adsabs/AstroCLIMB huggingface dataset:
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: [Ar/O] against [Ne/O] for the jet-driven SN models in this work, compared with the EMP galaxy catalog presented in K. Watanabe et al. (2024; black circles with error bars) and in Y. Isobe et al. (2022; purple squares with error bars). The colored lines stand for the sequence of 1D models with different explosion energies.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The chemical abundance patterns of Model S25-1000-1000 with R cut = 1500 km (blue solid line) and R cut = 2100 km (red dashed line).
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The comparison of the post-explosion [Ne/O] against [Ar/O] for selected EMP galaxies and the “spherical” explosion models. The straight line stands for the solar values of the corresponding isotope ratios. The data points correspond to the EMP galaxies reported in Y. Isobe et al. (2022).
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Similar to Figure 8, but for the mass cut at R cut = 2100 km in the 25 M ⊙ model with the same jet parameters.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Similar to Figure 8, but for the mass cut at R cut = 1500 km in the 25 M ⊙ model with the same jet parameters.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: The tracer thermodynamics history of the characteristic model using the 25 M ⊙ star as the progenitor with R cut = 900, 1500, and 2100 km at the mass cut.
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: [Ca/Fe] against [Mg/Fe] for the EMP star analyzed in M. Jeong et al. (2023; black circle with error bars). Other data points are the theoretical models reported in this work and S.-C. Leung et al. (2023).
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Top panel: the chemical abundance of J1010+2358 (circles with error bars; Q.-F. Xing et al. 2023) and the best-fit models searched from the jet-driven SN models with M prog = 25 and 40 M ⊙ and spherical explosion models. Middle panel: same as the top panel, but with the data from P. N. Thibodeaux et al. (2024). Bottom panel: same as the top panel, but with the data from Skúladóttir et al. (2024).
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Top panel: same as Figure 21, but for [Fe/O] against [Ne/O]. Middle panel: same as the top panel, but for [Fe/O] against [Ar/O]. Bottom panel: same as the top panel, but for [Fe/O] against [S/O].
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Same as Figure 24, but for [Ni/Fe] against [Mg/Fe].
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Same as Figure 21, but for [S/O] against [Ne/O].
Paper: Hydrodynamics and Nucleosynthesis of Jet-driven Supernovae. II. Comparisons with Abundances of Extremely Metal-poor Galaxies and Constraints on Supernova Progenitors
Authors: Shing-Chi Leung, Ken'ichi Nomoto
Figure caption: Same as Figure 24, but for [Cr/Fe] against [Mg/Fe].
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: Variability period histograms for different samples of this work and, in the last line, histograms of rotation periods from seismology. On the left, we present the histograms of periods up to 30 hr, and on the right, the histograms of periods up to 100 hr. The red bins show the magnetic population in our samples of WDs. The labels indicate the samples plotted as well as their number.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: The left panel displays the rotational period in hours in log scale vs. mass in solar masses, while the right panel shows the mass distribution of sample 1. The red and blue dots/bins represent the WDs with magnetic fields and with close pairs detected, respectively. The black circles indicate the stars that comprise the likely single WDs.
Paper: Polar Neptunes Are Stable to Tides
Authors: Emma M. Louden, Sarah C. Millholland
Figure caption: Simulation validation through recreation of Figure 6 of C13. Long-term evolution of the HD 74156 system with I 0 = 40° for different values of the argument of the periastron. The top, middle, and bottom panels show the mutual inclination I, eccentricities e 1 and e 2, and semimajor axis a 1, respectively. We reproduce this figure from C13 to validate our simulations, which use a different numerical scheme.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: Mass distribution for our complete sample corrected by the ﹩1/{V}_{\max }﹩ volume. The red and blue bins represent the WDs with magnetic fields and with close pairs, respectively. The hatch-filled bins indicated the likely single WDs.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: The left panel displays the rotational period in hours vs. the effective temperature in kelvins, both in log scale. The right panel shows the temperature distribution of sample 1. The red and blue dots/bins represent the WDs with magnetic fields and with close pairs detected, respectively.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: Time-series analysis for the star TIC 1507548590. The top panel shows the FT as well as its FAP of 1/1000 (red dashed line). The bottom panel shows the light curve folded on the period of 1.92772 hr and a sinusoidal curve with the same period in red.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: Time-series analysis for the star TIC 1100582330. The top panel shows its FT as well as its FAP of 1/1000 (red dashed line). The bottom panel shows the light curve folded on the period of 2.736 hr and a sinusoidal curve with the same period in red.
Paper: Photometric White Dwarf Rotation
Authors: Gabriela Oliveira da Rosa, S. O. Kepler, L. T. T. Soethe, Alejandra D. Romero, Keaton J. Bell
Figure caption: Rotation period vs. mass relation for period determinations from asteroseismology. The period axis is in log scale. The black, cyan, and pink dots indicate DAV, DBV, and DOV stars, respectively.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Color composites created by combining g, r, and i images obtained with OAJ T80. The bottom image, with a field of view of 1.°2 × 0.°6, shows the location of the afterglow within the LAT error box. The top panels show the area of the images with the location of the afterglow on the first and second nights and have a field of view of 3.′0 × 2.′1. The optical afterglow is located at coordinates R.A. = 10:12:10.029 and decl. = +45:45:13.925 (J2000).
