adsabs/AstroCLIMB huggingface dataset:
Paper: Scale Invariance in Gamma-Ray Flares of the Sun and 3C 454.3
Authors: Fang-Kun Peng, Jun-Jie Wei, Hai-Qin Wang
Figure caption: Scale-invariance structure of gamma-ray flares of 3C 454.3. Cumulative distributions with q-Gaussian function (solid lines) for the differences of isotropic gamma-ray energies (E iso, upper left panel), peak luminosities (L P, upper right panel), duration times (lower left panel), and waiting times (lower right panel) for n = 1 (circles), n = 20 (crosses), and n = 40 (stars), respectively.
Paper: Solar Electron Beam—Langmuir Wave Interactions and How They Modify Solar Electron Beam Spectra: Solar Orbiter Observations of a Match Made in the Heliosphere
Authors: Camille Y. Lorfing, Hamish A. S. Reid, Raúl Gómez-Herrero, Milan Maksimovic, Georgios Nicolaou, Christopher J. Owen, Javier Rodriguez-Pacheco, Daniel F. Ryan, Domenico Trotta, Daniel Verscharen
Figure caption: Pitch-angle distributions of 33.4–54.2 keV electrons observed by EPT’s four sensors during the 2020 November 24 (a), 2021 October 9 (b), and 2022 April 15 (c) electron events.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: The derived properties with associated errors for the spectroscopic sample are shown with numbered markers plotted together with binary evolutionary models for donor stars in binary systems (Götberg et al. 2018). Stars in the LMC are marked using circles, stars in the SMC with squares, and the foreground object with a diamond. From top to bottom, we show the Kiel diagram, the spectroscopic Hertzsprung–Russell diagram, and effective radius as function of effective temperature. The left panels are for the LMC, and the right panels are for the SMC. The evolutionary models are for stars with initial masses of 4.5, 7.4, 9.0, 12.2, and 18.2  M ⊙, with corresponding stripped stellar masses of 1.1(1.2), 2.0(2.2), 2.7(2.9), 4.1(4.5), and 7.2(7.3) M ⊙ for the LMC (SMC). The central-helium burning is marked with a thicker and darker line, and the evolutionary tracks are cut at central-helium depletion.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: The normalized spectra of the stars in the observed spectroscopic sample, described in Sections 2 and 3. These stars are selected from the sample of Drout et al. (2023) and thought to be stars stripped of their hydrogen-rich envelopes via binary interaction. A few cosmic rays are visible as narrow emission features in the spectrum of Star 3.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: We use the presence of a set of nitrogen lines (top) and helium lines (bottom) to constrain the model grid used when fitting the observed spectra. As an example, we show here the models with surface hydrogen mass fraction X H,surf = 0.3, spread out in the temperature–surface gravity plane. Triangular markers show the presence of nitrogen or helium lines that are used to constrain the grid (see also Table 4). Gray circles indicate models in which none of the lines specified by the legend are present.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Effect of varying surface hydrogen/helium mass fraction (left), temperature (center), and surface gravity (right) on the spectral lines Hδ/He II λ4100 (first row), He II λ4542 (second row), He I λ5876 (third row), and N V λ4604 (fourth row). We use the model with T eff = 70 kK, ﹩{\mathrm{log}}_{10}g=5.0﹩ and X H,surf = 0.3 as a base (black solid line) and vary each parameter according to the legends.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: The stars in our spectroscopic sample, shown with numbered markers, match well with models of stars stripped in binaries (gray lines) in the Hertzsprung–Russell diagram. The left panel shows the stars from the LMC plotted together with models of Z = 0.006, and the right panel shows stars in the SMC plotted together with models of Z = 0.002. Star 26, which likely is a foreground object, is plotted using an assumed distance of 10 kpc and diamond-shaped markers. We label the zero-age main sequences and shade in gray the parts of the diagrams with cooler temperatures. WR stars in each of the clouds are shown using purple circles and a shaded region, while the expected locations of bright subdwarfs are marked with a green-shaded ellipse. The weak-wind WN3/O3 stars in the LMC are indicated using a lighter-purple color.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Coverage of the spectral model grid used as base for spectral fitting to obtain stellar properties of stripped stars. This visualization shows which models have reached convergence using a colored circle, where the small and large circles correspond to the temperature and surface gravity at optical depth τ = 20 and 2/3, respectively. Thin, dotted lines indicate where the Eddington factor is 0.1 (leftmost), 0.5 (middle), and 1 (rightmost).
