adsabs/AstroCLIMB huggingface dataset:
Paper: Material Properties of Organic Liquids, Ices, and Hazes on Titan
Authors: Xinting Yu, 婷 余馨, Yue Yu, 越 于, Julia Garver, Jialin Li, 霖 李嘉, Abigale Hawthorn, Ella Sciamma-O'Brien, Xi Zhang, Erika Barth
Figure caption: Comparison of the selected l-g SVP functions in Table 3 to the other evaluated l-g SVP functions in Table A1, for the first half of the species in Table 1. The notations are the same as in Figure 3. Similar to Figure 3, the different SVP functions agree relatively well for the applicable temperature range, and they start to deviate from each other for the extrapolated temperature range.
Paper: Catalog of Planetary Nebulae Detected by GALEX and Corollary Optical Surveys
Authors: M. A. Gómez-Muñoz, L. Bianchi, A. Manchado
Figure caption: Left panels: color–color diagrams for optically extended PNs (blue crosses), optically pointlike PNs (green pluses), UV pointlike PNs (green circles), CSPNs of extended PNs (black upward triangles), and known binary CSPNs (red dots; see the text). The CSPN photometry in Tables 2 and 3 is used for the CSPNs of extended PNs. The purple/black density maps are pointlike/extended sources, respectively, from the matched GALEXxSDSS sample from Bianchi & Shiao (2020); from their work, we also took the model colors shown in the plots. The purple sequence of stellar model colors (labeled “WD”) is for ﹩\mathrm{log}g=7.0﹩. MS (red) and supergiant (cyan) sequences are for stellar model colors with solar ﹩\mathrm{log}g=5.0﹩ and ﹩\mathrm{log}g=3.0﹩, respectively, and binaries composed of WD+MS are for WD stars of R WD = 0.01 R ☉ (pink solid line) and R WD = 0.1 R ☉ (pink dashed line), for different MS spectral types. Galaxy templates of representative types (E0–Irr, Im; green solid line) are also shown. A reddening vector for E(B − V) = 0.3 mag is shown in the upper right corner of each panel. Right panels: same as the left panels, but with a reduced range to enhance the binary CSPN region (black and dashed line regions).
Paper: Catalog of Planetary Nebulae Detected by GALEX and Corollary Optical Surveys
Authors: M. A. Gómez-Muñoz, L. Bianchi, A. Manchado
Figure caption: Distribution of the GALEX-SDSS (blue) and the GALEX-PS1 (orange) best-match coordinate separations. About 88% of the separations are smaller than the GALEX resolution (5″).
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Equatorial view (top) and projection (bottom) on the solar surface of Earth, STA, and STB locations on 2011 November 3 superposed on a background image showing the distribution of the radial magnetic field. The pink arrows denote the directional axis of the shock geometry, or the shock front, found by the ellipsoid model. The curves are magnetic field lines that connect to the three locations. The yellow hatched areas indicate the latitude–longitude coverage of the CME shock at the time 23:40 UT (single hatched) and after November 4 05:54 UT (double hatched). A shift (60°) of the heliocentric Earth equatorial (HEEQ) coordinate system in longitude is used, with the Earth located at 60° in longitude to match the magnetogram plots published by the Global Oscillation Network Group (GONG) of National Solar Observatory (NSO).