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Observational data and parameter evolution of the main pulse of GRB 200613A. The light curve (red) of the main pulse with a time resolution of 0.128 s and the Bayesian block (black) are shown in the first panel. The background level is indicated by the green dotted–dashed line. The subsequent three panels display the evolution of the spectral index (α), peak energy (E  p ), and energy flux (10–1000 keV) in the Band model. In the second panel, the synchrotron limit (–2/3) and fast-cooling limit (–3/2) are illustrated by a dashed line and a dotted line, respectively.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: A portion of the HST WFPC2 F606W image mosaic from 1997 March, with the location of the SN site indicated by a dashed circle (with radius corresponding to the 3σ uncertainty in the astrometric registration using an LBT r-band image of the SN from 2022 March). A stellar-like object with M F606W ≈ −8.2 mag is indicated by the black tick marks. We tentatively identify this object as the progenitor candidate. North is up, and east is to the left.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Arnett model fit of the bolometric light curve. The fit is done with an MCMC routine. The best-fitting results are represented by the 100 randomly chosen models drawn from the MCMC chain. The blue lines are the two-component fit and the gray lines are the one-component fit. The red lines and the green lines are the contributions from the inner region and the outer region, respectively. Only the blue points are used for the fit. The phase is shown with respect to the explosion epoch.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: One- and two-dimensional spectra of the host galaxy of GRB 200613A. The blue solid line shows the spectrum, while the gray dotted line shows the error spectrum. The black vertical lines mark the positions of both emission and absorption lines. The gray region marks the region of terrestrial absorption lines. According to prominent emission lines [O II] 3727/3729 doublet, we get a redshift of z = 1.2277 ± 0.0011 for GRB 200613A, and a similar redshift of z = 1.2262 ± 0.0009 for the intervening system by the absorption line.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Comparison of the nebular spectra of SN 2022crv at 290.6 days and 371.5 days post-explosion with models from A. Jerkstrand et al. (2015) and L. Dessart et al. (2021). The spectra are contaminated by the host galaxy, so we fit them with a combination of a star-forming galaxy spectrum and the model SN spectra. For the spectrum at day 371.5, there is strong background contamination below ∼5800 Å (marked with gray shading), which makes the observed spectrum clearly depart from the assumed star-forming galaxy spectrum.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Fermi/GBM and Fermi/LAT observational data for GRB 200613A. The points show the arriving times and energies of Fermi/LAT photons ≥100 MeV, and the photons whose probabilities associated with GRB 200613A excess 90% are highlighted in red. A third-order polynomial fit to the background level is shown as a green dotted–dashed line.
Paper: Characterizing the Rapid Hydrogen Disappearance in SN 2022crv: Evidence of a Continuum between Type Ib and IIb Supernova Properties
Authors: Yize Dong, 一泽 董, Stefano Valenti, Chris Ashall, Marc Williamson, David J. Sand, Schuyler D. Van Dyk, Alexei V. Filippenko, Saurabh W. Jha, Michael Lundquist, Maryam Modjaz, Jennifer E. Andrews, Jacob E. Jencson, Griffin Hosseinzadeh, Jeniveve Pearson, Lindsey A. Kwok, Teresa Boland, Eric Y. Hsiao, Nathan Smith, Nancy Elias-Rosa, Shubham Srivastav, Stephen Smartt, Michael Fulton, WeiKang Zheng, Thomas G. Brink, Melissa Shahbandeh, K. Azalee Bostroem, Emily Hoang, Daryl Janzen, Darshana Mehta, Nicolas Meza, Manisha Shrestha, Samuel Wyatt, Katie Auchettl, Christopher R. Burns, Joseph Farah, Lluís Galbany, Estefania Padilla Gonzalez, Joshua Haislip, Jason T. Hinkle, D. Andrew Howell, Thomas De Jaeger, Vladimir Kouprianov, Sahana Kumar, Jing Lu, Curtis McCully, Shane Moran, Nidia Morrell, Megan Newsome, Craig Pellegrino, Abigail Polin, Daniel E. Reichart, B. J. Shappee, Maximilian D. Stritzinger, Giacomo Terreran, M. A. Tucker
Figure caption: Comparison of the spectrum of SN 2022crv at 121 days after the explosion with models from L. Dessart et al. (2023).
Paper: Molecular Distribution in the Central Region of M87
Authors: Mahitosh Ray, Chorng-Yuan Hwang
Figure caption: (a) CO(1–0) velocity map of the nucleus with the p–v cut with average pixel width of 3. (b) P–v diagram of the CO(1–0) taken along the morphological minor axis (east to west) with a 3 pixel width. (c) P–v diagram of the CO(1–0) taken along the morphological major axis (northeast to southwest) with a cut of 3 pixel width.
