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Paper: Applying the Velocity Gradient Technique in NGC 1333: Comparison with Dust Polarization Observations
Authors: Archana Soam, Ka Ho Yuen, Ian Stephens, Chi Yan Law, Ka Wai Ho, Simon Coudé
Figure caption: Left panel: the B-field morphology traced by the SOFIA/HAWC+ 214 μm dust polarization observations of NGC 1333 plotted on the Stokes I total intensity map. The plotted line segments correspond to P/σ  P  > 3, and only one in two vectors is plotted for clarity. Right panel: B-field map obtained from 850 μm polarizations observations plotted on the Stokes I total intensity, as adapted from Y. Doi et al. (2020). Young stellar objects identified by G. Sandell & L. B. G. Knee (2001) are shown in both panels. The SOFIA/HAWC+ and the JCMT/POL-2 beam sizes are shown in the lower-left corner of their respective panels.
Paper: Applying the Velocity Gradient Technique in NGC 1333: Comparison with Dust Polarization Observations
Authors: Archana Soam, Ka Ho Yuen, Ian Stephens, Chi Yan Law, Ka Wai Ho, Simon Coudé
Figure caption: Peak-normalized 12CO spectral line in the form of velocity caustics for the three separate regions. Hinge: blue; Blob: orange; Filament: green, as shown in Figure 2.
Paper: Applying the Velocity Gradient Technique in NGC 1333: Comparison with Dust Polarization Observations
Authors: Archana Soam, Ka Ho Yuen, Ian Stephens, Chi Yan Law, Ka Wai Ho, Simon Coudé
Figure caption: The predicted B-field direction drawn via LIC given by the VGT method (Section 3.3) overlaid on the velocity channel intensities for three selected velocity channels: v = 11.09, 7.28, 5.58 km s−1.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Starspot maps on 2022 April 10, from (a) Doppler imaging and (b) TESS light-curve modeling. (c) Comparison of the spots from the Doppler imaging (green, right color bar) and those from the TESS light-curve modeling (gray circles), plotted on the radial magnetic field (background red and blue colors, the same as Figure 3(a)). The hemisphere is the same as Figures 3 and 4, a visible hemisphere when the prominence eruption occurred (BJD–2459680.033). The values in the intensity map are dimensionless as they are normalized by the quiescent surface intensity of the star.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Coronal extrapolation of the radial surface magnetic field using a potential field source surface model (e.g., M. D. Altschuler et al. 1977). Here, we assume that the field becomes open and fully radial beyond 3.4 R star, mimicking the effects of a stellar wind blowing open the field lines. The background surface radial magnetic field is the same as Figure 3 and the map depicts the hemisphere visible from Earth when the prominence eruption occurred (BJD–2459680.033).
Paper: Applying the Velocity Gradient Technique in NGC 1333: Comparison with Dust Polarization Observations
Authors: Archana Soam, Ka Ho Yuen, Ian Stephens, Chi Yan Law, Ka Wai Ho, Simon Coudé
Figure caption: Histograms of both gradient angles (computed for each tracer in the upper panels) and polarization angles (computed for 214 and 850 μm dust polarization observations in the lower panels) for the three selected regions in NGC 1333 by choosing the same velocity channel. From left to right: Blob, Hinge, Filament.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Magnetic field maps on 2022 April 10 for (a) radial, (b) azimuthal, and (c) meridional components. The maps take into account the stellar inclination angle and depict the hemisphere visible from Earth when the prominence eruption occurred (BJD–2459680.033).
