adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Thermal Emission of the Terrestrial Exoplanet GJ 1132b
Authors: Qiao Xue, Jacob L. Bean, Michael Zhang, Alexandra Mahajan, Jegug Ih, Jason D. Eastman, Jonathan Lunine, Megan Weiner Mansfield, Brandon Park Coy, Eliza M.-R. Kempton, Daniel Koll, Edwin Kite
Figure caption: Corner plot of the planet temperature and temperature factor along with key star/planet parameters. The posteriors for T  s , a/R ⋆, and R  p /R ⋆ come from the global modeling described in Section 4. The posteriors for T  p  and ﹩{ \mathcal R }﹩ come from the modeling described in Section 5.1. Black shows the results using PHOENIX stellar models, and blue shows the results using SPHINX models.
Paper: JWST Thermal Emission of the Terrestrial Exoplanet GJ 1132b
Authors: Qiao Xue, Jacob L. Bean, Michael Zhang, Alexandra Mahajan, Jegug Ih, Jason D. Eastman, Jonathan Lunine, Megan Weiner Mansfield, Brandon Park Coy, Eliza M.-R. Kempton, Daniel Koll, Edwin Kite
Figure caption: Pixel-level light curves at 10.7861 and 10.8060 μm. An anomalous rise in flux followed by an exponential decay was found at 10.7861 μm, and a sharp drop at 10.8060 μm was found at the same time stamp.
Paper: Magnetically Arrested Circumbinary Accretion Flows
Authors: Elias R. Most, Hai-Yang Wang, 海洋 王
Figure caption: Circumbinary accretion cycle in the magnetically arrested state. (Left) The quiescent state, in which strong vertical magnetic fields (black streamlines) push out the accretion flow and support it. The cavity truncates well inside the inner Lindblad radius. We can also see a previous eruption episode to the right of the central cavity. (Center) Interchange instabilities trigger accretion streams through the cavity onto the mass sinks, with the cavity being highly distorted and expanded. We can also see that a reconnection-driven magnetic flare is launched vertically outward. (Right) This leads to an ejection of vertical net flux from the cavity in the circumbinary disk. The ejected (magnetic pressure-dominated) flux tube gets strongly sheared. Shown in color are the mass density ρ and magnetization parameter β, with the top and bottom rows showing the meridional and equatorial planes, respectively. Times t are stated relative to the orbital time period t orb.
Paper: Magnetically Arrested Circumbinary Accretion Flows
Authors: Elias R. Most, Hai-Yang Wang, 海洋 王
Figure caption: Mass ﹩\dot{M}﹩, electromagnetic energy ﹩{\dot{E}}_{\mathrm{EM}}﹩, and angular momentum ﹩\dot{J}﹩ fluxes into the cavity, normalized to the mass accretion rate ﹩{\dot{M}}_{\mathrm{out}}﹩ at large distances. The time series is shown relative to the orbital period t orbit ≡ 2π/Ω b . The red dashed line denotes the expected value of ﹩\left\langle \dot{J}/\dot{M}\right\rangle \simeq 0.68\,{a}^{2}{{\rm{\Omega }}}_{b}﹩ for a converged noneccentric, equal-mass, vertically integrated hydrodynamic accretion flow (D. J. Muñoz et al. 2019), and the cyan dashed line represents the threshold value, ﹩\left\langle \dot{J}/\dot{M}\right\rangle \simeq 3/8\,{a}^{2}{{\rm{\Omega }}}_{b}﹩, for the binary orbit to shrink (R. Miranda et al. 2017; D. Lai & D. J. Muñoz 2023).
Paper: Magnetically Arrested Circumbinary Accretion Flows
Authors: Elias R. Most, Hai-Yang Wang, 海洋 王
Figure caption: Radial profile of the mass accretion rate ﹩\dot{M}﹩ and the normalized magnetic flux ﹩{\phi }_{B}(r)={{\rm{\Phi }}}_{B}(r)/\sqrt{\dot{M}{r}^{2}}﹩, where Φ B (r) is the magnetic flux at cylindrical radius R, given relative to the binary separation, and a. Ωorb and M 0 are the binary orbital frequency and initial disk mass, respectively. Different times are shown with different colors, as denoted in the legend.
