adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HD 33142 b and HD 332231 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HD 2952 b and HD 32518 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HD 4313 b and HD 43197 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HD 360 b and HD 37124 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HIP 105854 b and HIP 107773 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HIP 109600 b and HIP 12961 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HIP 14810 c and HIP 34222 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HD 92788 b and HD 93083 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HIP 5158 b and HIP 57274 c.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HD 87646 b and HD 89744 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HD 96063 b and HD 99283 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HD 82943 c and HD 8574 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters HD 9446 b and HD 9446 c.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters TYC 3667-1280-1 b and TYC 4282-00605-1 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters TYC 0434-04538-1 b and TYC 1422-614-1 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters WASP-117 b and WASP-130 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters TOI-2202 c and TOI-3362 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters TOI-2180 b and TOI-2202 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters WASP-148 c and XO-2 S c.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters TOI-1899 b and TOI-201 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters TOI-677 b and TOI-892 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters TOI-481 b and TOI-558 b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters ups And c and xi Aql b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters omi CrB b and rho CrB b.
Paper: Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters
Authors: Marvin Morgan, Brendan P. Bowler, Quang H. Tran, Robert A. Wittenmyer, Duncan J. Wright, George Zhou, Tyler R. Fairnington
Figure caption: Summary of results for the warm Jupiters mu Leo b and ome Ser b.
Paper: MaNGA DynPop. VII. A Unified Bulge–Disk–Halo Model for Explaining Diversity in Circular Velocity Curves of 6000 Spiral and Early-type Galaxies
Authors: Kai Zhu, Michele Cappellari, Shude Mao, Shengdong Lu, Ran Li, Yong Shi, David A. Simon, Youquan Fu, Xiaohan Wang
Figure caption: The correlations between σe and circular velocity at the half-light radius ﹩{V}_{{\rm{circ}}}({R}_{{\rm{e}}}^{{\rm{maj}}})﹩ (top panels) as well as the maximum circular velocity ﹩{V}_{{\rm{circ}}}^{{\rm{\max }}}﹩ (bottom panels). These relations are derived from Qual ≥ 1 galaxies with nearly face-on galaxies (inclination angles below 30∘) excluded. Top left: The relation between σe and ﹩{V}_{{\rm{circ}}}({R}_{{\rm{e}}}^{{\rm{maj}}})﹩. Symbols with different color correspond to different JAM model qualities (see Section 5.1 in K. Zhu et al. 2023b). The coefficients of the best-fitting line y = a + b(x – x0) and the observed rms scatter Δ are obtained from the LTS_LINEFIT procedure (with clip = 4) (M. Cappellari et al. 2013a). The black solid, red dashed, and red dotted lines represent the best-fitting, the 1σ error (68%), and the 2.6σ error (99%), respectively. The best-fitting relation can be approximated as ﹩{V}_{{\rm{circ}}}({R}_{{\rm{e}}}^{{\rm{maj}}})\approx 1.62\times {\sigma }_{{\rm{e}}}﹩ (Equation (9)) with an error of ﹩{\rm{\Delta }}/\sqrt{2}=7﹩%. The black dashed and black dotted lines correspond to the best-fitting relations for ETGs (k ≈ 1.59) and LTGs (k ≈ 1.71), respectively. Top right: comparisons with ATLAS3D (cyan line), EAGLE simulation (magenta line), Illustris-TNG simulation (red line), and the theoretical prediction of J. Wolf et al. (2010; black dashed line), which are taken from I. Ferrero et al. (2021). Bottom left: Similar to the top-left panel but showing the correlation between σe and ﹩{V}_{{\rm{circ}}}^{{\rm{\max }}}﹩. The best-fitting relation can be described as ﹩{V}_{{\rm{circ}}}^{{\rm{\max }}}\approx 1.72\times {\sigma }_{{\rm{e}}}﹩ with an error of ﹩{\rm{\Delta }}/\sqrt{2}=7﹩%. The black dashed and black dotted lines correspond to the best-fitting relations for ETGs and LTGs, respectively. Bottom right: Similar to the bottom-left panel but only including the galaxies whose radius of maximum circular velocity lies in the kinematic data range. The best-fitting relation remains nearly unchanged with a slightly smaller error of 5%.
