adsabs/AstroCLIMB huggingface dataset:
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Evolution with time (Interval 4) over the northeast limb from SDO (top) the prominence maximum height, h  m , and (bottom) corresponding limb angle, ﹩{B}_{m}^{* }﹩. Points in light gray indicate the times and longitudes where a small filament surge affects the results (between relative times t = 206 hr and t = 221 hr). The vertical line corresponds to t = 215.5 hr. Time is expressed in hours from 2011 March 14 00:00 UT.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Automated detection results (AIA) for a set of synoptic images (March 19 at 17:30 UT). (a) The eight detection results are combined to give an overall detection map. Increasing heat level is used to show increased detection frequency. (b) The combined result is converted to a binary map, using a threshold value of 3. (c) The detected prominences.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Evolution with time (Interval 5) over the northeast limb from STEREO-A (circles) and northwest limb at STEREO-B (triangles) of (top) the prominence maximum height, h  m , and (bottom) corresponding limb angle, ﹩{B}_{m}^{* }﹩. Time is expressed in hours from 2011 March 14 00:00 UT. The hatched region denotes the relative time interval of the prominence eruption, between t = 328 hr and t = 335 hr, which corresponds to between March 27 at 16:00 and 23:00 UT, respectively.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: (a) Spacecraft locations on 2011 March 27 at 16:06 UT, in the ecliptic plane (viewed from above, with the Sun at the center): (1) SDO, (2) STEREO-A, and (3) STEREO-B. The angular coordinate gives the Carrington longitude; the radial coordinate is in astronomical units. The magnetic field lines at each spacecraft are estimated based on an ideal Parker heliospheric magnetic field (E. N. Parker 1958; J. Gieseler et al. 2023), assuming a solar wind speed of 400 km s−1. (b)–(d) Erupting prominence at 16:06 UT, shown in the 304 Å channel of (b) STEREO-B/EUVI, (c) SDO/AIA, and (d) STEREO-A/EUVI.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Automated detection results (STEREO-A/EUVI) for a set of synoptic images (March 25 at 16:14 UT) I  λ , in units of DN s−1. In each case, λ denotes the bandpass wavelength, in Å. (a) Normalized ratio image I 304/I 195. Small upper and lower percentiles of the ratio are removed prior to normalization to exclude extreme values. (b)–(d) Pixels that appear bright in I 304 but dark in (b) I 171, (c) I 195, and (d) I 284. (e) The detected prominences.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: (Left) The large prominence, shown in the 304 Å channel of SDO/AIA toward the northeastern limb. (Right) Eruption of filament material overlapping with the line-of-sight observation of the prominence over the limb. The images correspond respectively to relative times t = 137.5 and 215.5 hr.
Paper: Testable Predictions of Outside-in Age Gradients in Dwarf Galaxies of All Types
Authors: Claire L. Riggs, Alyson M. Brooks, Ferah Munshi, Charlotte R. Christensen, Roger E. Cohen, Thomas R. Quinn, James Wadsley
Figure caption: Both panels show dark matter density slope vs. age gradient (﹩{{dt}}_{90}/{f}_{{R}_{e}}﹩) for simulated galaxies. Stars denote satellite galaxies, while circles denote field galaxies. The left panel is colored by stellar mass. In the left panel, it is evident that the core slope varies as expected with stellar mass; halos with lower stellar mass are “cuspy,” while increasing mass leads to a “cored” profile. This trend extends somewhat to the age gradient; lower-mass “cuspy” halos have flat age gradients, while higher-mass “cored” halos have some of the steepest negative age gradients. The right panel focuses on the mid- to high-mass halos and colors by global t 90 value. Open symbols with no color are galaxies with t 90 < 8 Gyr. Here it shows that among “cored” halos, those with the steepest age gradients tend to have a t 90 value closer to ≈8 Gyr, while the flatter age gradients tend to have t 90 closer to z = 0. The example galaxies shown in Figure 2 are outlined in red in both panels and labeled with text in the left panel. Overall, we interpret these trends as evidence that dark matter core formation correlates with age gradient for the lower-mass galaxies, but that for the higher-mass dwarfs with cores, t 90 instead dominates the age gradient.