Paper: Magnetically Arrested Circumbinary Accretion Flows
Authors: Elias R. Most, Hai-Yang Wang, 海洋 王
Figure caption: Angular momentum transport in the circumbinary disk during a flux eruption. Shown is the ratio of the magnetic ﹩{\dot{J}}_{\mathrm{mag}}﹩ to advected ﹩{\dot{J}}_{\mathrm{adv}}﹩ angular momentum fluxes. (Top) Flux eruption in the equatorial plane. Angular momentum is largely transported outward due to magnetic stresses (pink regions). (Bottom) Angular momentum fluxes inside a flux tube (right). As the flux tube gets ejected into the disk (1 < x/a < 1.5), it drives a wind carrying angular momentum outward.
Paper: Magnetically Arrested Circumbinary Accretion Flows
Authors: Elias R. Most, Hai-Yang Wang, 海洋 王
Figure caption: Azimuthally and vertically integrated radial angular momentum fluxes as a spacetime diagram. (Left) Total radial angular momentum flux, ﹩{\left\langle \dot{J}\right\rangle }_{z,\phi }﹩. s = + 1 (outward)/ − 1 (inward) indicates the sign of the flux. (Right) Ratio of the magnetic ﹩{\left\langle {\dot{J}}_{\mathrm{mag}}\right\rangle }_{z,\phi }﹩ to the advective ﹩{\left\langle {\dot{J}}_{\mathrm{adv}}\right\rangle }_{z,\phi }﹩ contribution of the radial angular momentum flux. The cylindrical radius R is shown in units of the binary separation a. Times t are shown relative to the orbital period t orbit.
Paper: Magnetically Arrested Circumbinary Accretion Flows
Authors: Elias R. Most, Hai-Yang Wang, 海洋 王
Figure caption: Initial circumbinary evolution toward a magnetically arrested state over the first 110 binary orbits. (Top and bottom) Meridional slices along the orbital axis; (center) equatorial slices. Shown in color are the mass density ρ and magnetization parameter β. Times t are stated relative to the orbital period t orbit, whereas distances are stated relative to the binary separation a.
Paper: Implication of Jet Physics from MeV Line Emission of GRB 221009A
Authors: Zhen Zhang, Haoxiang Lin, Zhuo Li, Shao-Lin Xiong, Yan-Qiu Zhang, Qinyuan Zhang, Shu-Xu Yi, Xilu Wang
Figure caption: The time evolution of the emission line observed in GRB 221009A, which is reproduced from the discovery paper (Y.-Q. Zhang et al. 2024b). Panel (a): Central energy of emission line and the power-law fit. Vertical purple dashed line is the best-fit initial time (t 0) of the power-law evolution. Under the high-latitude effect framework, k = 1 is fixed in the fitting to derive the amplitude parameter A. Panel (b): Observed line flux and isotropic line luminosity with the power-law fit. Panel (c): Ratio of line width to line central energy. The horizontal dashed line denotes the 10%. Panel (d): Isotropic gamma-ray luminosity measured by GECAM-C (black line) and TeV luminosity observed by LHAASO (gray line).
Paper: Implication of Jet Physics from MeV Line Emission of GRB 221009A
Authors: Zhen Zhang, Haoxiang Lin, Zhuo Li, Shao-Lin Xiong, Yan-Qiu Zhang, Qinyuan Zhang, Shu-Xu Yi, Xilu Wang
Figure caption: Schematic plot for an expanding sphere (i.e., a jet with opening angle θ jet) that produces emission only at the radius from r to r + Δr. The EATS of a certain observer time is illustrated.
Paper: Implication of Jet Physics from MeV Line Emission of GRB 221009A
Authors: Zhen Zhang, Haoxiang Lin, Zhuo Li, Shao-Lin Xiong, Yan-Qiu Zhang, Qinyuan Zhang, Shu-Xu Yi, Xilu Wang
Figure caption: Constraints of r − Γ space for the line emission region by Equations (6) (blue line), (12) (brown shaded area), (15) (green lines), and (17) (red lines). It is assumed that L  γ  = 1054 erg s−1, L em = 1054 erg s−1, δ E  γ  = 1054 erg, and f v = 1, except that L em = 1055 erg s−1 for the solid green line, and f v = 3/8 for the solid red line. The gray shaded area is not allowed since E line > 37 MeV gives Γ > 80. The dark thick segment is the allowed parameter space for τ es < 1.