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: The relation between mass and luminosity for stripped stars half-way through central-helium burning (X He,center ≡  0.5) is used to estimate the evolutionary mass. Here, we show the relation for stars stripped via stable mass transfer using evolutionary models from Götberg et al. (2018) for Z = 0.006 (pink line) and Z = 0.002 (dark red line). The shaded background color demonstrates the variation throughout helium-core burning when the central-helium mass fraction is between 0.8 and 0.1.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 1. See Appendix A for the fits of the remaining stars. See Table 3 for the derived temperature and surface gravity at optical depth τ = 20.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Contraction (top) and expansion (bottom) phases for stripped stars demonstrated using the Z = 0.006 stripped star models of Götberg et al. (2018), labeled by stripped star mass. We show the fraction of the stripped star duration using blue and pink shaded regions and the central-helium burning phase when 0.9 > X He,c > 0.01 using dark-gray background for the evolutionary tracks. The stars in the spectroscopic sample are plotted using their effective radii and bolometric luminosities with numbered markers (see Table 3). The top panel shows that contraction lasts ∼10% of the stripped star duration, while the bottom panel shows the expansion phase lasts ∼1%–5%. All stars but Star 16 agree with the helium-core burning phase and the expansion phase, while Star 16 could either be contracting or expanding.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Inferred emission rates of H-, He-, and He+-ionizing photons (Q 0, Q 1, and Q 2, respectively), plotted against each other to explore ionizing hardness for the stars in the spectroscopic sample and using numbered colored symbols. A large fraction (∼50%) of the H-ionizing photons are He-ionizing, but only a small fraction (∼0.001%–1%) are He+-ionizing. This shape of the SED is expected for stars with temperatures ∼50–100 kK, but remains to be observationally confirmed. For comparison, we also display models with Z = 0.006 for stripped stars by Götberg et al. (2018) using pale blue and labeled with the stripped star mass, along with models with Z = 0.4Z ⊙ from Smith et al. (2002) for OB-type main-sequence stars in dark gray, labeled by spectral types, and for WN-type WR stars in light gray, labeled by temperature in kilokelvin.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Rough estimates for the mass-loss rate upper limits (and tentative number in the case of Stars 1, 5 and 7) plotted as function of bolometric luminosity for the stars in the sample using colored and numbered symbols (because the symbols for Stars 2 and 4 are behind other markers, we label them above). We also plot the mass-loss rate prescriptions from Nugis & Lamers (2000), Krtička et al. (2016), Vink (2017), and Sander & Vink (2020) in beige, brown, light gray, and dark gray. We do not extrapolate the Krtička et al. (2016) scheme above 104 L ⊙ since these models were created for subdwarfs. For the Sander & Vink (2020) scheme, we only show Z = 0.006 since the lower-metallicity predictions are beyond the parameter space of the plot.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: The shape of the He II λ4686 spectral line is very sensitive to surrounding gas, and we, therefore, use it to estimate wind mass-loss rates. The observed He II λ4686 lines are shown from top to bottom for each star along with models for a range of wind mass-loss rates (﹩{\dot{M}}_{\mathrm{wind}}={10}^{-6}﹩ —red, 10−7—purple, 10−8—blue, 10−9—green, and 10−10 M ⊙ yr−1—yellow). The right column shows zoomed-in panels of the observed spectral lines, while the left column shows zoomed-out panels that also include the expectations for wind emission.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Comparison of the spectroscopic and evolutionary masses for the stars in the spectroscopic sample. The lines at 2.5  M ⊙ are meant as approximations for the limit for stripped stars that reach core collapse vs. those that evolve to white dwarfs.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 4.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 3.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 2.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 5.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Left: comparison of the mean radial velocity observed for Star 26 to known OB stars in the LMC (gray histogram). Horizontal “error bars” designate the range of radial velocities observed at different epochs. Right: comparison of the Gaia proper motions measured for Star 26 to likely LMC members (gray points). Other LMC stars presented in Drout et al. (2023) are shown as colored/numbered circles in both panels. Figures adapted from Drout et al. (2023).
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Best-fit models for Star 5 after having added the contribution from a 2.2  M ⊙ late B-type companion star, assuming it contributes 10% (top) and 20% (bottom) of the optical flux. While the 20% contribution results in a poor fit, the 10% contribution is acceptable and almost reproduces the effective temperature, surface gravity, and surface hydrogen mass fraction derived for Star 5.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Best-fit models for Star 6 after having removed the contribution from a 2.2  M ⊙ late B-type companion star, assuming it contributed 10% (top) and 20% (bottom) of the optical flux. In both examples, the fits are poor.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 16.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 6. We have clipped out the line cores of He II λ4339/Hγ, He II λ4860/Hβ, He II λ5412, and He II λ6563/Hα.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 26, assuming a foreground distance of 10 kpc.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 26, assuming it is a member of the LMC.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 7.
