adsabs/AstroCLIMB huggingface dataset:
Paper: Partial Eruption of Solar Filaments. I. Configuration and Formation of Double-decker Filaments
Authors: Yijun Hou, Chuan Li, Ting Li, Jiangtao Su, Ye Qiu, Shuhong Yang, Liheng Yang, Leping Li, Yilin Guo, Zhengyong Hou, Qiao Song, Xianyong Bai, Guiping Zhou, Mingde Ding, Weiqun Gan, Yuanyong Deng
Figure caption: Temporal evolution of the double-decker filament system before and during its partial eruption. (a1)–(a8) Sequence of SDO/AIA 304 and 171 Å images showing the partial eruption process of the double-decker filaments and the resultant postflare loops. The slit “A–B” in (a1) approximates the moving direction of the erupting filament section. (b) Time–distance map derived from the 304 Å images along the slit “A–B” shown in (a1).
Paper: Partial Eruption of Solar Filaments. I. Configuration and Formation of Double-decker Filaments
Authors: Yijun Hou, Chuan Li, Ting Li, Jiangtao Su, Ye Qiu, Shuhong Yang, Liheng Yang, Leping Li, Yilin Guo, Zhengyong Hou, Qiao Song, Xianyong Bai, Guiping Zhou, Mingde Ding, Weiqun Gan, Yuanyong Deng
Figure caption: Mass motions of the filaments before and after the partial eruption observed by CHASE/HIS in the Hα channel. (a1)–(a4) Images of the Hα line center and two wings (Δλ = ± 0.5 Å) and the corresponding Doppler velocity map derived from Hα spectra data exhibiting the material flows in filaments before the eruption. The blue and red quadrilaterals mark the filament sections dominated by blueshift and redshift, respectively. The choice of solid and dotted lines depends on whether the signal is clear. (b1)–(b4) Similar to (a1)–(a4), but for the filament after the eruption.
Paper: Partial Eruption of Solar Filaments. I. Configuration and Formation of Double-decker Filaments
Authors: Yijun Hou, Chuan Li, Ting Li, Jiangtao Su, Ye Qiu, Shuhong Yang, Liheng Yang, Leping Li, Yilin Guo, Zhengyong Hou, Qiao Song, Xianyong Bai, Guiping Zhou, Mingde Ding, Weiqun Gan, Yuanyong Deng
Figure caption: Material flow and transient brightenings within the double-decker filament system before its partial eruption. (a1)–(a4) Sequence of SDO/AIA 304 Å images showing the material flow rotating around the lower filament (MFR1). The slit “C–D” in (a2) approximates the moving direction of the flow. (b) Time–distance map derived from the 304 Å images along the slit “C–D” shown in (a2). (c) 304 Å image showing the filament system after being disturbed by the flow. (d1)–(d4) Sequence of SDO/AIA 171 Å images showing the frequent brightenings in the southern region of the filament system before its eventual eruption.
Paper: Partial Eruption of Solar Filaments. I. Configuration and Formation of Double-decker Filaments
Authors: Yijun Hou, Chuan Li, Ting Li, Jiangtao Su, Ye Qiu, Shuhong Yang, Liheng Yang, Leping Li, Yilin Guo, Zhengyong Hou, Qiao Song, Xianyong Bai, Guiping Zhou, Mingde Ding, Weiqun Gan, Yuanyong Deng
Figure caption: 3D magnetic topology of the filaments before the partial eruption revealed by the NLFFF extrapolation. (a)–(c) Top and side views of two MFRs (MFR1 and MFR2) composing a double-decker configuration. (d)–(f) Distributions of the magnetic twist T  w  and logarithmic Q in the vertical plane based on the green cut denoted in (a).
Paper: Kinetic and Shear Alfvén Waves in a Large Guide-field Reconnection at Earth's Magnetopause
Authors: Wai-Leong Teh, Wenzhe Zhang, Huishan Fu
Figure caption: The consecutive difference in B  L  at the four MMS spacecraft for (a) SAW and (c) KAW. The PSD of δ B  L  based on MMS1 is displayed for (b) SAW and (d) KAW, where the red and black dashed lines denote the spectral peaks, and the proton gyrofrequency is at the green line. The two values of the normalized frequency correspond to 1 Hz and 10 Hz in the spacecraft frame.
Paper: Kinetic and Shear Alfvén Waves in a Large Guide-field Reconnection at Earth's Magnetopause
Authors: Wai-Leong Teh, Wenzhe Zhang, Huishan Fu
Figure caption: (a)–(f) Wave structures for ion and electron plasma velocities, and magnetic field. (g) Comparison of the Poynting flux ∣S∣ to ∣S ∥∣. (h) The ratio of parallel to perpendicular temperature for ions (blue) and electrons (red). The first and second waveforms are enclosed by the green and gray lines, respectively. The red dashed lines denote the wave peaks.