Paper: Solar Wind Structures from the Gaussianity of Magnetic Magnitude
Authors: Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Nikos Sioulas, Olga Panasenco, Trevor Bowen, Lorenzo Matteini, Mingtao Xia, 铭涛 夏, Xiaofei Shi, 晓霏 石, Sheng Huang, 胜 黄, Jia Huang, 佳 黄, Lizet Casillas
Figure caption: Selected interval from 2021 November, encounter 10 of PSP. (a) Spacecraft trajectory in the Carrington corotating frame from the afternoon of 2021 November 16 to the afternoon of 2021 November 22. Each day’s start is indicated with black circles. The ballistic solar wind streamlines are plotted at a 2 hr cadence and colored according to the 10 minute averaged solar wind speed profile from SPAN-ion moment. The selected interval is emphasized with a golden bar, and the 24 hr window JSD of normalized magnetic magnitude B * is represented by the colored band. An inset displays the helioradial power-law dependence of B. (b) Histogram of B and B * from the selected interval. (c) Histogram of B * and ﹩{\rm{JSD}}({{\rm{PDF}}}_{{B}^{* }})﹩. (d1) Spacecraft heliocentric distance (black) and Carrington longitude (orange). (d2) Magnetic field radial component B  r  and magnitude B. (d3) GS (scalogram of JSD). The selected interval is highlighted with the green pyramid. (d4) Helioradial power-law fit index scalogram of B.
Paper: Observation of the Galactic Center PeVatron beyond 100 TeV with HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, A. Andrés, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, U. Cotti, J. Cotzomi, S. Coutiño de León, E. De la Fuente, C. de León, D. Depaoli, N. Di Lalla, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, J. C. Díaz-Vélez, K. Engel, T. Ergin, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, H. Goksu, M. M. González, J. A. Goodman, S. Groetsch, J. P. Harding, S. Hernández-Cadena, I. Herzog, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, T. B. Humensky, P. Hüntemeyer, A. Iriarte, S. Kaufmann, D. Kieda, A. Lara, W. H. Lee, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Montes, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, M. Osorio-Archila, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, H. Salazar, D. Salazar-Gallegos, A. Sandoval, M. Schneider, G. Schwefer, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, E. Varela, X. Wang, Z. Wang, I. J. Watson, E. Willox, H. Wu, S. Yu, S. Yun-Cárcamo, H. Zhou
Figure caption: GC analysis results. (a) Significance map obtained using the HAWC neural network energy estimator (on- and off-array events; A. U. Abeysekara et al. 2019) and the position of the three main point sources and one extended source in the GC region as measured by H.E.S.S.. The dashed circle outlines the extension UL at the 68% CL. We also include the diffuse region used in the H.E.S.S. analysis (H.E.S.S. Collaboration et al. 2016). (b) Spectra of the two H.E.S.S. sources, along with the best-fit spectrum of HAWC J1746-2856. The dashed lines for the H.E.S.S. sources show the extrapolation of their best fit to the HAWC energy range. The flux points are calculated for each energy bin (A. Albert et al. 2024) by fixing all the fit parameters except for the flux normalization. (c) HAWC emission after subtracting the two H.E.S.S. point sources. We also show the density distribution contours of the ambient gas as traced by CS (J1-0) line emission (M. Tsuboi et al. 1999). (d) Original best-fit HAWC spectral energy distribution and the result after subtracting the two H.E.S.S. point-source spectra. As a reference, we include the diffuse emission measured by H.E.S.S. Collaboration et al. (2016), as their region is almost spatially coincident with our model. See Section 3 for details.
Paper: Solar Wind Structures from the Gaussianity of Magnetic Magnitude
Authors: Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Nikos Sioulas, Olga Panasenco, Trevor Bowen, Lorenzo Matteini, Mingtao Xia, 铭涛 夏, Xiaofei Shi, 晓霏 石, Sheng Huang, 胜 黄, Jia Huang, 佳 黄, Lizet Casillas
Figure caption: Gaussianity Scalogram from Ulysses' first orbit from 1993 to 1998. (a) Ulysses heliocentric distance R (black line) and heliographic latitude colored with local 48 hr averaged solar wind speed. (b) GS compiled from magnetic magnitude B (lower half) and helioradial power-law normalized magnitude B * (upper half). (c)﹩{R}_{\max }/{R}_{\min }﹩ of each interval (pixel), where the cutoff value is chosen to be ﹩{R}_{\max }/{R}_{\min }=1.5﹩, beyond which B is normalized into B * using the helioradial power-law fit before calculating the Gaussianity.