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Coronagraph observations of the 2011 November 3 CME from three vantage locations at SOHO, STA, and STB (from left to right) and their fits to a 3D ellipsoid model. Overplotted is the ellipsoid model that represents the 3D geometry of the shock. Red, orange, blue, and cyan lines refer to the four quadrants of the ellipsoid. White lines are used to indicate the surface of the ellipsoid.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Ellipsoid CME shock surfaces (yellow color) at selected time intervals and their intersections (black circles) with the magnetic field lines to Earth (green), STA (red), and STB (blue). Note that the scales in the bottom row differ from the rest.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Top row: simulated time profiles of SEP proton flux expected at Earth (0°), STA (HEEQ longitude 105°), and STB (255°) for various energies as indicated in the graph. The solid lines are color coded to approximately match the observed time–intensity profile in Figure 5 without consideration of energy. The arrows indicate the time of the energy spectra. Bottom row: the simulation assumes a constant radial particle mean free path of λ  r  = 200 R ⊙(p/(GqV/c))1/3 and an α ⊥ = 0.37 for perpendicular diffusion κ ⊥.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Onset time as a function of c/v and linear fit. Data points for STA, STB, and SOHO observations are taken from Gómez-Herrero et al. (2015) and Prise et al. (2014). The SOHO points only contain three electron channels. The left panel is based on a run with a large mean free path λ  r  = 200 R ⊙(p/(GqV/c))1/3, and the right panel contains a run with a small mean free path λ  r  = 20 R ⊙(p/(GqV/c))1/3.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Top: calculated peak flux (red histogram) of 36 MeV protons as a function of longitude in comparison with the observed peak fluxes in similar energy channels at the three spacecraft locations (symbols). The black curve at the top panel is a Gaussian distribution fitted to the observed peak fluxes. Bottom: peak flux time (blue color) and onset time (red color) as a function of longitude together with data from observations (symbols). The simulation results are obtained from the runs with a large mean free path λ  r  = 200 R ⊙(p/(GqV/c))1/3 and an α ⊥ = 0.37 for perpendicular diffusion coefficient κ ⊥.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Proton fluxes at selected energy levels between ∼1 and ∼50 MeV observed by SOHO/ACE at Earth’s L1 point, STA, and STB during the 2011 November 3 SEP event. The dotted traces are simulation results of absolute SEP fluxes for the three locations from one model run with a common set of model parameters.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: From top to bottom: radial distance (r shf), normal shock speed relative to upstream plasma (V  n1), upstream Alfvén speed (V A), Alfvén Mach number (M A), fast magnetosonic Mach number (M  S ), and shock compression ratio (R) at the CME shock front along the ellipsoid axis as a function of time. The color shade regions in the top panel indicate the time when STA and/or STB are connected to the shock.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Proton fluxes at selected energy levels between ∼1 and ∼50 MeV observed by STA. The dotted traces are simulation results with mean free paths fine-tuned to match the observation individually in each energy channel.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Calculated flux of 36 MeV protons as a function of time and longitude obtained from the simulation runs with a large mean free path λ  r  = 200 R ⊙(p/(GqV/c))1/3 and an α ⊥ = 0.37 for perpendicular diffusion coefficient κ ⊥.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Same as Figure 6, but for smaller radial mean free path of λ  r  = 20 R ⊙(p/(GqV/c))1/3 and smaller α ⊥ = 0.074 for perpendicular diffusion κ ⊥.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Average energy spectra at STA. The energy of simulated fluxes needs to be scaled as 100(E/100 MeV)0.6 MeV to fit the observation.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Top: equatorial distribution of particle source within ±10° latitude released at the CME shock that contributed to 36 MeV proton fluxes expected to be seen by SOHO, STA, and STB at 02:03 UT on 2011 November 4. The abrupt cutoff of source particles beyond ∼15 R ⊙ is because they have not arrived yet. The second to fifth rows are shock properties: upstream Alfvén Mach number, sonic Mach number, obliquity, and solar wind density at the locations where the CME shock releases the particles for the calculated fluxes. The colored curves are magnetic field lines connected to the three spacecraft.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Top: peak flux of 36 MeV protons as a function of longitude. Bottom: peak flux time and onset time of 36 MeV protons as a function of longitude, together with data from observations. The results are obtained from the simulation runs with a small mean free path λ  r  = 20 R ⊙(p/(GqV/c))1/3 and an α ⊥ = 0.074 for perpendicular diffusion coefficient κ ⊥.
