adsabs/AstroCLIMB huggingface dataset:
Paper: Hydrodynamic 3D Simulation of Roche Lobe Overflow in High-mass X-Ray Binaries
Authors: David Dickson
Figure caption: Mass flux through system zones. The L1 stream sums zones exceeding the maximal density of the supersonic wind at the L1 radius, 3 × 10−13 g cm−3. The lower mass zones on the spherical surface at the L1 radius around the donor are summed for the donor wind mass flux. Disk inflow corresponds to the net inflow through an accretor-centered spherical surface fully enclosing the disk. Accretion demarcates the net inflow through a spherical surface in the interdisk zone. The L1 stream and disk inflow mass fluxes of the 1.1 case are nearly identical across simulated time. The donor wind and external mass fluxes are nearly identical across simulation time in both cases. We exclude the settling time required to achieve a quasisteady state from initial conditions, in which fluxes were not generally observed nor physically meaningful.
Paper: Hydrodynamic 3D Simulation of Roche Lobe Overflow in High-mass X-Ray Binaries
Authors: David Dickson
Figure caption: Donor, tidal stream, and banded accretion disk visualized by an isodensity surface. The tidal stream is angled with respect to the line connecting centers of mass, and is centered on the ecliptic. View given from below the ecliptic to better image the stream impact shock front and the nonconservative outflow stream formed where the tidal stream collides with the disk.
Paper: Hydrodynamic 3D Simulation of Roche Lobe Overflow in High-mass X-Ray Binaries
Authors: David Dickson
Figure caption: 1D envelope-to-wind transition plotted in temperature and density. Photospheric density corresponds to an optical depth τ = 1, in keeping with the model O II atmosphere of R. Hainich et al. (2019). Wind launch density indicates where velocities become supersonic. Pink arrows labeled by ΦRL(1.01) and ΦRL(1.1) demarcate the effective potential offset of the Roche lobe relative to the donor radius for both 1.01 and 1.1 cases.
Paper: Exploring Waveform Variations among Neutron Star Ray-tracing Codes for Complex Emission Geometries
Authors: Devarshi Choudhury, Anna L. Watts, Alexander J. Dittmann, M. Coleman Miller, Sharon M. Morsink, Tuomo Salmi, Serena Vinciguerra, Slavko Bogdanov, Sebastien Guillot, Michael T. Wolff, Zaven Arzoumanian
Figure caption: Resultant hot spot shapes based on the geometry parameters prescribed in Table 1. Full animation sets showing the spot geometries as the star rotates are available in Zenodo. The purple-shaded regions represent the X-ray-emitting areas. The Ring-Eq, Ring-Polar, and Crescent-Eq spots are viewed from the observer inclination angle of 2.391 radians and include the effects of gravitational lensing. The darker latitude represents the equator for the three aforementioned configurations. The Crescent-Polar and Bithermal spots are viewed from the north pole and do not include lensing effects for visualization purposes. The lighter-shaded region of the Bithermal spot represents the ceding emission component. Doppler aberrations are not shown for any of the plots to make it easier to discern the spot shapes.