Paper: MaNGA DynPop. VII. A Unified Bulge–Disk–Halo Model for Explaining Diversity in Circular Velocity Curves of 6000 Spiral and Early-type Galaxies
Authors: Kai Zhu, Michele Cappellari, Shude Mao, Shengdong Lu, Ran Li, Yong Shi, David A. Simon, Youquan Fu, Xiaohan Wang
Figure caption: Scaling relations between structural parameters (B/T, nSer,bulge, Re,bulge/Re,disk, rs/Re) and σe for the Qual ≥ 1 galaxies. B/T, nSer,bulge, and Re,bulge/Re,disk are taken from H. Domínguez Sánchez et al. (2022) (see Section 2.2 for definitions). rs/Re is the ratio between the dark halo scale radius and Re of the whole galaxy, where rs is estimated from the Chabrier IMF-based stellar mass, the stellar-mass-to-halo-mass relation in B. P. Moster et al. (2013), and the mass–concentration relation in A. A. Dutton & A. V. Macciò (2014). The blue contours are the kernel density estimate for the galaxy distribution, while the black dashed curve and the gray shaded region represent the median value and [16th, 84th] percentile of values, respectively. The best-fitting relations to the median trends (Equations (21) and (22)) are shown in red solid curves. The horizontal red dashed line in the third panel represents the median value of lg (Re,bulge/Re,disk) for the entire sample, while the horizontal red dashed line in the fourth panel represents the median value of lg (rs/Re) for galaxies with lg (σe/km s−1) < 2.1.
Paper: MaNGA DynPop. VII. A Unified Bulge–Disk–Halo Model for Explaining Diversity in Circular Velocity Curves of 6000 Spiral and Early-type Galaxies
Authors: Kai Zhu, Michele Cappellari, Shude Mao, Shengdong Lu, Ran Li, Yong Shi, David A. Simon, Youquan Fu, Xiaohan Wang
Figure caption: Comparisons between the BDH model-predicted shape of normalized CVCs (solid curves) and those derived from JAM (dashed curves) for four different velocity dispersion (σe) bins, indicated by different colors. In the left panel, we show the median profile of the JAM-derived CVCs for each σe bin, while the BDH model predictions are calculated at the bin centers using the scaling relations (three relations as a function of σe, and two are constants) presented in the left panel. The ratio between the JAM-derived and BDH-predicted CVCs, along with the associated error (represented by the [16th, 84th] percentiles of the JAM-derived CVCs), is shown in the right panel.
Paper: MaNGA DynPop. VII. A Unified Bulge–Disk–Halo Model for Explaining Diversity in Circular Velocity Curves of 6000 Spiral and Early-type Galaxies
Authors: Kai Zhu, Michele Cappellari, Shude Mao, Shengdong Lu, Ran Li, Yong Shi, David A. Simon, Youquan Fu, Xiaohan Wang
Figure caption: The normalized CVCs correlate with other galaxy properties. Definitions can be found in Sections 2.2 and 2.3. These properties include masses (dynamical mass MJAM and stellar mass M* based on Salpeter IMF), morphology (T-Type and B/T), velocity dispersion σe, spin parameter ﹩{\lambda }_{{{\rm{R}}}_{{\rm{e}}}}﹩, the cosmic times when stars accounting for 50% (T50) and 90% (T90) of galaxies’ present-day stellar mass were formed, luminosity-weighted stellar age, stellar metallicity, and their radial gradients.
Paper: MaNGA DynPop. VII. A Unified Bulge–Disk–Halo Model for Explaining Diversity in Circular Velocity Curves of 6000 Spiral and Early-type Galaxies
Authors: Kai Zhu, Michele Cappellari, Shude Mao, Shengdong Lu, Ran Li, Yong Shi, David A. Simon, Youquan Fu, Xiaohan Wang
Figure caption: Examples of different shapes of JAM-derived CVCs (rising CVCs for the first two rows, flat CVCs for the second two rows, and declining CVCs for the third two rows). For each galaxy, there are six images: the RGB image with plateifu (top left), the map of circular velocities (top middle), the map of line-of-sight velocity (top right), the CVC in the equatorial plane derived from JAM model (bottom left), the map of stellar age (bottom middle), and the map of stellar metallicity (bottom right). The black contours are the observed surface brightness contours in steps of 1 mag. The black dots are the centroids of the Voronoi bins from which the maps were linearly interpolated.