Paper: A Data-driven, Physics-based Transport Model of Solar Energetic Particles Accelerated by Coronal Mass Ejection Shocks Propagating through the Solar Coronal and Heliospheric Magnetic Fields
Authors: Ming Zhang, Lei Cheng, Ju Zhang, Pete Riley, Ryun Young Kwon, David Lario, Laura Balmaceda, Nikolai V. Pogorelov
Figure caption: Calculated flux of 36 MeV protons as a function of time and longitude obtained from the simulation runs with a small mean free path λ  r  = 20 R ⊙(p/(GqV/c))1/3 and an α ⊥ = 0.074 for perpendicular diffusion coefficient κ ⊥.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: NGSL stars are plotted in ﹩\mathrm{log}\,{T}_{\mathrm{eff}}﹩, ﹩\mathrm{log}\,g﹩ space. The previously published stars from proposals GO9088, GO9786, and GO10222 (pluses; Koleva & Vazdekis 2012) and the GO13776 stars (circles) are split by metallicity, metal poor (MP): [Fe/H] ≤ −1 (red), or metal rich (MR): [Fe/H] > −1 (blue). An approximate Eddington stability line and spectral-type boundaries are included in the plot as visual guides.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: CCD images of HD102212 using (a) G230LB, (b) G430L, and (c) G750L. Due to longer exposure time in the UV, the topmost panel shows the presence of cosmic-ray events whereas the bottom two do not have any significant ion contamination. It is worth noting for this cool star that what appears to be a stellar trace in the UV shortward of 2500 Å is actually light scattered from the visible portion of the spectrum into the UV by grating G230LB.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: The [Fe/H] distribution of all reduced targets in a stacked histogram. Blue corresponds to 345 targets from Koleva & Vazdekis (2012) and red corresponds to 169 targets from HST proposal GO13776.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Extracted and fluxed CCD/G750L spectrum of HD102212. The spectrum before defringing (black) is compared to the same spectrum after (red).
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: CMD for all 513 NGSL stars. The color bar shows the Mg2800 strength. Stars warmer than (B − V)0 = 0 or fainter than M  V  = 3.0 were considered dwarfs. For (B − V)0 > 0, any star with M  V  > 6.25 × (B − V)0 − 2.5 is considered a dwarf whereas M  V  < 6.25 × (B − V)0 − 2.5 is considered a giant. For dwarfs, Mg II emission fills in the absorption redder than B − V = 0.9, whereas emission begins to dominate for giants at B − V = 1.2.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Mg2800 vs. (B − V)0. Dwarfs (red) and giants (blue) are given different symbol types to denote metallicity groups: metal poor (crosses), intermediate (filled circles), and metal rich (unfilled triangles). Carbon star HD 54361 lies outside the plot limit and its position is indicated by a black arrow to the right.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Mg2800 as a function of [Fe/H] for a narrowed color range of 0.5 < (B − V)0 < 0.8. Dwarfs (crosses) and giants (circles) are color coded by (B − V)0. Black lines indicate Mg2800 from synthetic LTE spectra for dwarfs (T eff = 5770 K, ﹩\mathrm{log}\,g﹩ = 4.5, solid) and giants (T eff = 5770 K, ﹩\mathrm{log}\,g﹩ = 1.5, dashed).
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Mg2800 as a function of [Fe/H]. The color bar codes (B − V)0 and the symbol type distinguishes dwarfs (crosses) and giants (circles).
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Spectra of two stars, HD002857 (T eff  =  7607 K, the blue line) and HD102212 (T eff  =  3738 K, the black line), showing the feature band (green), blue side band (blue), and red side band (red) for our calculation of Mg2800 feature strength. The flux for HD002857 is scaled up by a factor of 10 for visual prominence. The hotter star (HD002857) and the cooler star (HD102212) has Mg2800 in absorption and emission, respectively.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: The fluxed spectrum of the star HD102212 in the UV region without any scattered-light correction (blue) and with scattered-light correction (red). It is seen that the spectrum is a little overcorrected in the region around 1800 Å.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Individual spectra for NGSL star HD190360 in the UV (blue and orange) illustrate the presence of bad pixels. After marking, the bad pixels were removed by the algorithm described in Section 3.7. The cleaned spectrum is also plotted (black). We elevated the errors for the corrected portions of the spectrum.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Typical cross correlation value as a function of pixel shift in angstroms, in this case for the red spectrum of the G0 V star HD 115383.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: A part of the spectrum for HD115383 (blue) showing a shift of the spectrum with respect to the template (red).