Paper: Kinetic and Shear Alfvén Waves in a Large Guide-field Reconnection at Earth's Magnetopause
Authors: Wai-Leong Teh, Wenzhe Zhang, Huishan Fu
Figure caption: The dispersion relation and frequency vs. k ⊥ d for (a), (b) SAW and (c), (d) KAW. The color code is the wave power derived from a wavelet transform. The red dashed line in (a) and (c) denotes the local Alfvén speed at 221 and 394 km s−1, respectively. The cross and triangle results are obtained from a different method.
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: Left and middle panels: Halo mass assembly as a function of the lookback time of the four subsamples at a given halo mass (M halo = 1012.0–1012.1 M ⊙) at z = 0, binned by halo assembly time (t h,50, defined as the lookback time of a halo first assembled half of the present-day halo mass) for star-forming central galaxies (left panel) and passive central galaxies (middle panel) in L-GALAXIES. These halos are divided into four subsamples according to their t h,50 value, marked by blue (HAT1, t h,50 = 10–12 Gyr), orange (HAT2, t h,50 = 8–10 Gyr), green (HAT3, t h,50 = 6–8 Gyr), and red (HAT4, t h,50 < 6 Gyr) curves. The shaded regions represent the 1σ  error on the median value and the gray dashed horizon line represents the average value of half present-day halo mass. Right panel: Mass increase rate of halo (MIRhalo) as a function of the lookback time for the same four subsamples of different t h,50 in L-GALAXIES, with the shaded regions covering 40th to 60th percentiles variation.
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: Top four panels: Stellar mass distribution of star-forming central galaxies (SFGs) and passive central galaxies (PGs) residing in halos of different t h,50 at a given halo mass (M halo = 1012.0–1012.1 M ⊙) at z = 0 in L-GALAXIES. These colors indicate different t h,50 bins, consistent with Figure 7. The fifth panel: Stellar mass distribution of all SFGs and PGs residing in M halo = 1012.0–1012.1 M ⊙ halos. Each panel presents two histograms, one for SFGs and one for PGs, plotted by solid and dashed step lines, respectively. The vertical black solid/dashed lines represent the median stellar mass of SFGs/PGs at z = 0, and the shaded regions indicate a 1σ  error on the median value. The quenched fraction for each panel is given in the top-right corner, calculated with a stellar mass cut of M * ≥ 1010.0 M ⊙. Bottom panel: The same as other panels but for central galaxies (z = 0.02–0.10) residing in M halo = 1011.9–1012.1 M ⊙ halos in SDSS DR7 with ﹩{V}_{\max }﹩ weighted. The halo mass of central galaxies in SDSS DR7 is derived from Zhao et al. (2023, in preparation).
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: Stellar mass growth history of the eight subsamples of central galaxies residing in halos of different t h,50 at a given halo mass (M halo = 1012.0–1012.1 M ⊙) at z = 0 in L-GALAXIES. Each color represents a different t h,50 bin, consistent with those in Figure 7. The solid and dashed lines denote the median values of star-forming central galaxies (SFGs) and passive central galaxies (PGs), respectively, while the shaded regions indicate the 1σerror on the median value. The “stars” and “triangles” show the median values of the present-day total stellar mass for groups with a star-forming or passive central galaxy, respectively, and are randomly offset to prevent overlap with other curves.
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: Halo mass assembly (left panel) and specific mass increase rate of halo (sMIRhalo, right panel) as a function of the lookback time of central galaxies in L-GALAXIES. The colors represent galaxies in different stellar mass ranges at z = 0: ﹩\mathrm{log}({M}_{* }/{M}_{\odot })=9.0\mbox{--}10.0﹩ (M1: blue), 10.0–10.5 (M2: orange), 10.5–11.0 (M3: green), and 11.0–12.0 (M4: red), respectively. The solid and dashed lines show the median values of star-forming central galaxies (SFGs) and passive central galaxies (PGs), respectively. The shaded regions represent the 1σ  error on the median value (left panel) or the 40th to 60th percentile variation (right panel).
Paper: Massive Black Hole Binaries from the TNG50-3 Simulation. II. Using Dual AGNs to Predict the Rate of Black Hole Mergers
Authors: Kunyang Li, Tamara Bogdanović, David R. Ballantyne, Matteo Bonetti
Figure caption: The redshift distribution of all dAGNs with total bolometric luminosity larger than 1043 erg s−1 and with separations of 0.7, 0.4, and 0.1 kpc.