Paper: Solar Wind Structures from the Gaussianity of Magnetic Magnitude
Authors: Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Nikos Sioulas, Olga Panasenco, Trevor Bowen, Lorenzo Matteini, Mingtao Xia, 铭涛 夏, Xiaofei Shi, 晓霏 石, Sheng Huang, 胜 黄, Jia Huang, 佳 黄, Lizet Casillas
Figure caption: Panoramic plot of the data considered in this study. (a) Heliocentric distance of the spacecraft from encounter 1 to 14. The data analyzed in this study are from ±10 days around the perihelia, which are highlighted with black lines and pink-shaded areas. The two normally distributed long intervals under investigation are represented by the two green segments. (b) Detailed illustration of E10 to E12, with the spacecraft’s angular velocity in the Carrington corotation frame displayed on the twin axis. The corotating periods (ω < 10 [deg Day−1]) are marked with golden-shaded areas, and the selected intervals are highlighted in green on top of the angular velocity profile. (c),(d) Synopsis plot of E10 and E12 spacecraft trajectories from ±8 days around the perihelion in the Carrington corotating frame. The starts of each day are indicated by black dots, and the two arrows show the spacecraft’s entering directions, with the corresponding dates highlighted by red circles. The solar wind streamlines are colored according to the 10 minute averaged solar wind speed and are plotted every 2 hr. The two selected intervals are also highlighted in green.
Paper: Solar Wind Structures from the Gaussianity of Magnetic Magnitude
Authors: Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Nikos Sioulas, Olga Panasenco, Trevor Bowen, Lorenzo Matteini, Mingtao Xia, 铭涛 夏, Xiaofei Shi, 晓霏 石, Sheng Huang, 胜 黄, Jia Huang, 佳 黄, Lizet Casillas
Figure caption: Selected interval from E12.
Paper: Solar Wind Structures from the Gaussianity of Magnetic Magnitude
Authors: Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Nikos Sioulas, Olga Panasenco, Trevor Bowen, Lorenzo Matteini, Mingtao Xia, 铭涛 夏, Xiaofei Shi, 晓霏 石, Sheng Huang, 胜 黄, Jia Huang, 佳 黄, Lizet Casillas
Figure caption: Magnetic field connectivity with the solar sources during inbound of PSP encounter 12. The thick black lines are the model neutral lines. Black contours indicate magnetic field pressure at 1.05 R  s . The ballistic projection of the PSP trajectory (blue diamonds) on the source surface (blue crosses) and down to the solar wind source regions (blue circles) is calculated for source surfaces R  ss /R  s  = 2.5 (see O. Panasenco & M. Velli 2020 for details) and measured in situ solar wind speed ±80 km s1. Open magnetic field regions are shown in blue (negative) and green (positive).
Paper: Solar Wind Structures from the Gaussianity of Magnetic Magnitude
Authors: Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Nikos Sioulas, Olga Panasenco, Trevor Bowen, Lorenzo Matteini, Mingtao Xia, 铭涛 夏, Xiaofei Shi, 晓霏 石, Sheng Huang, 胜 黄, Jia Huang, 佳 黄, Lizet Casillas
Figure caption: GS of the PSP E10 inbound midlatitude coronal hole. (a) From top to bottom: Carrington longitude plotted with 1° cadence colored with spacecraft angular velocity in the corotating frame (blue: prograde, red: retrograde); JS scalogram with 1 minute resolution, normalized magnetic magnitude B *, radial component ﹩{B}_{r}^{* }﹩, and radial solar wind speed V  r ; (b) expanded view of panel (a) with a 10 s resolution.
Paper: Solar Wind Structures from the Gaussianity of Magnetic Magnitude
Authors: Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Nikos Sioulas, Olga Panasenco, Trevor Bowen, Lorenzo Matteini, Mingtao Xia, 铭涛 夏, Xiaofei Shi, 晓霏 石, Sheng Huang, 胜 黄, Jia Huang, 佳 黄, Lizet Casillas
Figure caption: Relaxation of magnetic magnitude B in Alfvénic MHD turbulence simulation. Upper panels: (Left) Probability distribution of B (PDF B ) at t = 0.00 t A, where t A = L/v A is the Alfvén time and L is the size of the simulation box, v A is the Alfvén speed; (Right) PDF B  at t = 0.40 t A. Lower panel: time evolution of the JSD between PDF B  and GS (blue line), and normalized standard deviation of B (dashed–dotted line). The time axis is normalized with the Alfvén time t A. The simulation time step of the upper left and right panels is highlighted with two red circles in the lower panel.
