adsabs/AstroCLIMB huggingface dataset:
Paper: Neutron-quark Stars: Discerning Viable Alternatives for the Higher-density Part of the Equation of State of Compact Stars
Authors: Sudipta Hensh, Yong-Jia Huang, Toru Kojo, Luca Baiotti, Kentaro Takami, Shigehiro Nagataki, Hajime Sotani
Figure caption: Left panel: power spectral densities for the QHC21Ch-stiff model. Here, ﹩\tilde{h}(f)\equiv \sqrt{\frac{{\left|{\tilde{h}}_{+}(f)\right|}^{2}+{\left|{\tilde{h}}_{\times }(f)\right|}^{2}}{2}}﹩, where ﹩{\tilde{h}}_{+}﹩ and ﹩{\tilde{h}}_{\times }﹩ are the Fourier transforms of the two polarization modes (h+ and h×), computed as we did in Y.-J. Huang et al. (2022). Vertical lines indicate the contact frequency. The labels in the legend consist, for each QHC21Ch-stiff model, in the rest mass of a star in the binary, followed by the Γth coefficient if different from 2, followed by the finest grid spacing if different from the standard 231 m, followed by the difference between the time between merger (fcont) and collapse. Right panel: energy radiated in the l = m = 2 GW mode as a function of time; tmer is the time of merger.
Paper: Neutron-quark Stars: Discerning Viable Alternatives for the Higher-density Part of the Equation of State of Compact Stars
Authors: Sudipta Hensh, Yong-Jia Huang, Toru Kojo, Luca Baiotti, Kentaro Takami, Shigehiro Nagataki, Hajime Sotani
Figure caption: Isodensity contours on the (x, y) (equatorial) plane for the QHC21Ch models with different masses, as shown in each panel, at time t = 10 ms after the merger. The black contour lines show the number density when the crossover starts. The cyan contour lines show the number density above which only deconfined quark matter is present.
Paper: Neutron-quark Stars: Discerning Viable Alternatives for the Higher-density Part of the Equation of State of Compact Stars
Authors: Sudipta Hensh, Yong-Jia Huang, Toru Kojo, Luca Baiotti, Kentaro Takami, Shigehiro Nagataki, Hajime Sotani
Figure caption: Evolution of the maximum of the number density (nmax) in units of nuclear saturation density for the QHC21Ch-stiff EOS model with mass 3.1 M⊙ and different combinations of Γth and grid spacing of the finest refinement level, Δx.
Paper: Neutron-quark Stars: Discerning Viable Alternatives for the Higher-density Part of the Equation of State of Compact Stars
Authors: Sudipta Hensh, Yong-Jia Huang, Toru Kojo, Luca Baiotti, Kentaro Takami, Shigehiro Nagataki, Hajime Sotani
Figure caption: Radiated angular momentum and energy as a function of time. t = tmer is the time of merger.
Paper: Neutron-quark Stars: Discerning Viable Alternatives for the Higher-density Part of the Equation of State of Compact Stars
Authors: Sudipta Hensh, Yong-Jia Huang, Toru Kojo, Luca Baiotti, Kentaro Takami, Shigehiro Nagataki, Hajime Sotani
Figure caption: Radiated energy as a function of radiated angular momentum. The two panels on the left show the relation between quantities normalized to their values at the time of merger. The two panels on the right show nonnormalized quantities calculated excluding the inspiral contribution.
Paper: The Gravitational-wave Background from Massive Black Holes in the ASTRID Simulation
Authors: Nianyi Chen, Tiziana Di Matteo, Yihao Zhou, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: Left: the merger rates of major mergers (q > 0.25) from simulations in the mass bins most relevant for PTA-band sources. The solid curves show the merger rates from ASTRID. The shaded bands enclose merger rates from TNG300 with a range of dynamical friction delays (see Appendix A). We also include the best-fit binary population from NG15-binary (crosses) at z = 0.5 for comparison. Simulations show consistent merger rates except for the 108.5 M⊙ < Mror < 109.5 M⊙ mass bin (highlighted by a red arrow). Middle and right: single and binary MBH mass function from ASTRID (green) and TNG300 (purple; the upper curve corresponds to short DF, and the lower curve corresponds to longer DF). We also plot the constraints on single MBH masses from local scaling relations shown in G. Sato-Polito et al. (2023; yellow) and the constraints from NG15-binary (gray shaded).