Paper: Testable Predictions of Outside-in Age Gradients in Dwarf Galaxies of All Types
Authors: Claire L. Riggs, Alyson M. Brooks, Ferah Munshi, Charlotte R. Christensen, Roger E. Cohen, Thomas R. Quinn, James Wadsley
Figure caption: Here we recreate Figure 1 but use t 50 instead of t 90. We show the age gradient ﹩{{dt}}_{50}/{f}_{{R}_{e}}﹩ vs. global t 50 in gigayears since the Big Bang. We calculate ﹩{{dt}}_{50}/{f}_{{R}_{e}}﹩ as we did for ﹩{{dt}}_{90}/{f}_{{R}_{e}}﹩, now using the time when the galaxy or annulus formed 50% of its stellar mass. Each point represents a simulated galaxy, with circles representing field dwarfs and stars representing satellite galaxies, with colors corresponding to the stellar mass of the galaxy. Light blue diamonds correspond to the galaxies presented in A. S. Graus et al. (2019), and green triangles correspond to a subset of galaxies presented in R. E. Cohen et al. (2024, in preparation). Unlike the data in Figure 1, we do not find a strong correlation in the ﹩{{dt}}_{50}/{f}_{{R}_{e}}﹩ age gradient with global t 50. This is in contrast to A. S. Graus et al. (2019), who find a strong age gradient trend using both t 50 and t 90. We infer this to mean that the age gradients in our simulated galaxies are established at later times (lower z) than those in A. S. Graus et al. (2019).
Paper: Testable Predictions of Outside-in Age Gradients in Dwarf Galaxies of All Types
Authors: Claire L. Riggs, Alyson M. Brooks, Ferah Munshi, Charlotte R. Christensen, Roger E. Cohen, Thomas R. Quinn, James Wadsley
Figure caption: The left panel shows the average radius enclosing 90% of the star formation over time normalized to the effective radius at z = 0, while the right panel shows the effective radius normalized to the effective radius at z = 0. We exclude satellites from this plot because their size evolution may be impacted by their evolution within a parent halo. Field galaxies are split up according to their age gradient value. We define a flat gradient as a gradient with a ﹩{{dt}}_{90}/{f}_{{R}_{e}}﹩ value above the average ﹩{{dt}}_{90}/{f}_{{R}_{e}}﹩ value of our sample, −1.95 Gyr, while a steep gradient is a gradient with a ﹩{{dt}}_{90}/{f}_{{R}_{e}}﹩ value less than or equal to −1.95 Gyr. Furthermore, the sample of field galaxies with flat age gradients is split into high mass and low mass, with a cutoff at 105.8 M ⊙. This is because smaller galaxies with a flat gradient have a flat gradient because they quench early, not because recent star formation erases their gradient. In both panels, the shaded lines show the data within 68% of the average value. Overall, both panels show evidence that massive dwarfs with flat age gradients at z = 0 started off smaller than their counterparts with steep gradients but overtook them more at recent times.
Paper: Testable Predictions of Outside-in Age Gradients in Dwarf Galaxies of All Types
Authors: Claire L. Riggs, Alyson M. Brooks, Ferah Munshi, Charlotte R. Christensen, Roger E. Cohen, Thomas R. Quinn, James Wadsley
Figure caption: Here we examine two galaxies run with different star formation physics: h516 and h516lt. h516 is run with a high star formation density threshold (requiring the presence of H2) and forms a dark matter core, while h516lt has a low density threshold for star formation and does not form a core. We remake the left and middle panels from Figure 2 for these two galaxies. We also label the stellar mass, effective radius, age gradient, and global t 90 value. We find that only h516 has significant reshuffling of its oldest stars, consistent with the idea that the same process that creates dark matter cores also reshuffles the stars.