Paper: Memory in the Burst Occurrence of Repeating Fast Radio Bursts
Authors: Ping Wang, Li-Ming Song, Shao-Lin Xiong, Xiao-Yun Zhao, Jin Wang, Shu-Min Zhao, Shuo Xiao, Ce Cai, Sheng-Lun Xie, Wang-Chen Xue, Chen-Wei Wang, Yue Wang, Wen-Long Zhang
Figure caption: The conditional residual time ﹩\hat{\lambda }(t| {\lambda }_{0})﹩. The λ 0 is either from q + (above the median of the entire data), q − (below the median of the entire data), or q 0 (the unconditional case). Two cases of ﹩\hat{\lambda }(t| {\lambda }_{0})﹩ for the elapsed time t are considered for (a) t = 0 and (b) ﹩t=\bar{\lambda }/2﹩. In the two cases, all FRBs studied exhibit ﹩\hat{\lambda }(t| {\lambda }_{0}^{+})\gt \hat{\lambda }(t| {\lambda }_{0}^{-})﹩ and are symmetrically distributed around ﹩\hat{\lambda }(t)﹩ at t = 0. Additionally, relative to t = 0, the residual time ﹩\hat{\lambda }(t| {\lambda }_{0})﹩ at ﹩t=\tfrac{\bar{\lambda }}{2}﹩ generally increases, regardless of whether λ 0 comes from q +, q −, or q 0. Fluence thresholds are the same as in Figure 4.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Computed Γ = k rp/k cr, the ratio of the radiative force on aggregates to the gravitational force for forsterite with a fractal dimension of 1.8. Values are computed for M = 1.0 ∗ M ⊙, T = 2700 K, and L = 7000L ⊙, and the radiative pressure term is integrated over the stellar blackbody curve. Values are computed based on a 0.3 fractional conversion of the silicon and each point within the contour plot represents the same amount of condensable material.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Variation in radiative pressure opacity with increasing aggregate size for forsterite. The aggregate radiative pressure opacity per gram, κ agg, is scaled via the product of the number of primary particles in the aggregate, N, and the radiative pressure of a single primary particle, κ primary. Data are shown for both fractal dimensions of 1.8 and 2.8 and primary particle radii of (a) 0.01, (b) 0.05, (c) 0.1, and (d) 0.3 μm, and calculated at a wavelength of 1.0 μm.
Paper: Memory in the Burst Occurrence of Repeating Fast Radio Bursts
Authors: Ping Wang, Li-Ming Song, Shao-Lin Xiong, Xiao-Yun Zhao, Jin Wang, Shu-Min Zhao, Shuo Xiao, Ce Cai, Sheng-Lun Xie, Wang-Chen Xue, Chen-Wei Wang, Yue Wang, Wen-Long Zhang
Figure caption: The conditional probability of waiting time R(t∣λ 0), exceeding a specified fluence threshold for four FRB data sets, respectively, and separated by the previous time interval λ 0, are succeeded by the next FRBs within time t. The λ 0 comes from either q 1, q 2, q 3, or q 4 and the thresholds are 0.1, 0.6, and 0.5 Jy ms and 1.0 Jy s for FRB 20121102A, FRB 20220912A, FRB 20201124A(B), and FRB 20201124A(A).
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Computed Γ = k rp/k cr, the ratio of the radiative force on aggregates to the gravitational force for forsterite with a fractal dimension of 1.8. Values are computed for M = M ⊙, T = 2700 K, and L = 7000L ⊙, and the radiative pressure term is integrated over the stellar blackbody curve. The contour lines represent the location of the point where k rp/k cr = 1 and the corresponding fractional conversion of silicon is listed on the contour line.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Computed Γ = k rp/k cr, the ratio of the radiative force on aggregates to the gravitational force for forsterite with a fractal dimension of 2.8. Values are computed for M = M ⊙, T = 2700 K, and L = 7000L ⊙, and the radiative pressure term is integrated over the stellar blackbody curve. The contour lines represent the location of the point where k rp/k cr = 1 and the corresponding fractional conversion of silicon is listed on the contour line.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: Examples of aggregates used to compute opacity properties. The top panel shows aggregates with a fractal dimension of 1.8 for (a) 32, (b) 64, and (c) 128 primary particles. The lower panel shows more compact aggregates with a fractal dimension of 2.8 for (d) 32, (e) 64, and (f) 128 primary particles.
Paper: Radiative Pressure on Fractal Dust Grains in Oxygen-rich AGB Stars
Authors: Frank T. Ferguson, Joseph A. Nuth, John A. Paquette
Figure caption: After generation of the fractal aggregates via the DLA software, the radius of gyration was computed from the geometry files to verify that the computed aggregates followed the scaling law given by Equation (1).
Paper: Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements
Authors: Alice P. Curtin, Joel M. Weisberg, Joanna M. Rankin
Figure caption: Magnetic field strengths measured in this work along the Local Arm (magenta) and the Sagittarius Arm (green) in the approximate longitude and latitude regions studied by A. Ordog et al. (2017). Magnetic field direction along an arm is indicated with a cross (positive, CCW) or a circle (negative, CW), with its magnitude shown via the symbol’s size. For pulsars for which ∣B∣ < 0.5 μG, we set the symbol size to be equivalent to that of ∣B∣ = 0.5 μG. Similarly, for any pulsars for which ∣B∣ > 20 μG, we set the symbol size to be equivalent to that of ∣B∣ = 20 μG. Outliers (listed in Table 3) are not shown.
