (5b)). In the lower panels, the black lines represent comparison simulations without radiation, with solid lines indicating low spin (a = 0.3) and dashed lines indicating high spin (a = 0.9375). The gray shaded regions indicate the time windows used for time-averaged analysis of the steady-state structure.
Paper: Measurement and Modeling of Electron Temperature in Laboratory Photoionized Plasmas Relevant to Astrophysics
Authors: J. J. Rowland, R. C. Mancini, G. S. Jaar, D. C. Mayes, H. Scott, I. E. Golovkin, M. Chatzikos, G. Ferland, G. P. Loisel, J. E. Bailey
Figure caption: Electron temperature Te spatial profile for t = 100 ns predicted by HeliosCR for the P = 15 Torr case (neon atom number density 5 × 1017 cm−3) showing all regions in the simulation, namely front and rear windows and neon gas.
Paper: Radiation GRMHD Models of Accretion onto Stellar-mass Black Holes. I. Survey of Eddington Ratios
Authors: Lizhong Zhang, 张 力 中, James M. Stone, Patrick D. Mullen, Shane W. Davis, Yan-Fei Jiang, 姜 燕 飞, Christopher J. White
Figure caption: Density (colors) and magnetic field (blue streamlines) in the initial conditions for the single-loop (left) and double-loop (right) magnetic configurations.
Paper: Simulation of the 2010 September 9 Solar Energetic Particle Event by Using a Data-constrained Transport Model
Authors: Xinyi Tao, Fang Shen, Xueshang Feng, Wanyi Lian, Bofeng Tang, Yi Yang
Figure caption: Longitudinal distributions of (a) normal component of upstream solar wind velocity V1n, (b) shock obliquity angle θBn, and (c) shock compression ratio R at different moments after the CME initialization. The black dashed line denotes the HEE longitude of the shock apex. α and β, respectively, indicate the two flanks of the shock front, corresponding to the marks in Figure 4.
Paper: Simulation of the 2010 September 9 Solar Energetic Particle Event by Using a Data-constrained Transport Model
Authors: Xinyi Tao, Fang Shen, Xueshang Feng, Wanyi Lian, Bofeng Tang, Yi Yang
Figure caption: CME-driven shock front (cyan curve) at different moments since CME initialization in the HEE coordinate. The black curves present the interplanetary magnetic field lines connecting to STA (red filled circle), Earth (green filled circle), and STB (blue filled circle), as obtained from the solar wind model. The angle between the two black dashed lines refers to the angular size of the shock front. α and β indicate the two flanks of the shock front, respectively.