Paper: Solar Wind Structures from the Gaussianity of Magnetic Magnitude
Authors: Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Nikos Sioulas, Olga Panasenco, Trevor Bowen, Lorenzo Matteini, Mingtao Xia, 铭涛 夏, Xiaofei Shi, 晓霏 石, Sheng Huang, 胜 黄, Jia Huang, 佳 黄, Lizet Casillas
Figure caption: Skewness and normalized standard deviation scalogram. From top to bottom: spacecraft Carrington longitude plotted with 0.°1 cadence; magnetic magnitude (B, black) and radial component (B  r , blue); radial solar wind speed (V  r ); skewness scalogram of B; normalized standard deviation scalogram of B.
Paper: Solar Wind Structures from the Gaussianity of Magnetic Magnitude
Authors: Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Nikos Sioulas, Olga Panasenco, Trevor Bowen, Lorenzo Matteini, Mingtao Xia, 铭涛 夏, Xiaofei Shi, 晓霏 石, Sheng Huang, 胜 黄, Jia Huang, 佳 黄, Lizet Casillas
Figure caption: Benchmark of all three free parameters: number of standard deviation σ, number of bins, and number of points. (a) JSD between a given probability distribution function and the standard Gaussian distribution ﹩{ \mathcal N }(0,1)﹩. (b) “Ground-truth” values, i.e., the JSD of the histogram with N  b  number of bins estimated from N  p  number of points from ﹩{ \mathcal N }(0,1)﹩. (c) The same x- and y-bins as panel (b), with values of ﹩{\rm{JSD}}({{\rm{PDF}}}_{{\rm{Logistic}}}\parallel { \mathcal N }(0,1))﹩.
Paper: Solar Wind Structures from the Gaussianity of Magnetic Magnitude
Authors: Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Nikos Sioulas, Olga Panasenco, Trevor Bowen, Lorenzo Matteini, Mingtao Xia, 铭涛 夏, Xiaofei Shi, 晓霏 石, Sheng Huang, 胜 黄, Jia Huang, 佳 黄, Lizet Casillas
Figure caption: GS of the magnetic magnitude from the fluxgate magnetometer noise. From top to bottom: magnetic magnitude B time series; GS of B; standard deviation scalogram of B.
Paper: A Growing Braking Index and Spin-down Swings for the Pulsar PSR B0540–69
Authors: Cristóbal M. Espinoza, Lucien Kuiper, Wynn C. G. Ho, Danai Antonopoulou, Zaven Arzoumanian, Alice K. Harding, Paul S. Ray, George Younes
Figure caption: The evolution of ﹩\dot{\nu }﹩ of PSR B0540−69 between 2015 February and 2024 May. Top panel: the spin-down rate ﹩\dot{\nu }﹩ measured from overlapping intervals approximately 80 days long, containing at least six TOAs each. The data window was moved by 10 days at each stride, and for these short fits, ﹩\ddot{\nu }﹩ was held constant at a value measured from a larger TOA set (spanning at least 600 days). Middle panel: ﹩\ddot{\nu }﹩ measured over 250 day long, nonoverlapping time intervals. For these fits, a third derivative of the frequency was included in Equation (2), which was held as a fixed parameter at a value calculated from much longer intervals. These values are very small (﹩\dddot{\nu }\lt {10}^{-28}﹩ Hz s−3) and model a slow increase of ﹩\ddot{\nu }﹩ that is observed across the studied data set. Bottom panel: the braking index ﹩n=\nu \ddot{\nu }/{\dot{\nu }}^{2}﹩ calculated from each fit of the same intervals as in the middle panel. The two blue, open circles in the bottom panels show measurements corrected by the 2023 timing event, according to the TN model in Table 1.
Paper: Alpha–Proton Differential Flow of a Coronal Mass Ejection at 15 Solar Radii
Authors: Xuechao Zhang, Hongqiang Song, Xiaoqian Wang, Leping Li, Hui Fu, Rui Wang, Yao Chen
Figure caption: (a) and (c) Distributions of V  α p  and T  α /T  p  of the CME for different Coulomb number ranges. Dashed line, red, and green shaded regions show the V  α p  (or T  α /T  p ) of the combined, N  c  ≤ 0.5, and Nc  > 0.5, respectively. (b) and (d) Distributions of V  α p  and T  α /T  p  as a function of N  c .