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: Evolution of IGM neutral fraction (x H I) in the reionization era. The IGM neutral fractions derived from our z > 6.5 NIRSpec sample are shown by red stars. We show the constraints derived from CMB optical depth and Lyα and Lyβ forest dark pixel fraction (C. A. Mason et al. 2019b) as gray shaded regions (dark gray: 68% percentiles; light gray: 95% percentiles). We overplot the IGM neutral fractions derived from multiple observational probes in the literature: CMB optical depth (white hexagon; Planck Collaboration et al. 2020), Lyα and Lyβ forest dark pixel fraction (blue circles; I. D. McGreer et al. 2015; X. Jin et al. 2023), Lyα damping wing absorption of quasars (cyan squares; E. Bañados et al. 2018; F. B. Davies et al. 2018; F. Wang et al. 2020; J. Yang et al. 2020; B. Greig et al. 2022; D. Ďurovčíková et al. 2024), Lyα damping wing absorption of Lyman break galaxies (green triangles; E. Curtis-Lake et al. 2023; T. Y.-Y. Hsiao et al. 2024; H. Umeda et al. 2024), the clustering of LAEs (orange diamond; E. Sobacchi & A. Mesinger 2015; M. Ouchi et al. 2018), Lyα luminosity function (LF; pink pentagon; M. Ouchi et al. 2010; A. Konno et al. 2014, 2018; Z.-Y. Zheng et al. 2017; A. K. Inoue et al. 2018; H. Goto et al. 2021; A. M. Morales et al. 2021; Y. Ning et al. 2022), and Lyα EW (violet stars; C. A. Mason et al. 2018, 2019a; A. Hoag et al. 2019; L. R. Whitler et al. 2020; P. Bolan et al. 2022; S. Bruton et al. 2023; T. Morishita et al. 2023; M. Nakane et al. 2024).
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: Spatial distribution of spectroscopically confirmed galaxies in the two GOODS fields (top: GOODS-South; bottom: GOODS-North) at z = 7.0–8.5 identified from both the JADES and the FRESCO data set. We show galaxies with NIRSpec redshift confirmation as stars, and the [O III] emitters identified from FRESCO observations (R. A. Meyer et al. 2024) as hexagons. Lyα emitting galaxies are marked by red stars, and we highlight strong LAEs with EW > 50 Å as red circles. We find possible overdensities of [O III] emitters (blue shaded regions) around three strong LAEs, JADES-1129 (z = 7.087) and JADES-13041 (z = 7.090) in GOODS-N and JADES-13682 (z = 7.275) in GOODS-S, and at z ≃ 7.7 in GOODS-S and at z ≃ 7.6 in GOODS-N.
Paper: Discovery of MgS and NaS in the Interstellar Medium and Tentative Detection of CaO
Authors: Marta Rey-Montejo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Víctor M. Rivilla, Andrés Megías, David San Andrés, Miguel Sanz-Novo, Laura Colzi, Shaoshan Zeng, Álvaro López-Gallifa, Antonio Martínez-Henares, Sergio Martín, Belén Tercero, Pablo de Vicente, Miguel Requena-Torres
Figure caption: Unblended transitions of NaS detected toward G+0.693, displayed in order of decreasing line intensity. The observed spectrum is represented in gray. The best LTE fit derived with MADCUBA is shown with a red line, while the blue line shows the expected molecular emission from all of the molecular species identified to date in our survey. The quantum numbers of each transition are shown in the upper part of each panel, and indicate the J + 1 → J transition and the parity (e or f). All the transitions shown here correspond to the sub-state ﹩{{\rm{\Pi }}}_{3/2}^{2}﹩ (see the text).