Paper: Testable Predictions of Outside-in Age Gradients in Dwarf Galaxies of All Types
Authors: Claire L. Riggs, Alyson M. Brooks, Ferah Munshi, Charlotte R. Christensen, Roger E. Cohen, Thomas R. Quinn, James Wadsley
Figure caption: Radial distribution of gas and stars of each halo with a major merger in its history. The black, dark gray, and light gray colors represent stars, gas that turned into stars, and gas particles of the primary halo involved in the merger, and the varying shades of pink represent the same from the secondary halo involved in the merger. Note that Storm halo 1 had more than one merging halo. We show the contribution from the secondary only; the white space represents contributions from a smaller, tertiary halo.
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: Upper panel: spectrum 1 of HZ Dra observed on 2021 June 5. Bottom panel: spectrum 2 obtained on 2021 June 12. The black and red lines represent the observed and fitted spectra, respectively. The four Balmer absorption lines H δ , H γ , H β , and H α  are also marked.
Paper: Testable Predictions of Outside-in Age Gradients in Dwarf Galaxies of All Types
Authors: Claire L. Riggs, Alyson M. Brooks, Ferah Munshi, Charlotte R. Christensen, Roger E. Cohen, Thomas R. Quinn, James Wadsley
Figure caption: A recreation of Figure 1, but only the halos with a major merger are colored and identified. The colors correspond to the time after the Big Bang of their most recent major merger.
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: Upper panel: the TESS light curves of HZ Dra (TJD = BJD − 2457000.0). Bottom panel: a section of the light curve is displayed in the enlarged panel.
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: The basic solutions for HZ Dra. Left panel: the relationship between q and the mean residuals ﹩\overline{{\rm{\Sigma }}}﹩ for W-D Mode 5; the red dot indicates the best q with the minimum mean residual. Right upper panel: the average light curve (black circles), the theoretical fit curve in the Ic  band with third light (the red solid line for Mode 5 and the green solid line for Mode 2), and the Roche lobe geometry of HZ Dra at phases 0.00, 0.25, 0.50, and 0.75, respectively. Right lower panel: the enlarged view of residuals for the average light curve (the red and green for Mode 5 and 2, respectively).
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: The O − C diagrams of HZ Dra. Top panel: the ﹩{\left(O-C\right)}_{1}﹩ values calculated by using Equation (1). The black dashed and solid lines indicate the model of a slash line plus LTTE (light travel-time effect); the slash-line model indicates that the ephemeris needs to be revised. The red and black dots refer to data from TESS, and the red pentagrams to data from the 60 cm telescope of the Yunnan Observatories of CAS. Middle panel: the ﹩{\left(O-C\right)}_{2}﹩ data of the mainly cyclical variation after subtracting the linear change from the ﹩{\left(O-C\right)}_{1}﹩ values. Bottom panel: the variations of the residual data of the middle panel.
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: Corner plot of the MCMC fitting code for the model of a slash line plus LTTE. Blue vertical lines indicate the median values of the histograms presented for each parameter. Posterior distributions at the 16% and 84% quantiles are shown by black vertical dashed lines. The units for A, P 3, ω, ΔT 0, ΔP 0, and d are days, years, degree, HJD, and days, respectively. In the plot, ﹩{mm}0=\tfrac{2\pi (2458683.4042-{T}_{3})}{365.25\times {P}_{3}}﹩.
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: The graphs of spot solutions obtained using the W-D program. Top panels: the average light curve (black circles), the calculated fitting light curves (red solid line), and the Roche lobe geometry. Spot parameters are also marked in these panels: latitude (θ, radians), longitude (ϕ, radians), angular radius (r, radians), temperature factor (T  f , the ratio of spot temperature to stellar temperature). Bottom panels: the enlarged views of the residuals.
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: Fourier amplitude spectra of the TESS light curve for HZ Dra. Top panel: the original spectrum. Middle panel: the residual spectrum. Bottom panel: the same as the middle panel, but for a different view. The red dotted lines represent the harmonics of the orbital frequency. The colored solid lines represent the six highest-amplitude multiplets.
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: The variations of Max II and Max I and Max II − Max I.
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: One sector of the TESS light curve fitted by the tenth-order Fourier series of the orbital frequency. The black dots refer to the TESS light curve. The green solid line represents the fitting light curve. The pink dots refer to the fitting residuals.
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: Echelle plot of all frequencies above 3 day−1 vs. the modulo the orbital frequency. The colored solid lines are the same as those in the bottom panel of Figure 10.