Paper: Stellar Properties of Observed Stars Stripped in Binaries in the Magellanic Clouds
Authors: Y. Götberg, M. R. Drout, A. P. Ji, J. H. Groh, B. A. Ludwig, P. A. Crowther, N. Smith, A. de Koter, S. E. de Mink
Figure caption: Fit for Star 8.
Paper: The Implication of the Helium-to-proton Flux Ratio in Galactic Cosmic Rays
Authors: Xiaojian Song, Xi Luo
Figure caption: (a) The variation of ﹩\mathrm{ln}(\mathrm{He}/{\rm{H}})﹩ as a function of ln(H) for particles at different rigidities (marked by different colors). The average values are subtracted from both the x and y axes. The data points are fitted by the straight line; the fit parameters and the linear correlation coefficient are given at the bottom. (b) The dependence of the parameter S on rigidity for different helium isotopes; the observed result is marked by error bars.
Paper: The Implication of the Helium-to-proton Flux Ratio in Galactic Cosmic Rays
Authors: Xiaojian Song, Xi Luo
Figure caption: Comparison between simulation (lines) and observation (filled circles) at four selected rigidities (marked by different colors). (a) The proton flux; (b) the helium flux; (c) the helium-to-proton flux ratio, which is normalized to the average value. Note that, restricted by the geomagnetic cutoff and instrumental effects, the centers of the lowest rigidity bins of proton and helium measured by AMS-02 are 1.08 and 1.815 GV, respectively.
Paper: The Implication of the Helium-to-proton Flux Ratio in Galactic Cosmic Rays
Authors: Xiaojian Song, Xi Luo
Figure caption: The dependence of S on k. The x and y axes show the power index of proton and helium phase space densities of the LIS, respectively. The asterisks denote the values of k He and k H used to fit the observation.
Paper: The Implication of the Helium-to-proton Flux Ratio in Galactic Cosmic Rays
Authors: Xiaojian Song, Xi Luo
Figure caption: The numerical results of p (n) k  n /n! (top) and q (n) k  n /n! (bottom) for different rigidities when k is set to the proper value −3. Their values are determined by the combination of λ, μ (represent by different colors), A/Z (represented by different line styles), and R 0 (marked in the title).
Paper: The Implication of the Helium-to-proton Flux Ratio in Galactic Cosmic Rays
Authors: Xiaojian Song, Xi Luo
Figure caption: The dependence of S  r  on k. The format is the same as in Figure 3.
Paper: The Implication of the Helium-to-proton Flux Ratio in Galactic Cosmic Rays
Authors: Xiaojian Song, Xi Luo
Figure caption: The format is the same as in Figure 2(a), but the data points are calculated using the customized LIS with k He = −3 and k H = −3, which differ from those for the real LIS.
Paper: Evidence of a Cloud–Cloud Collision from Overshooting Gas in the Galactic Center
Authors: Savannah R. Gramze, Adam Ginsburg, David S. Meier, Juergen Ott, Yancy Shirley, Mattia C. Sormani, Brian E. Svoboda
Figure caption: Velocity field (colors) and integrated-intensity contours (gray) from the NH3 (3,3) Mopra HOPS Survey (Walsh et al. 2011; Purcell et al. 2012; Longmore et al. 2017). The contour levels of the gray moment 0 are [0.2, 0.4, 0.6, 0.8, 1.5]. Green contours are from 70 μm Hi-GAL, with contour levels of [0.1, 0.2, 0.4, 0.6, 0.8] (Molinari et al. 2016). The magenta boxes outline the fields. The clouds G5a and G5b are labeled.
Paper: Evidence of a Cloud–Cloud Collision from Overshooting Gas in the Galactic Center
Authors: Savannah R. Gramze, Adam Ginsburg, David S. Meier, Juergen Ott, Yancy Shirley, Mattia C. Sormani, Brian E. Svoboda
Figure caption: Averaged spectra of 12CO 2 → 1 over the two fields defined in Figure 3. Top: Field 1, which contains emission from cloud G5a from velocities 50–200 km s−1 that continues down into Field 2 at a higher velocity, and also a line-of-sight H II region disassociated with G5 at a lower velocity. Bottom: Field 2, which contains emission from both clouds G5a and G5b. We identify G5a as associated with the emission from 75–200 km s−1, and G5b as the emission from 15–75 km s−1. G5b likely continues in emission to ∼0 km s−1, but overlap with line-of-sight emission from 12CO associated with the Galactic disk prevents it from being included.