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: Quenched fraction (left panel) and averaged stellar mass (right panel) of central galaxies as a function of the halo mass and halo assembly time t h,50 in L-GALAXIES, with a stellar mass cut of M * ≥ 1010.0 M ⊙. The red/blue color codings indicate high/low values of the quenched fraction (left panel) and averaged stellar mass (right panel).
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: Stellar mass growth history of star-forming central galaxies (SFGs, blue) and passive central galaxies (PGs, red) in L-GALAXIES, normalized to the stellar mass at z = 0. Each panel corresponds to a different range of present-day stellar mass: ﹩\mathrm{log}({M}_{* }/{M}_{\odot })=9.0\mbox{--}10.0﹩ (M1), 10.0–10.5 (M2), 10.5–11.0 (M3), and 11.0–12.0 (M4), respectively. The curves depict the median values of each stellar mass bin, with shaded regions representing 1σ  error on the median value. Dashed lines mark half of the present-day stellar mass.
Paper: From Halos to Galaxies. VII. The Connections between Stellar Mass Growth History, Quenching History, and Halo Assembly History for Central Galaxies
Authors: Cheqiu Lyu, Yingjie Peng, Yipeng Jing, Xiaohu Yang, Luis C. Ho, Alvio Renzini, Bitao Wang, Kai Wang, Bingxiao Xu, Dingyi Zhao, Jing Dou, Qiusheng Gu, Roberto Maiolino, Filippo Mannucci, Feng Yuan
Figure caption: As for Figure 10 but with stellar mass cut of M * ≥ 109.0 M ⊙ (left panel) and M * ≥ 109.5 M ⊙ (right panel).
Paper: Magnetohydrodynamical Torsional Oscillations from Thermoresistive Instability in Hot Jupiters
Authors: Raphaël Hardy, Paul Charbonneau, Andrew Cumming
Figure caption: Magnetic Reynolds number Rm = u 0 H/η as a function of pressure and temperature, where we take the characteristic velocity u 0 = 5 km s−1, H is the pressure scale height, and η is evaluated at the local temperature and pressure. The solid lines represent typical T–P profiles of HJs used in our simulations, with intervals of T eq = 50 K. The profiles with T eq = 1000 and 1200 K are identified with a label above them. The dotted line shows Rm = 1.
Paper: Magnetohydrodynamical Torsional Oscillations from Thermoresistive Instability in Hot Jupiters
Authors: Raphaël Hardy, Paul Charbonneau, Andrew Cumming
Figure caption: Recurrence period in the instability region for systems with ﹩\dot{v}=0.01﹩ m s−1 and κ th = 0.0005 m2 kg−1 and different values of equilibrium temperature and radial background magnetic field. Three different regions have been identified corresponding to the behavior of the systems.
Paper: Magnetohydrodynamical Torsional Oscillations from Thermoresistive Instability in Hot Jupiters
Authors: Raphaël Hardy, Paul Charbonneau, Andrew Cumming
Figure caption: The top panels show the evolution of a solution including the ∇η term of Equation (3), where we show (a) the velocity, (b) the magnetic field, and (c) MD. The bottom panels show the evolution of a solution omitting the ∇η term of Equation (3), where we show (d) the velocity, (e) the magnetic field, and (f) MD. The top panels cover one Alfvénic oscillation (approximately 2% of the recurrence time) to better show the strong radial gradients during the burst phase; the bottom panels show the full recurrence period. The parameters of the simulation are the same as in Figure 3.
Paper: Magnetohydrodynamical Torsional Oscillations from Thermoresistive Instability in Hot Jupiters
Authors: Raphaël Hardy, Paul Charbonneau, Andrew Cumming
Figure caption: Rosseland mean opacity from Freedman et al. (2008) at solar metallicity in the T–P plane. The black lines represent standard T–P profiles used in our simulations with T eq = 1000 and 1200 K.
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption:                       ﹩\mathrm{log}\epsilon (\mathrm{Th}/\mathrm{Eu})﹩ (left panel) and ﹩\mathrm{log}\epsilon (\mathrm{Eu})﹩ (right panel) as a function of [Fe/H] for metal-poor stars in the literature with both Th and Eu measured ([Fe/H] ≤ −1.0 and [Eu/Fe] ≥ +0.60), compared to SPLUS J1424−2542. The point sizes are proportional to [Eu/Fe] (left) and [Th/Fe] (right), according to the labels between the panels. The horizontal solid gray line marks the solar ﹩\mathrm{log}\epsilon (\mathrm{Th}/\mathrm{Eu})﹩ value and on the right panel, the limits for the r-II and r-III stars are shown. Individual references are given in Table 6.