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: Number of expected galaxies in a volume with an effective radius of 4.′4 (or R = 1.3 pMpc, equivalent to the area of one of the FRESCO fields) and Δz = 0.2. The black dashed line shows the total number of UV-selected z ≃ 8 galaxies visible to a given M UV limit, assuming an average density field according to the R. J. Bouwens et al. (2021) UV LFs. The red line shows the corresponding number of [O III] emitters in the same area that would be recovered in ≃2 hr grism observations down to the 5σ line flux limit (>2 × 10−18 erg s−1 cm−2). Dotted lines highlight the absolute magnitude where we expect to identify one and 30 total galaxies in the volume. Existing grism observations become incomplete among the faint (M UV > −19) galaxy population. Fully characterizing overdensities will ultimately require deeper spectroscopy.
Paper: Discovery of MgS and NaS in the Interstellar Medium and Tentative Detection of CaO
Authors: Marta Rey-Montejo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Víctor M. Rivilla, Andrés Megías, David San Andrés, Miguel Sanz-Novo, Laura Colzi, Shaoshan Zeng, Álvaro López-Gallifa, Antonio Martínez-Henares, Sergio Martín, Belén Tercero, Pablo de Vicente, Miguel Requena-Torres
Figure caption: Transitions of MgS detected toward G+0.693, displayed in order of decreasing line intensity. Four of the observed transitions are unblended, while the other three appear blended with emission from other molecular lines. The spectra are represented as gray histograms. The best LTE fit derived with MADCUBA is shown with a red line, while the blue line shows the predicted molecular emission from all of the molecular species identified to date in our survey. The quantum numbers of each transition are shown in the upper part of each panel.
Paper: JWST/NIRSpec Observations of Lyman α Emission in Star-forming Galaxies at 6.5 ≲ z ≲ 13
Authors: Mengtao Tang, Daniel P. Stark, Michael W. Topping, Charlotte Mason, Richard S. Ellis
Figure caption: Spatial distribution of the spectroscopically confirmed galaxies (stars) at z ≃ 7–8 identified from public NIRSpec data sets in the EGS (top left), A2744 (top right), GOODS-South (bottom left), and GOODS-North (bottom right) fields. We mark LAEs as red filled stars. We also show AGNs as diamonds. In the EGS field, we overplot high S/N (>7) Lyα detections from ground-based observations (P. A. Oesch et al. 2015; V. Tilvi et al. 2020; I. Jung et al. 2022) as red pentagons.
Paper: Discovery of MgS and NaS in the Interstellar Medium and Tentative Detection of CaO
Authors: Marta Rey-Montejo, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Víctor M. Rivilla, Andrés Megías, David San Andrés, Miguel Sanz-Novo, Laura Colzi, Shaoshan Zeng, Álvaro López-Gallifa, Antonio Martínez-Henares, Sergio Martín, Belén Tercero, Pablo de Vicente, Miguel Requena-Torres
Figure caption: Rotational diagram of NaS (red dots) using the transitions reported in Table 2. The black dashed line corresponds to the best linear fit to the data points. The derived values for the molecular column density, N, and the excitation temperature, T ex, are shown in blue. Ten points are represented in the figure, corresponding to the different parity of each line due to lambda doubling.
Paper: Parkes Radio and NuSTAR X-Ray Observations of the Composite Supernova Remnant B0453–685 in the Large Magellanic Cloud
Authors: Jordan Eagle, Jeremy Hare, Elizabeth Hays, Daniel Castro, Joseph Gelfand, Jwaher Alnaqbi, Matthew Kerr, Shi Dai, Jean Ballet, Fabio Acero, Patrick Slane, Marco Ajello
Figure caption: NuSTAR FPMA detector image of B0453–685 in the 3–78 keV energy range. The image is smoothed with a Gaussian kernel. The source (blue) and background (cyan) regions used for spectral extraction are indicated. The source emission appears pointlike, with a nearby, unrelated source “Src2” (green; see the main text for details). The coordinate grid shows the International Celestial Reference System R.A. and decl. in degrees.