Paper: Alpha–Proton Differential Flow of a Coronal Mass Ejection at 15 Solar Radii
Authors: Xuechao Zhang, Hongqiang Song, Xiaoqian Wang, Leping Li, Hui Fu, Rui Wang, Yao Chen
Figure caption: In situ measurements of the CME and solar wind by PSP from 11:00 to 15:00 UT on 2022 June 2. (a) and (b) The fluxes of protons and alphas as a function of azimuthal angle in the spacecraft frame. (c) Magnetic field. (d) The number density of protons and the absolute abundance of alphas. (e) The velocity of protons and alphas. (f) Alfvén Mach number and plasma β. (g) Differential flow and the flow normalized to the local Alfvén speed. (h) Temperature of protons and alpha-to-proton temperature ratio. (i) Coulomb number.
Paper: Alpha–Proton Differential Flow of a Coronal Mass Ejection at 15 Solar Radii
Authors: Xuechao Zhang, Hongqiang Song, Xiaoqian Wang, Leping Li, Hui Fu, Rui Wang, Yao Chen
Figure caption: Remote-sensing observations of the CME occurred on 2022 June 2. (a) Positions and/or directions of the Earth (SDO), STEREO-A, and PSP relative to the Sun in the ecliptic plane. (b) Direct image of AIA 304 Å. (c) Difference image of EUVI-A 195 Å. (d) Difference image of COR2-A. The green arrows denote the erupting filament or CME.
Paper: A Growing Braking Index and Spin-down Swings for the Pulsar PSR B0540–69
Authors: Cristóbal M. Espinoza, Lucien Kuiper, Wynn C. G. Ho, Danai Antonopoulou, Zaven Arzoumanian, Alice K. Harding, Paul S. Ray, George Younes
Figure caption: The rotational evolution of PSR B0540−69 since 2023 January. (a) The timing residuals relative to a model like Equation (2) adjusted up to MJD 60105. The two vertical dashed lines mark the epochs of the ﹩\dot{\nu }﹩ changes according to the TN model (t  g1 and t  g2), while the vertical dotted line indicates t  g  according to the glitch model. (b) Frequency residuals relative to the same model. (c) The behavior of ﹩\dot{\nu }﹩. The blue line represents the model used in the other panels. (d) The residuals of ﹩\dot{\nu }﹩ relative to the same model. Frequency and spin-down rate values were calculated as in Figure 1; thus, short-term features (<80 days) have been smoothed.
Paper: A Growing Braking Index and Spin-down Swings for the Pulsar PSR B0540–69
Authors: Cristóbal M. Espinoza, Lucien Kuiper, Wynn C. G. Ho, Danai Antonopoulou, Zaven Arzoumanian, Alice K. Harding, Paul S. Ray, George Younes
Figure caption: Timing residuals for the two models in Table 1. The vertical dotted line shows the epoch t  g  for the glitch model, while the two vertical dashed lines mark the epochs t  g1 and t  g2 for the TN model.
Paper: Sculpting of Exoplanetary Systems Driven by a Misaligned Disk and Stellar Oblateness: Origin of Perpendicular Orbits in HD 3167
Authors: Tao Fu, 韬 伏, Yue Wang, 悦 王
Figure caption: Equilibria and bifurcations of a fiducial two-planet system. The results are obtained for our fiducial system by using J 2,0 = 5 × 10−4, ψ ⋆0 = 80°, and the other parameters are those listed in Table 1. (A) shows all coplanar equilibrium solutions within the 0°–180° range. The solutions evolve over time as shown in the upper panel, where the sky blue dashed curve represents the equilibrium path that a planet initially aligned with the disk is likely to follow. The lower panel tracks the evolution of the parameters ε ⋆dk and ε ⋆c. (B) illustrates the phase portraits of the system by plotting the level curves of the integral of motion Φ given by Equation (A1) in the ﹩\left({\rm{\Delta }}h,{\psi }_{{\rm{b}}\star }\right)﹩ space, where Δh = h b − h c represents the differences in the longitude of the ascending node of the inner and outer orbits. Panels (a)–(d) correspond to the four stages during the evolution highlighted in (A). Note: Δh = 0 or π denotes the alignment or antialignment of  l  b with  l  c (or  l  dk), and Δh = ± π/2 denotes the perpendicularity between  l  b and  l  c (or  l  dk).