Paper: Applying the Velocity Gradient Technique in NGC 1333: Comparison with Dust Polarization Observations
Authors: Archana Soam, Ka Ho Yuen, Ian Stephens, Chi Yan Law, Ka Wai Ho, Simon Coudé
Figure caption: (Top left) The B-field direction computed at 6.43 km s−1 as predicted by the N2H+ VGT compared to the dust polarization at 214 μm (black vectors) and 850 μm polarization (green vectors). The filled yellow stars are the locations of the protostars (J. J. Tobin et al. 2016). The region classifications (Blob, Hinge, Filament) are laid out as in Figure 2. Furthermore, the outflow directions (I. W. Stephens et al. 2017) are plotted also in the same figure. Similar plots on 12CO, 13CO, and C18O channel maps are also provided at their respective velocity channel with peak intensities. The name of each tracer is labeled in the lower right corner.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Observed Stokes V LSD profiles (back dots) and synthetic LSD profiles produced by the ZDI model (red curves). The blue dashed lines show the zero level. The numbers on the right indicate the rotation cycles. Successive observations are vertically shifted for plot clarity.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Same as Figure 1, but for the Stokes I LSD profiles.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Results from TESS light-curve modeling. The gray line represents the observed data from TESS Full Frame Images (FFI) in 2022 (Sector 50), and the red line shows the modeled light curve, which includes three spots.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: (a) The flare energy (﹩{E}_{\mathrm{flare}}﹩) as a function of spot group area (A spot) of solar flares and superflares on solar-type stars. The lower axis is the area of the spot group in the unit of the solar hemisphere (1/2 × A ☉ ∼ 3 × 1022 cm2). The top horizontal axis is the magnetic flux of spots under the assumption of B = 3000 G. The left vertical axis shows the bolometric energy released by each flare. The right vertical axis GOES X-ray class where we assume that bolometric energies of 1029, 1030, 1031, and 1032 erg scales to the GOES X-ray class of C, M, X, and X10, respectively. The black solid and dashed lines are the relationship between ﹩{E}_{\mathrm{flare}}﹩ and A spot for B = 3000 G and 1000 G, respectively. The relation assumes that the maximum flare energy against a given spot area can be explained by the total magnetic energy, i.e., ﹩{E}_{\mathrm{flare}}=\tfrac{1}{8\pi }{{fB}}^{2}{A}_{\mathrm{spot}}^{3/2}﹩, where f is a filling factor (e.g., K. Shibata et al. 2013). Here we did not add the error bars in the data because the xy-axis is in log scale, and the error range is too small to be plotted. (b) Comparison of the histograms for eruptive and non-eruptive events as a function of the ratio of flare area to spot area for the Sun and EK Dra. Stellar data are taken from Table 3. Solar data are taken from S. Toriumi et al. (2017), who derived the flare ribbon size from temporally stacked ultraviolet 1600 Å images. “FE” and “PE” mean filament and prominence eruptions, respectively.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Results from a 1D hydrodynamic simulation of the flow along the expanding magnetic loop (pseudo 2D MHD model; Section 3.3) described in K. Ikuta & K. Shibata (2024) and K. Ikuta et al. (2024, in preparation). (a) Schematic representation of the magnetic loop expanding at a constant velocity (depicted as a looplike structure at different times). The observer’s direction is indicated by the black axis. The loop’s footpoints are connected to the star, located at the stellar limb. The direction of the eruption is perpendicular to the line of sight. The prominence material in the loop is indicated with orange. The Lagrangian trajectory of plasma at the bottom, middle, and top of the original prominence are indicated with black solid, dashed, and dotted lines. (b) Expanded picture of panel (a). The initial condition of the magnetic loop and explanations of parameters are described in Appendix A.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: The velocity and length scale evolution with the estimated parameters from the 1D freefall model (“1D-FF”). The panels (a) and (b) represent the time evolution of velocity for the one-component and two-component fit for Hα line profiles, respectively. The modeled time evolution with the most likely parameters is indicated with a red solid line and its extrapolation with the red dashed line. The time range used for MCMC sampling is indicated with arrows. The panels (c) and (d) represent the time evolution of the x(t) (gray dashed–dotted line) and the prominence height (red solid line) for the one-component and two-component fit for Hα line profiles, respectively. For reference, panels (a) and (c) depict the components at three locations within a 1D hydrodynamic simulation of the flow along the expanding magnetic loop (“Pseudo 2D MHD” model; K. Ikuta & K. Shibata 2024 and K. Ikuta et al. 2024, in preparation) from Figure 11 using black lines (the line styles are consistent with those in Figure 11). Additionally, in panel (a), the center positions of the Gaussian fits to the pseudo Hα from Figure 11(c) are indicated by gray squares.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Comparison between the modeled and observed dynamic spectrum of Hα line from a 1D hydrodynamic simulation of the flow along the expanding magnetic loop (pseudo 2D MHD model; Section 3.3). (a) Simulated dynamic spectrum of the Hα line from the prominence material. Each black line corresponds to the velocity evolution of each Lagrangian trajectory of plasma in panel (a) of Figure 11. (b) Observed dynamic spectrum of the Hα line during the giant prominence eruptions on EK Dra, as reported in Paper                       I.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Correlations between posterior samples for each parameter for the “1D freefall” model (Section 3.2). Panels (a) and (b) show the MCMC sampling results for the velocity evolution obtained by the one- and two-component fitting of the Hα line, respectively. The green line represents the central value obtained by fitting the histogram to a normal distribution using scipy.stats.norm.fit. The black dashed lines indicate the 16% and 84% regions of the distribution. These boundaries correspond to the 68% confidence interval, commonly used to represent parameter uncertainty in MCMC analysis. The figure is plotted with a corner in Python.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Schematic picture of the simple “1D freefall” model.