Paper: Evidence of a Cloud–Cloud Collision from Overshooting Gas in the Galactic Center
Authors: Savannah R. Gramze, Adam Ginsburg, David S. Meier, Juergen Ott, Yancy Shirley, Mattia C. Sormani, Brian E. Svoboda
Figure caption: Geometry of the line of sight looking at the Milky Way’s Galactic bar, depicted as the blue ellipse bisected along its major and minor semi-axes. Not to scale. The dark-blue-dotted line is the line of sight to the center of the Galaxy, with the CMZ as the yellow ellipse. The solid green lines are lines of sight to the ends of the Galactic bar. The green-dotted line is the same angle from the center of the Galaxy line as the solid green line to the closer end of the bar. Going by this geometry, we conclude that features at the same angular distance from the Galactic center are not necessarily related to symmetrical features on the Galactic bar.
Paper: Evidence of a Cloud–Cloud Collision from Overshooting Gas in the Galactic Center
Authors: Savannah R. Gramze, Adam Ginsburg, David S. Meier, Juergen Ott, Yancy Shirley, Mattia C. Sormani, Brian E. Svoboda
Figure caption: View of the inner 12° of the Galactic plane. G5 at (ℓ, b) = (+5.4, −0.4) and Bania 1 (B1) at (ℓ, b) = (−5.4, +0.4) are circled in red. The first three panels illustrate NH3 (1,1), NH3 (3,3), and HC3N (2–1) from the Mopra HOPS survey (Walsh et al. 2011; Purcell et al. 2012; Longmore et al. 2017). The fourth panel illustrates 13CO (2–1) from the APEX SEDIGISM survey (Schuller et al. 2021). The last panel illustrates 850 μm from the ATLASGAL survey (Schuller et al. 2009).
Paper: Evidence of a Cloud–Cloud Collision from Overshooting Gas in the Galactic Center
Authors: Savannah R. Gramze, Adam Ginsburg, David S. Meier, Juergen Ott, Yancy Shirley, Mattia C. Sormani, Brian E. Svoboda
Figure caption: Integrated-intensity maps of the surveyed region of G5. First row: left image shows 12CO J = 2 → 1, right image shows 13CO J = 2 → 1. Second row: C18O J = 2 → 1, SiO J = 5 → 4. Third row: H2CO J = 322 → 221, H2CO J = 303 → 202. The contours are the integrated intensity with five contours evenly spaced between the 0.25th and 99.75th percentiles.
Paper: Switchbacks and Associated Magnetic Holes Observed near the Alfvén Critical Surface
Authors: Anthony P. Rasca, William M. Farrell, Jacob R. Gruesbeck, Robert J. MacDowall, Stuart D. Bale, Justin C. Kasper
Figure caption: Summaries of the magnetic field and Alfvén Mach number profiles. (a) and (b) E8 profiles for B  r  and ∣B∣ (left) and M A (right). Shaded regions correspond to switchback patches P1–P3 and the sub-Alfvénic region. (c) and (d) E12 profiles for B  r  and ∣B∣ (left) and M A (right). Shaded areas correspond to the super-Alfvénic switchback patch (blue) and the E12 sub-Alfvénic region (red).
Paper: Switchbacks and Associated Magnetic Holes Observed near the Alfvén Critical Surface
Authors: Anthony P. Rasca, William M. Farrell, Jacob R. Gruesbeck, Robert J. MacDowall, Stuart D. Bale, Justin C. Kasper
Figure caption: Co-added B  r , V  r , and ∣B∣ profiles from the superposed epoch analyses for switchback boundaries sample populations for P1–P3 and the sub-Alfvénic region during E8. The top panels correspond to switchback entries (step-ups during E1) and the bottom panels correspond to switchback exits (step-downs). Mean measurement changes at the switchback boundaries are indicated. While evidence of MHs at switchback boundaries is evident during P1–P3, the MHs do not occur frequently enough the appear in the co-added ∣B∣ profiles during the sub-Alfvénic region.
Paper: Switchbacks and Associated Magnetic Holes Observed near the Alfvén Critical Surface
Authors: Anthony P. Rasca, William M. Farrell, Jacob R. Gruesbeck, Robert J. MacDowall, Stuart D. Bale, Justin C. Kasper
Figure caption: The change in ∣B∣ as a function of M A for E8 (left) and E12 (right). (a) and (b) All points color coded for P1–P3 and the sub-Alfvénic region during E8 and the super-Alfvénic switchback patch and sub-Alfvénic region for E12. (c) and (d) All points corresponding to an SBI>3000 nT km s−1. (e) and (f) All points corresponding to switchback boundaries used in the E8 and E12 superposed epoch analyses.