Paper: Evidence for a Close-in Tertiary Orbiting around the Algol-type System HZ Dra with Tidal Splitting and Spots Activities
Authors: Ping Li, Wen-Ping Liao, Sheng-Bang Qian, Lin-Jia Li, Qi-Bin Sun, Xiang-Dong Shi, Azizbek Matekov, Qi-Huan Zeng, Zhao-Long Deng, Xiao-Hui Fang
Figure caption: The energy required to produce the periodic variation in the O − C diagram using the Applegate mechanism model.
Paper: Mass Function of Stellar Black Holes as Revealed by the LIGO–Virgo–KAGRA Observations
Authors: Xiao-Fei Dong, Yong-Feng Huang, Zhi-Bin Zhang, Xiu-Juan Li, Ze-Cheng Zou, Chen-Ran Hu, Chen Deng, Yang Liu
Figure caption: Distribution of the BH masses and redshifts. Left panel: mass vs. redshift for the premerger sample. The crosses and open circles represent the lighter (m 2) and heavier (m 1) BHs, respectively. Right panel: mass vs. redshift for the postmerger sample. In both panels, the dashed line represents the truncation limit, and the solid line is the baseline used in our statistical analysis.
Paper: Mass Function of Stellar Black Holes as Revealed by the LIGO–Virgo–KAGRA Observations
Authors: Xiao-Fei Dong, Yong-Feng Huang, Zhi-Bin Zhang, Xiu-Juan Li, Ze-Cheng Zou, Chen-Ran Hu, Chen Deng, Yang Liu
Figure caption: Mass function of BHs. The thin solid line represents the premerger sample, and the thick solid line represents the postmerger sample. Both samples are normalized by the maximum value of the function, respectively. The thin and thick dashed lines represent the best-fitting results by using a broken power-law function correspondingly.
Paper: Mass Function of Stellar Black Holes as Revealed by the LIGO–Virgo–KAGRA Observations
Authors: Xiao-Fei Dong, Yong-Feng Huang, Zhi-Bin Zhang, Xiu-Juan Li, Ze-Cheng Zou, Chen-Ran Hu, Chen Deng, Yang Liu
Figure caption: Testing the nonparametric method by expanding the observed BBH sample to a much larger mock BBH sample. Left panel: distribution of the mock BHs on the mass–redshift plane. The crosses and open circles represent the lighter (mock m 2) and heavier (mock m 1) BHs, respectively. Right panel: number density vs. redshift derived from the mock BHs. The solid step line represents the results derived directly by using our method. The dashed–dotted line represents the best-fit power-law function.
Paper: Mass Function of Stellar Black Holes as Revealed by the LIGO–Virgo–KAGRA Observations
Authors: Xiao-Fei Dong, Yong-Feng Huang, Zhi-Bin Zhang, Xiu-Juan Li, Ze-Cheng Zou, Chen-Ran Hu, Chen Deng, Yang Liu
Figure caption: Testing the nonparametric method by using completely simulated BBH events. Left panel: distribution of the mock BHs on the mass–redshift plane. The crosses and open circles represent the lighter (mock m 2) and heavier (mock m 1) BHs, respectively. Right panel: number density vs. redshift derived from the mock BHs. The dashed–dotted line represents the best-fit power-law function.
Paper: Mass Function of Stellar Black Holes as Revealed by the LIGO–Virgo–KAGRA Observations
Authors: Xiao-Fei Dong, Yong-Feng Huang, Zhi-Bin Zhang, Xiu-Juan Li, Ze-Cheng Zou, Chen-Ran Hu, Chen Deng, Yang Liu
Figure caption: The number density of BHs vs. redshift. The thick step line represents the premerger sample, and the thin step line represents the postmerger sample. The dashed–dotted line and the dashed line represent the best-fitting results of the premerger sample and the postmerger sample, respectively, by using a simple power-law function.