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: Initial configurations and parameters of a 1D hydrodynamic simulation of the flow along the expanding magnetic loop (pseudo 2D MHD model; Section 3.3) described in K. Ikuta & K. Shibata (2024) and K. Ikuta et al. (2024, in preparation). The initial position of the prominence is indicated by the thick orange line. In our model, specifying the velocity parameter at the loop apex, V top (blue arrow), automatically determines the velocity distribution in the other parts of the magnetic loop (red arrows).
Paper: Multiwavelength Campaign Observations of a Young Solar-type Star, EK Draconis. II. Understanding Prominence Eruption through Data-driven Modeling and Observed Magnetic Environment
Authors: Kosuke Namekata, Kai Ikuta, Pascal Petit, Vladimir S. Airapetian, Aline A. Vidotto, Petr Heinzel, Jiří Wollmann, Hiroyuki Maehara, Yuta Notsu, Shun Inoue, Stephen Marsden, Julien Morin, Sandra V. Jeffers, Coralie Neiner, Rishi R. Paudel, Antoaneta A. Avramova-Boncheva, Keith Gendreau, Kazunari Shibata
Figure caption: An example of (a) the blueshifted Hα spectra and (b) the time evolution of the velocity taken from Paper                       I.
Paper: Chemical Pathways of SO2 with Hydrogen Atoms on Interstellar Ice Analogues
Authors: Thanh Nguyen, Yasuhiro Oba, W. M. C. Sameera, Kenji Furuya, Naoki Watanabe
Figure caption: (a) Comparison of SO2 after codeposition with H2 (black line) and H atoms (blue line) for up to 2 hr. The peaks at 1110, 1050, and 842 cm−1 could be derived from S-bearing species such as H2SO, HOSOH, and HS(O)OH. (b) Variations in the FTIR spectrum of products after the codeposition of SO2 with H atoms as the temperature increases. The vertical dotted lines in (b) are guides for eyes.
Paper: Chemical Pathways of SO2 with Hydrogen Atoms on Interstellar Ice Analogues
Authors: Thanh Nguyen, Yasuhiro Oba, W. M. C. Sameera, Kenji Furuya, Naoki Watanabe
Figure caption: Calculated reaction pathways with relative energies expressed in electronvolts. Cartesian coordinates of the optimized structures are in the Supporting Information (Table A1).
Paper: Chemical Pathways of SO2 with Hydrogen Atoms on Interstellar Ice Analogues
Authors: Thanh Nguyen, Yasuhiro Oba, W. M. C. Sameera, Kenji Furuya, Naoki Watanabe
Figure caption: (a) Variation in FTIR spectra of SO2 after exposure to H atoms on c-ASW for 5, 20, 60, and 120 minutes at 10 K. (b) Relative abundance of SO2 after exposure to H atoms for up to 2 hr on c-ASW at 10, 30, 40, and 60 K.
Paper: Chemical Pathways of SO2 with Hydrogen Atoms on Interstellar Ice Analogues
Authors: Thanh Nguyen, Yasuhiro Oba, W. M. C. Sameera, Kenji Furuya, Naoki Watanabe
Figure caption: TPD–QMS profiles after the codeposition of SO2 with H atoms (solid line) or H2 molecules (dotted line) at 10 K for up to 2 hr: (a) at m/z = 34 (for H2S); and (b) at m/z = 66 (for HS(O)OH). The peaks observed at ~80 and ~155 K correspond to the desorption of H2S from H2S and H2O, respectively (M. P. Collings et al. 2004). A minor peak observed at ~110 K in panel (a) for the blank experiment is attributed to the fragment (34S) of 34SO2.
Paper: Chemical Pathways of SO2 with Hydrogen Atoms on Interstellar Ice Analogues
Authors: Thanh Nguyen, Yasuhiro Oba, W. M. C. Sameera, Kenji Furuya, Naoki Watanabe
Figure caption: FTIR spectrum of the codeposition of SO2 with D atoms (blue) compared to D2 molecules as a blank (black) for 2 hr at 10 K. The peaks at 1948, 1075, and 847 cm−1 could be derived from S-bearing species such as D2SO, DOSOD, and DS(O)OH.