Paper: MaNGA DynPop. VII. A Unified Bulge–Disk–Halo Model for Explaining Diversity in Circular Velocity Curves of 6000 Spiral and Early-type Galaxies
Authors: Kai Zhu, Michele Cappellari, Shude Mao, Shengdong Lu, Ran Li, Yong Shi, David A. Simon, Youquan Fu, Xiaohan Wang
Figure caption: The distributions of B/T (top-left panel), lg nSer,bulge (top-right panel), T50/T90 (bottom-left panel), and the median CVC within a given mass and size bin (bottom-right panel) are shown on the ﹩{M}_{{\rm{JAM}}}-{R}_{{\rm{e}}}^{{\rm{maj}}}﹩ plane. Distributions of fDM( < Re) can be found in K. Zhu et al. (2024, top-right panel of Figure 16). The distributions are smoothed by the LOESS software (M. Cappellari et al. 2013b) with frac = 0.05. In all panels, the dashed lines correspond to effective velocity dispersion σe =  50, 100, 200, 300, 400, and 500 km s−1 from left to right, which are calculated using the scalar virial equation ﹩{\sigma }_{{\rm{e}}}^{2}\equiv G{M}_{{\rm{JAM}}}/(5{R}_{{\rm{e}}}^{{\rm{maj}}})﹩ (with factor 5 from M. Cappellari et al. 2006). The magenta curve shows the zone of exclusion (ZOE) defined in M. Cappellari et al. (2013b, equation 4), with the ZOE above MJAM = 2 × 1010M⊙ approximately ﹩{R}_{{\rm{e}}}^{{\rm{maj}}}\propto {M}_{{\rm{JAM}}}^{0.75}﹩. The gray contours show the kernel density estimate for the galaxy distribution. Bottom-right panel: The inset panels in the bottom-right panel show the median (red solid) and the [16th, 84th] percentiles (red shaded region), as well as the median FWHM of PSF (vertical shaded gray region). All the inset panels have the same physical scales as the bottom-right panel, while the ticks and labels are shown in the upper-left inset panel.
Paper: MaNGA DynPop. VII. A Unified Bulge–Disk–Halo Model for Explaining Diversity in Circular Velocity Curves of 6000 Spiral and Early-type Galaxies
Authors: Kai Zhu, Michele Cappellari, Shude Mao, Shengdong Lu, Ran Li, Yong Shi, David A. Simon, Youquan Fu, Xiaohan Wang
Figure caption: Similar to Figure 5, but adopting an alternative extreme assumption that all galaxies have infinitely thin exponential disks (K. C. Freeman 1970).