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Hα as a function of (B − V)0 for dwarfs (red) and giants (blue) is shown, segregated by metal-poor (crosses), intermediate (filled circles), and metal-rich (unfilled triangles) status. Be stars scatter to negative values for hot stars with (B − V)0 < 0. Any star caught during a flare event should also scatter toward negative index values. Four stars (three dwarfs and one giant) with Hα < −0.15 and (B − V)0 > 1.5 are thought to be flaring: GJ 551, GJ 876, and GL 109 are dwarfs while HD 126327 is a giant. Noise prevents reliable measurement of Mg2800 in GJ 551 (Proxima Centauri) and GJ 876. Therefore, these stars do not appear in figures that illustrate Mg2800. Carbon star HD 54361 lies outside the plot limit and its position is indicated by a black arrow to the right.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Inferred surface flux from Mg II 2800 (log10, cgs units) as a function of T eff for both giants (red) and dwarfs (blue) with T eff < 5000 K. The green line is the “basal flux” from Martínez et al. (2011). Three stars with ﹩\mathrm{log}\,(\mathrm{Flux})\lt 3.0﹩ (HD 54361, HD 126327, and HD 232078) are below the plot limits. The downward black arrows show ﹩\mathrm{log}10\,({T}_{\mathrm{eff}})﹩ for them. For comparison, the blackbody emergent flux integrated over the Mg2800 central passband (black line) is shown.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Spectra of five stars are shown in the λ2800 region. Top: fluxed spectra are normalized at 2820 Å. Bottom: fluxed spectra are normalized such that the continuum-subtracted emission scales as the surface-emergent emission F  λ  derived for Figure 18. “Normal” HD 136726 and HD 131918 lie near the green line in Figure 18 and the remaining three stars are low outliers. HD 232078 and carbon star HD 54361 lie outside the plot limits in Figure 18 and HD 126327 was caught during a flare event (Figure 14).
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Mg2800 is plotted against Hα for dwarfs (crosses) and giants (circles). The points are color coded by (B − V)0. Three stars to the extreme left of the figure are all Be stars: HD 37202, HD 109387, and HD 190073.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Spectra of two stars, HD221377 (T eff  =  6399 K, in upper panel (a)) and HD126327 (T eff  =  2874 K, in lower panel (b)), showing the feature band (green), blue side band (blue), and red side band (red) for our calculation of Hβ feature strength. For the hotter star (HD221377, upper panel (a)), we see clear absorption for Hβ whereas the lower panel (b) shows no apparent activity for Hβ for the cooler star (HD126327).
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Hβ as a function of (B − V)0 for dwarfs (red) and giants (blue), segregated by metal-poor (crosses), intermediate (filled circles), and metal-rich (unfilled triangles) status. Hβ is less sensitive to emission than Hα. Carbon star HD 54361 lies outside the plot limit and its position is indicated by a black arrow to the right.
Paper: HST Low-resolution Stellar Library
Authors: Tathagata Pal, Islam Khan, Guy Worthey, Michael D. Gregg, David R. Silva
Figure caption: Mg II 2800 feature in HD 102212 as observed by IUE (blue), in the NGSL (red), and by Worthey et al. (2022a) (green). The IUE spectrum is at lower resolution compared to Worthey et al. (2022a) and NGSL.
Paper: Parker Solar Probe Observations of High Plasma β Solar Wind from the Streamer Belt
Authors: Jia Huang, J. C. Kasper, Davin E. Larson, Michael D. McManus, P. Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, K. G. Klein, Weijie Sun, Bart van der Holst, Zhenguang Huang, Lan K. Jian, Adam Szabo, J. L. Verniero, C. H. K. Chen, B. Lavraud, Mingzhe Liu, Samuel T. Badman, Tatiana Niembro, Kristoff Paulson, M. Stevens, A. W. Case, Marc Pulupa, Stuart D. Bale, J. S. Halekas
Figure caption: Overview of the high plasma β streamer belt solar wind in E4. From top to bottom, the panels show plasma β, electron number density Ne and solar wind speed V p, proton temperatures, magnetic field components in RTN coordinates, radial magnetic field to total magnetic field strength ratio Br/∣B∣, normalized e-PAD at energy of 346.5 eV, angular distance to the HCS crossing ϕ HCS (degrees), alpha-to-proton abundance ratio Na/Np, and alpha–proton differential speed normalized by local Alfvén speed ΔVap/V A. In panel (b), we add 300 km s−1 to the solar wind speed. In panel (c), the perpendicular temperature (T ⊥p), parallel temperature (T ∥ p), and total temperature (T p) are indicated by red, blue, and black dots, respectively. Gray shaded regions 1 and 2 mark high plasma β solar winds around PCS crossings. The blue shaded region 3 is the HPS solar wind around the HCS crossing, as indicated by the red vertical dashed line. The blue vertical dashed lines represent the switchbacks in these high-β solar winds.