Paper: Chemical Pathways of SO2 with Hydrogen Atoms on Interstellar Ice Analogues
Authors: Thanh Nguyen, Yasuhiro Oba, W. M. C. Sameera, Kenji Furuya, Naoki Watanabe
Figure caption: TPD–QMS profiles after the codeposition of SO2 and D atoms (solid line) and D2 molecules (dotted line) for 2 hr at 10 K: (a) m/z = 20; (b) m/z = 36; and (c) m/z = 68.
Paper: Chemical Pathways of SO2 with Hydrogen Atoms on Interstellar Ice Analogues
Authors: Thanh Nguyen, Yasuhiro Oba, W. M. C. Sameera, Kenji Furuya, Naoki Watanabe
Figure caption: FTIR spectrum of solid SO2 on c-ASW at 10 K. The inset provides a detailed view of the 2200–2600 cm−1 region.
Paper: Chemical Pathways of SO2 with Hydrogen Atoms on Interstellar Ice Analogues
Authors: Thanh Nguyen, Yasuhiro Oba, W. M. C. Sameera, Kenji Furuya, Naoki Watanabe
Figure caption: Changes in the relative abundances of solid SO2 on c-ASW with exposure to H or D atoms at 10 K. The dotted lines represent fits to Equation (15).
Paper: Chemical Pathways of SO2 with Hydrogen Atoms on Interstellar Ice Analogues
Authors: Thanh Nguyen, Yasuhiro Oba, W. M. C. Sameera, Kenji Furuya, Naoki Watanabe
Figure caption: Top and side views of the ice cluster models: (a) ASW and (b) Ih.
Paper: Chemical Pathways of SO2 with Hydrogen Atoms on Interstellar Ice Analogues
Authors: Thanh Nguyen, Yasuhiro Oba, W. M. C. Sameera, Kenji Furuya, Naoki Watanabe
Figure caption: Binding energies of (a) SO2, (b) HSO2, and (c) HSO2H on ASW (1–5) and I h (6–10).
Paper: Interplanetary Rotation of 2021 December 4 Coronal Mass Ejection on Its Journey to Mars
Authors: Mengxuan Ma, Liping Yang, Fang Shen, Chenglong Shen, Yutian Chi, Yuming Wang, Yufen Zhou, Man Zhang, Daniel Heyner, Uli Auster, Ingo Richter, Beatriz Sanchez-Cano
Figure caption: Panels (a) and (b) show the calculated quasi-steady solar wind solution for the radial speed Vr and the magnetic field lines in the equatorial plane (a) and in the meridional plane (b) from 1 to 18 Rs. Panels (c) shows a 3D view of the initialized spheromak CME and the calculated quasi-steady corona from 1 to 5 Rs. Magnetic field lines are drawn as solid color lines with the color denoting the radial speed Vr. The color contours show the distribution of Br on the solar surface. The orange transparent 3D surface marks the contour of the ρ  c  = 0.01 surface. The black line with an arrow displays the direction of the symmetry axis of the spheromak CME.
Paper: Interplanetary Rotation of 2021 December 4 Coronal Mass Ejection on Its Journey to Mars
Authors: Mengxuan Ma, Liping Yang, Fang Shen, Chenglong Shen, Yutian Chi, Yuming Wang, Yufen Zhou, Man Zhang, Daniel Heyner, Uli Auster, Ingo Richter, Beatriz Sanchez-Cano
Figure caption: Panels (a) and (b) show the 3D view of the simulated CME in interplanetary space at t = 51 hr (a) and t = 91 hr (b), respectively, where the slice is on the equatorial plane from 20 to 500 Rs, with the colors denoting the magnetic field strength (B tot). The orange lines represent magnetic field lines, and the gray lines show the trajectories of BepiColombo and MAVEN/Tianwen-1. Panel (c) shows, from top to bottom, the magnetic field strength B tot and the magnetic field vector (Br, Bt, and Bn) in RTN coordinates measured by BepiColombo (blue squares) and reproduced by our simulation (orange lines). The vertical line and shaded area indicate the arrival of the shock and interval of the CME at BepiColombo, respectively. Panel (d) shows, from top to bottom, the magnetic field strength B tot, the magnetic field vector (Br, Bt, and Bn) in RTN coordinates, the number density (N), and the bulk velocity (V) measured by MAVEN (blue squares) and reproduced by our simulation (orange lines). The vertical line and shaded area represent the shock caused by the CME and interval corresponding to the CME determined from the data of MAVEN, respectively.