Paper: MaNGA DynPop. VII. A Unified Bulge–Disk–Halo Model for Explaining Diversity in Circular Velocity Curves of 6000 Spiral and Early-type Galaxies
Authors: Kai Zhu, Michele Cappellari, Shude Mao, Shengdong Lu, Ran Li, Yong Shi, David A. Simon, Youquan Fu, Xiaohan Wang
Figure caption: Similar to Figure 5, but using a fixed nSer,bulge = 2.83 that corresponds to a Hernquist profile in the inner region (Appendix A and Figure A1 in E. Vitral & G. A. Mamon 2020). The trends of the CVC shape changing with σe still exist, but the BDH model-predicted curves tend to overestimate at the low σe end and underestimate at the high σe end.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: Double superposed epoch analysis of various parameters for (first–third columns) long-duration (duration ≥ 4 hr) radial, tangential, and normal IMF events, in the time frame of −12 to +15 hr with zero epoch at the start time and with +3 hr epoch at the end time of each event. (From top to bottom) Radial, tangential, and normal components of the proton bulk velocity, proton number density, proton temperature, alpha particle abundance, and IMF magnitude. Their median values and upper/lower quartile values in 1 hr epoch bins are plotted by circles and upper/lower envelopes, respectively. For this analysis, the isolated events are selected, and the rescaling and interpolation of the data in these events are made (see text for details). For each IMF configuration type, the number of isolated events (Niso) is denoted in parentheses above the first row panel, while the numbers of isolated events used for the analyses of proton parameters (Niso,p), alpha particle abundance (Niso,p&α), and IMF magnitude (Niso,B) are denoted in the first, sixth, and seventh column panels, respectively. The long-duration non-Parker spiral IMF events for each unsigned configuration type are only in the area shaded in gray from 0 to +3 hr epoch times.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: Schematic illustration of configurations of the radial IMF (red) and tangential IMF (blue) at the observation point (r = 1 au) at T = t, which are formed by the combined effect of tangential deflection of the solar wind (﹩{{\boldsymbol{V}}}_{T}﹩) and linear velocity of the solar rotation (﹩{{\boldsymbol{v}}}_{{\rm{rot}}}={\boldsymbol{\Omega }}\times {\boldsymbol{r}}﹩) at the source region (﹩{{\boldsymbol{r}}}_{0}﹩; close to the Sun) at T = t0, that is, ﹩{{\boldsymbol{V}}}_{T,0}﹩ and ﹩{{\boldsymbol{v}}}_{{\rm{rot}},0}﹩ (﹩=\,{\boldsymbol{\Omega }}\times {{\boldsymbol{r}}}_{0}﹩). The tangential deflection of the solar wind can behave as the local difference of the angular speed at the source region from the angular speed of the Sun (simply Ω′ < Ω for the eastward solar wind deflection cases and Ω′ > Ω for the westward solar wind deflection cases). The dashed line marks the radial direction between the source region at T = t0 (white circle) and the observation point at T = t (green circle) with t  > t0. As a baseline, the typical Parker spiral IMF that passes through the observation point is plotted by the dotted line. For simplicity, it is assumed that the Sun rotate like rigid body. The suborientations of the IMF configuration are not denoted here. Sizes are not to scale.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: (Top) The percentages of the number of data points for radial, tangential, and normal IMF conditions (different columns) identified in the time intervals of 446 ICMEs (left-side bars) and non-ICMEs (right-side bars) in 1995–2023. The numbers of (1 hr resolution) Wind/MFI data available during the time intervals of ICMEs (nICME) and non-ICMEs (nNon-ICME) are used for normalization for each. (Bottom) Those identified in the time intervals of 865 SIRs (left-side bars) and non-SIRs (right-side bars) in 1995–2016. The numbers of Wind/MFI data available during the time intervals of SIRs (nSIR) and non-SIRs (nNon-SIR) are used for normalization for each. The values denoted by n1995–2023 in the first column on the top and n1995–2016 in the first column on the bottom indicate the numbers of available Wind/MFI data measured at PX-GSE ≥ +50 RE, respectively, in 1995–2023 and 1995–2016.
Paper: Non-Parker Spiral Interplanetary Magnetic Field Configurations Observed in Near-Earth Space: Statistical Features of Their Occurrence and Solar Wind Conditions
Authors: Jong-Sun Park, Quanqi Shi, Jungjoon Seough, Hui Zhang, Tao Tang, Ruilong Guo, Kyung-Suk Cho, Dong-Hun Lee, Khan-Hyuk Kim
Figure caption: Double superposed epoch analysis of the tangential velocity components of the proton bulk velocity for long-duration (duration ≥ 4 hr) events of (a) outward IMF, (b) inward IMF, (c) westward IMF, and (d) eastward IMF. The medians and upper/lower quartiles are plotted in the same format as Figure 7. The long-duration outward and inward IMF events are segmented in the isolated events of the unsigned long-duration radial IMF, while the long-duration westward and eastward IMF events are segmented in those of the unsigned long-duration tangential IMF. The number of isolated events in the corresponding IMF configuration type is denoted by Niso in parentheses on the top of each panel. The number of these events used for the analysis is denoted by Niso,p in each panel.