Paper: Mass Function of Stellar Black Holes as Revealed by the LIGO–Virgo–KAGRA Observations
Authors: Xiao-Fei Dong, Yong-Feng Huang, Zhi-Bin Zhang, Xiu-Juan Li, Ze-Cheng Zou, Chen-Ran Hu, Chen Deng, Yang Liu
Figure caption: Cumulative redshift distribution of BHs. The solid line represents the premerger sample, and the dashed line represents the postmerger sample. The two curves are essentially overlapping each other.
Paper: Mass Function of Stellar Black Holes as Revealed by the LIGO–Virgo–KAGRA Observations
Authors: Xiao-Fei Dong, Yong-Feng Huang, Zhi-Bin Zhang, Xiu-Juan Li, Ze-Cheng Zou, Chen-Ran Hu, Chen Deng, Yang Liu
Figure caption: Distribution of the BH masses and redshifts after correcting for the selection effect. Left panel: mass vs. redshift for the premerger sample. The crosses and open circles represent the lighter (m 2) and heavier (m 1) BHs, respectively. Right panel: mass vs. redshift for the postmerger sample.
Paper: Observations of Preferential Heating and Acceleration of α-particles in the Young Solar Wind by Parker Solar Probe
Authors: Jingyu Peng, Jiansen He, Die Duan, Daniel Verscharen
Figure caption: Variations in the α-to-proton temperature ratios and drift speeds as functions of the radial distance (left column) and Coulomb collision number (right column). Panels (a)–(d) show the count distribution in each bin. Panels (e) and (f) display the average temperature ratio ﹩\tfrac{{T}_{\alpha }}{{T}_{p}}﹩, with its average value indicated by the color bar. Panels (g) and (h) depict the average α-particle temperature anisotropy ﹩\tfrac{{T}_{\alpha \perp }}{{T}_{\alpha \parallel }}﹩, while panels (i) and (j) show the average proton temperature anisotropy ﹩\tfrac{{T}_{p\perp }}{{T}_{p\parallel }}﹩. The color saturation of the bins in panels (e)–(j) is determined by the number of counts in each bin, with a threshold set at C 0 = 100. In panels (a) and (c), the black solid curves represent the median of ﹩\tfrac{{T}_{\alpha }}{{T}_{p}}﹩ and ﹩\left|\tfrac{{V}_{\alpha p}}{{V}_{{\rm{A}}}}\right|﹩ within the segmented heliocentric distance range, and the error bars represent the local first and third quartiles. The black dashed line in panel (c) marks the position of zero drift speed.
Paper: Observations of Preferential Heating and Acceleration of α-particles in the Young Solar Wind by Parker Solar Probe
Authors: Jingyu Peng, Jiansen He, Die Duan, Daniel Verscharen
Figure caption: Distribution in the two-dimensional parameter space of ﹩\tfrac{{V}_{\alpha p}}{{V}_{{\rm{A}}}}﹩ and ﹩\tfrac{{T}_{\alpha }}{{T}_{p}}﹩ as observed by PSP and Helios at different heliocentric distances. The color in the first row indicates the number of counts in each bin, while the color in the second row indicates the logarithm of the Coulomb collision number N C, and the color saturation indicates the ratio of the count number to a threshold count number (C 0), with C 0 = 100 for PSP data and C 0 = 10 for Helios data. The three columns from left to right correspond to the results of PSP, Helios within 0.5 au, and Helios beyond 0.5 au. The red dotted lines in (a)–(c) represent the linear fit results for ﹩\tfrac{{T}_{\alpha }}{{T}_{p}}﹩ and ﹩\left|\tfrac{{V}_{\alpha p}}{{V}_{{\rm{A}}}}\right|﹩, this fit is performed within the range of ﹩\left|\tfrac{{V}_{\alpha p}}{{V}_{{\rm{A}}}}\right|﹩ marked by the red dashed line. The black dashed curves in (a), (b), and (c) represent isocontours of constant maximum growth of the FM/W instability in terms of the drift speed, which are plotted based on Equation (29) with the parameters β  p∥ and ﹩\tfrac{{T}_{\alpha \perp }}{{T}_{\alpha \parallel }}﹩ being adopted in line with the average PSP/Helios observations in each bin, and we set ﹩\tfrac{{n}_{\alpha }}{{n}_{p}}﹩ to 0.05.