Paper: Parkes Radio and NuSTAR X-Ray Observations of the Composite Supernova Remnant B0453–685 in the Large Magellanic Cloud
Authors: Jordan Eagle, Jeremy Hare, Elizabeth Hays, Daniel Castro, Joseph Gelfand, Jwaher Alnaqbi, Matthew Kerr, Shi Dai, Jean Ballet, Fabio Acero, Patrick Slane, Marco Ajello
Figure caption: Left: the joint fit for Chandra data from 0.5 to 7 keV and the NuSTAR data from 3 to 20 keV for B0453–685. The PWN 0.5–20 keV X-ray spectrum can be fit assuming a simple power law with a photon index ΓX = 2.01 ± 0.13 plus a low-energy thermal component arising in the SNR. The Chandra and NuSTAR data points are background subtracted. The background data are shown in gray for NuSTAR FPMA. The solid and dashed lines represent the source spectral models and components. Right: the residuals of the joint best fit. In both panels, the data are grouped to 20 counts per bin for clarity.
Paper: Parkes Radio and NuSTAR X-Ray Observations of the Composite Supernova Remnant B0453–685 in the Large Magellanic Cloud
Authors: Jordan Eagle, Jeremy Hare, Elizabeth Hays, Daniel Castro, Joseph Gelfand, Jwaher Alnaqbi, Matthew Kerr, Shi Dai, Jean Ballet, Fabio Acero, Patrick Slane, Marco Ajello
Figure caption: A comparison of the power-law spectral index values measured from X-ray spectral models assuming varying data sets as labeled.
Paper: Synchrotron Polarization of a Hybrid Distribution of Relativistic Thermal and Nonthermal Electrons in Gamma-Ray Burst Prompt Emission
Authors: Cheng Kangfa, Jirong Mao, Zhao Xiaohong, Liu Hongbang, Merlin Kole, Nicolas Produit, Chen Zhifu
Figure caption: Instantaneous PDs with different temperatures (T  e ) in the gamma-ray (30–800 keV), X-ray (2–30 keV), and optical bands (4.3 × 1014–7.5 × 1014 Hz). The upper panels display the normalized light curves (scaled to the maximum flux), while the bottom panels show the corresponding instantaneous PDs. The numbers in parentheses represent the energy fraction of nonthermal electrons. “syn-decB” represents the synchrotron radiation produced by the pure nonthermal electrons with the decaying MF model.
Paper: Synchrotron Polarization of a Hybrid Distribution of Relativistic Thermal and Nonthermal Electrons in Gamma-Ray Burst Prompt Emission
Authors: Cheng Kangfa, Jirong Mao, Zhao Xiaohong, Liu Hongbang, Merlin Kole, Nicolas Produit, Chen Zhifu
Figure caption: Time-averaged PDs with different γ th in various T  e  in the gamma-ray, X-ray, and optical bands. For comparison, the observed polarization data of the gamma-ray band are presented in the left panel. f is the energy fraction of the nonthermal electrons. The black, red, and green numbers correspond to the temperatures of 1 × 1011 k, 1 × 1012 k, and 1 × 1013 k, respectively. The solid lines represent q = 0.8 and the dashed lines represent q = 1.1. The dotted green line in the left panel represents p = 2.0 and T  e  = 1 × 1013 k for q = 1.1. Note that all curves except the dotted green line are calculated by taking p = 2.8.
Paper: Synchrotron Polarization of a Hybrid Distribution of Relativistic Thermal and Nonthermal Electrons in Gamma-Ray Burst Prompt Emission
Authors: Cheng Kangfa, Jirong Mao, Zhao Xiaohong, Liu Hongbang, Merlin Kole, Nicolas Produit, Chen Zhifu
Figure caption: Polarization spectra (bottom panels), flux spectra (middle-row panels), and electron distributions (top panels) for different temperatures T  e  (left panels), conjunctive LFs γ th (middle-column panels), and normalized viewing angles q (right panels). The numbers in parentheses represent the energy fraction of nonthermal electrons.
Paper: Synchrotron Polarization of a Hybrid Distribution of Relativistic Thermal and Nonthermal Electrons in Gamma-Ray Burst Prompt Emission
Authors: Cheng Kangfa, Jirong Mao, Zhao Xiaohong, Liu Hongbang, Merlin Kole, Nicolas Produit, Chen Zhifu
Figure caption: Similar to Figure 3, but with different conjunctive LFs (γ th).