Paper: Molecular Distribution in the Central Region of M87
Authors: Mahitosh Ray, Chorng-Yuan Hwang
Figure caption: Integrated intensity map of CO(1–0) for the velocity range of 1200–1300 km s−1, where σ is 0.22 Jy beam−1 km s−1. The white contours show the position of CO(2–1) gas distribution.
Paper: Molecular Distribution in the Central Region of M87
Authors: Mahitosh Ray, Chorng-Yuan Hwang
Figure caption: 3σ integrated intensity map of CO(1–0) used for the mass calculation, where σ is 0.18 Jy beam−1 km s−1. The green circle indicates the central 210 pc region selected for the calculation of mass.
Paper: Molecular Distribution in the Central Region of M87
Authors: Mahitosh Ray, Chorng-Yuan Hwang
Figure caption: The 345 GHz continuum image of the nucleus of M87.
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: Dependence of saturated radial field on the amplitude of meridional circulation v 0 in the 2D dynamo model with an explicit α term for the Babcock–Leighton process at different values of diffusivity; blue: the reference diffusivity η t as given by Equation (5), green: 2η t (scaled by a factor of 2 to fit in the range), red: η t/2 (scaled by a factor of 1/3).
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: Top: representation of the toroidal field B T (blue curve) in comparison with the polar field B P (gray curve, scaled by a factor of 2000) in relation to the flow amplitude. Bottom: same as the top but the variation in toroidal field is from a set of simulations in which the same initial magnetic field is taken from the output of the simulation with v 0 = 8 m s−1.
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: Variation of the latitudinal component of the surface meridional flow v  θ (R s, 45°) (red dashed curve) and the radial average of the poleward flow ﹩{\overline{v}}_{\theta }^{\mathrm{pole}}﹩ at 45° latitude (blue dotted curve, scaled by a factor of 8) with the rotation period of the stars.
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: Same as Figure 6, but from the set of simulations in which the meridional flow is taken from L. L. Kitchatinov & S. V. Olemskoy's (2012) mean-field hydrodynamics model of Sun-like stars having rotation periods varying from 1 to 30 days. The horizontal axis represents the rotation period of the corresponding mean-field model of stars.
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: Variation of saturated polar field strength B P with the flow amplitude v 0, from a simulation in which a single BMR is placed at 15◦ latitude. Red and blue colors correspond to simulations with and without the magnetic pumping. The data for latter case are multiplied by a factor of 60 for better visibility.
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: Variation of (a) the mean magnetic fields and (c) the cycle period with the flow speed. The right panels are the same as the left ones but from a low-diffusivity case (η  t /2).
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: The polar field strength B P vs. the amplitude of meridional flow at three distinct diffusivity values; blue: η  t —the reference diffusivity as given by Equation (5), red: 2η  t , green: η  t /2. Here, a single BMR is placed at 15° latitude.
Paper: The Role of Meridional Flow in the Generation of Solar/Stellar Magnetic Fields and Cycles
Authors: Vindya Vashishth, Bidya Binay Karak
Figure caption: Variation of the polar field strength B P with the flow amplitude v 0 for three different cases in which the BMR is placed at latitudes of 5◦ (blue), 15◦ (red), and 30◦ (green).
Paper: Properties of Solar Wind Current Sheets in the Martian Space Environment
Authors: Yangjun Chen, Mingyu Wu, Heying Wang, Peng E, Sudong Xiao, Guoqiang Wang, Xuesong Leng, Aimin Du, Tielong Zhang
Figure caption: A CS in the solar wind observed by MAVEN on 2016 January 15. From top to bottom, the panels show: (a)–(c) the three components of magnetic field; (d) the magnetic field magnitude ﹩{B}_{T}﹩; (e) the three components of the magnetic field in LMN coordinates; (f) the solar wind velocity; (g) the proton number density; (h) the proton temperature; (i) the ion energy spectrum; and (j) the current density. The lower notes denote the positions. The solid lines represents the original data, while the dashed blue lines in panels (a)–(c) are the 32-point smoothed data. The vertical dashed red line indicates the minimum value of ﹩{B}_{T}﹩ after smoothing and the maximum current density.
Paper: Properties of Solar Wind Current Sheets in the Martian Space Environment
Authors: Yangjun Chen, Mingyu Wu, Heying Wang, Peng E, Sudong Xiao, Guoqiang Wang, Xuesong Leng, Aimin Du, Tielong Zhang
Figure caption: The distribution of CS events as a function of (a) the duration, (b) the thickness in units of kilometers, (c) the thickness normalized by the proton inertial length ﹩{d}_{i},﹩ and (d) the thickness normalized by the proton gyroradius ﹩{r}_{g}.﹩ The cyan histograms represent CSs in the upstream solar wind, while the orange histograms represent CSs in the Martian magnetosheath.