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Upper panel: heavy-element chemical abundance pattern of SPLUS J1424−2542, compared with the scaled solar system abundances. The r- and s-process contributions are calculated based on the fractions given by Burris et al. (2000) and scaled to match the observed abundances of Eu and Ba, respectively. Also shown are the r- and s-process fractions for each element (top), as well as the number of lines identified for each element (bottom). Open circles show the individual abundances for all the lines measured in the GHOST spectrum. Lower panel: residuals between the observations and the scaled solar system abundance patterns. A ±0.2 dex shaded area is shown for reference.
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Top panel: comparison between the vertical component of the angular momentum and orbital energy of SPLUS J1424−2542 (yellow star-shaped symbol) to those of known halo substructures (as defined by Koppelman et al. 2019) and DTGs (identified by Lövdal et al. 2022). Bottom panel: eccentricity and maximum distance from the Galactic plane for SPLUS J1424−2542 and the stars in the Lövdal et al. (2022) sample.
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Age (left) and initial mass (right) CDFs obtained for SPLUS J1424−2542 using the Bayesian isochronal method described in Almeida-Fernandes et al. (2023). The dashed lines correspond to the 16th (red), 50th (black), and 84th (blue) percentiles used to characterize the parameters and their uncertainties. For comparison, the ticks in the bottom panels correspond to the 16th (red), 50th (black), and 84th (blue) percentiles for all 522 stars in the Placco et al. (2022) sample.
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Upper panel: heavy-element chemical abundance pattern of SPLUS J1424−2542, compared with the scaled solar system r-process (yellow) and the best-fit neutron star merger model (blue), normalized to match the observed Eu abundance. Also shown (gray lines) are random realizations of the neutron star merger; see text for details. Lower panel: residuals between the observations and scaled predictions. A ±0.2 dex shaded area is shown for reference.
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Upper panel: light-element chemical abundance pattern of SPLUS J1424−2542, (filled circles, LTE) compared with the yields from metal-free supernova models (solid lines). The labels show the progenitor mass and explosion energy of the models and their percentage occurrence among the 10,000 abundance pattern resamples of SPLUS J1424−2542. Lower panel: residuals between the observations and the two best-fit models. A ±0.3 dex shaded area is shown for reference.
Paper: Wide-bandwidth Observations of PSR J0941–39 and PSR J1107–5907
Authors: S. N. Sun, N. Wang, W. M. Yan, S. Q. Wang, J. T. Xie
Figure caption: Single-pulse stacks of (a) PSR J0941–39 and (b) PSR J1107–5907 during the pulsar state and RRAT state.
Paper: SPLUS J142445.34–254247.1: An r-process–enhanced, Actinide-boost, Extremely Metal-poor Star Observed with GHOST
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Erika M. Holmbeck, Ian U. Roederer, Mohammad K. Mardini, Christian R. Hayes, Kim Venn, Kristin Chiboucas, Emily Deibert, Roberto Gamen, Jeong-Eun Heo, Miji Jeong, Venu Kalari, Eder Martioli, Siyi Xu, Ruben Diaz, Manuel Gomez-Jimenez, David Henderson, Pablo Prado, Carlos Quiroz, Roque Ruiz-Carmona, Chris Simpson, Cristian Urrutia, Alan W. McConnachie, John Pazder, Gregory Burley, Michael Ireland, Fletcher Waller, Trystyn A. M. Berg, J. Gordon Robertson, Zachary Hartman, David O. Jones, Kathleen Labrie, Gabriel Perez, Susan Ridgway, Joanna Thomas-Osip
Figure caption: Same as Figure 5, using the NLTE abundances listed in Table 5.
Paper: Kinetic and Shear Alfvén Waves in a Large Guide-field Reconnection at Earth's Magnetopause
Authors: Wai-Leong Teh, Wenzhe Zhang, Huishan Fu
Figure caption: (a)–(g) MMS1 observations of a large guide-field reconnection X-line during the magnetopause crossing enclosed by the vertical lines, with vectors shown in LMN coordinate systems. (h)–(j) The rates of energy conversion and the parallel electric fields. The magenta dashed line in panel (a) denotes the ambient reconnection guide field. The green line in panel (e) denotes the Hall electric fields evaluated in the X-line moving frame.
Paper: Kinetic and Shear Alfvén Waves in a Large Guide-field Reconnection at Earth's Magnetopause
Authors: Wai-Leong Teh, Wenzhe Zhang, Huishan Fu
Figure caption: (a) Electron PAD for the energy range of 0.2–2.0 keV. (b)–(d) The overlaid plots of the magnetic field and the ion and electron velocity (− V   i  and − V   e ) for each component in LMN coordinate systems. The vertical lines mark the duration of the magnetopause crossing.