Paper: Synchrotron Polarization of a Hybrid Distribution of Relativistic Thermal and Nonthermal Electrons in Gamma-Ray Burst Prompt Emission
Authors: Cheng Kangfa, Jirong Mao, Zhao Xiaohong, Liu Hongbang, Merlin Kole, Nicolas Produit, Chen Zhifu
Figure caption: Time-averaged PDs with different normalized viewing angles (q) for various T  e  in the gamma-ray, X-ray, and optical bands. The numbers in parentheses represent the energy fraction of nonthermal electrons. “syn-decB” represents the synchrotron radiation produced by the pure nonthermal electrons with the decaying MF model. These time-averaged results correspond to the instantaneous results in Figure 3.
Paper: Synchrotron Polarization of a Hybrid Distribution of Relativistic Thermal and Nonthermal Electrons in Gamma-Ray Burst Prompt Emission
Authors: Cheng Kangfa, Jirong Mao, Zhao Xiaohong, Liu Hongbang, Merlin Kole, Nicolas Produit, Chen Zhifu
Figure caption: Left panel: the energy fraction of nonthermal electrons with different conjunctive LFs (γ th). Right panel: the energy fraction of nonthermal electrons with different temperatures of thermal electrons (T  e ).
Paper: Synchrotron Polarization of a Hybrid Distribution of Relativistic Thermal and Nonthermal Electrons in Gamma-Ray Burst Prompt Emission
Authors: Cheng Kangfa, Jirong Mao, Zhao Xiaohong, Liu Hongbang, Merlin Kole, Nicolas Produit, Chen Zhifu
Figure caption: Similar to Figure 5, but with various γ th. These time-averaged results correspond to the instantaneous results in Figure 4.
Paper: Local Interstellar Spectra and Solar Modulation of Cosmic-Ray Proton and Helium
Authors: Cheng-Rui Zhu
Figure caption: (a) The model best-fit time profiles of the p/He ratio evaluated at rigidities R = 2.0, 2.5, 3.1, 5.6, 9.6 and 21.9 GV (from top to bottom) compare with the data. (b) Extending to rigidities R = 0.5 (red) and 1.0 GV (blue).
Paper: Local Interstellar Spectra and Solar Modulation of Cosmic-Ray Proton and Helium
Authors: Cheng-Rui Zhu
Figure caption: The rigidity break for different period. The red line stands for the mean value, which is about 6 GV.
Paper: Local Interstellar Spectra and Solar Modulation of Cosmic-Ray Proton and Helium
Authors: Cheng-Rui Zhu
Figure caption: The χ 2/d.o.f from our calculations. The cyan line represents the results obtained using the modified FFA, while the blue line corresponds to the outcomes of the FFA. The yellow band stands for the heliospheric magnetic field reversal period within which the polarity is uncertain.
Paper: Local Interstellar Spectra and Solar Modulation of Cosmic-Ray Proton and Helium
Authors: Cheng-Rui Zhu
Figure caption: The ratio of model prediction to data (model/data) for p fluxes of AMS-02 from 2011 May to 2017 May using modified FFA.
Paper: Local Interstellar Spectra and Solar Modulation of Cosmic-Ray Proton and Helium
Authors: Cheng-Rui Zhu
Figure caption: Same as Figure 5 but for p/He.
Paper: Local Interstellar Spectra and Solar Modulation of Cosmic-Ray Proton and Helium
Authors: Cheng-Rui Zhu
Figure caption: Same as Figure 5 but for He.
Paper: Electron Acceleration in Magnetic Islands in Quasi-parallel Shocks
Authors: N. Bessho, L.-J. Chen, M. Hesse, J. Ng, L. B. Wilson, J. E. Stawarz, H. Madanian
Figure caption: (a)–(d) Electron trajectory (red) trapped in island 2, and electric field E  y  (color) at Ω i  t = 18.75, 19.38, 20.00, and 20.63. The start and end points are marked by white and yellow dots, respectively. (e)–(f) Lorentz factor γ and work done by the x, y, and z components of the electric field (W  x , W  y , and W  z , respectively), as functions of time for the electron. Magenta: work done by the in-plane electric field. Black: total work. In (e), arrows correspond to each interval of up–down motion in island 2.