Paper: Weakened Magnetic Braking Signals the Collapse of the Global Stellar Dynamo
Authors: Travis S. Metcalfe, Jennifer L. van Saders, Marc H. Pinsonneault, Thomas R. Ayres, Oleg Kochukhov, Keivan G. Stassun, Adam J. Finley, Victor See, Ilya V. Ilyin, Klaus G. Strassmeier
Figure caption: Ratio of the observationally estimated and model wind braking torque as a function of Rossby number normalized to the solar value. The dotted line illustrates the fit described in Section 4, and the 95% confidence interval is shown as a gray shaded region. Flat-activity stars and other targets discussed in the text are labeled.
Paper: Weakened Magnetic Braking Signals the Collapse of the Global Stellar Dynamo
Authors: Travis S. Metcalfe, Jennifer L. van Saders, Marc H. Pinsonneault, Thomas R. Ayres, Oleg Kochukhov, Keivan G. Stassun, Adam J. Finley, Victor See, Ilya V. Ilyin, Klaus G. Strassmeier
Figure caption: Ratio of observations and model predictions as a function of Rossby number normalized to the solar value. Each ratio has been raised to a power that reflects its relative contribution to the change in wind braking torque and normalized so that unity represents agreement. (a) Dipole magnetic field strength as a proxy for the large-scale field, and (b) X-ray luminosity, reflecting changes in the stellar mass-loss rate. The solar dipole field strength is from A. J. Finley et al. (2018), while the X-ray luminosity over a complete solar cycle is from P. G. Judge et al. (2003).
Paper: The Gravitational-wave Background from Massive Black Holes in the ASTRID Simulation
Authors: Nianyi Chen, Tiziana Di Matteo, Yihao Zhou, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang, Rupert Croft
Figure caption: Top: the stochastic GWBs generated from the MBH merger population in cosmological simulations ASTRID (green) and TNG300 (purple). We draw 100 realizations of the binary population to estimate the GWB for each simulation. We show the median value among all realizations (solid) and the 68% intervals (shaded). We plot the power-law fit to the joint PTA analysis (black dashed) and the NANOGrav 15 yr GWB (gray violins) for comparison. Bottom: the ratio between the simulation-predicted GWB and the IPTA joint constraints.
Paper: Weakened Magnetic Braking Signals the Collapse of the Global Stellar Dynamo
Authors: Travis S. Metcalfe, Jennifer L. van Saders, Marc H. Pinsonneault, Thomas R. Ayres, Oleg Kochukhov, Keivan G. Stassun, Adam J. Finley, Victor See, Ilya V. Ilyin, Klaus G. Strassmeier
Figure caption: Relative wind braking torque as a function of Rossby number normalized to the solar value. Points are grouped by spectral type as shown in the legend. Standard spin-down models for the mean stellar properties within each spectral type are shown for reference. The solar point ⊙ is from A. J. Finley et al. (2018).
Paper: The Atomic Gas Properties of Green Pea Galaxies: Connections to Lyman Continuum Leakage
Authors: Archishman Khasnovis, Nissim Kanekar, Sangeeta Malhotra, James Rhoads
Figure caption: The H I mass, or the 3σ upper limits to the H I mass, plotted against the O32 ratio for the 60 GPs of the sample. The dashed vertical line indicates the value O32 = 10, above which galaxies are expected to show significant LyC leakage. The filled and open symbols indicate, respectively, detections and nondetections of H I 21 cm emission, with the green circles indicating GPs from the present work, the blue diamonds from N. Kanekar et al. (2021, K21), the orange squares from Y. Chandola et al. (2024, C24), and the purple triangle from S. Dutta et al. (2024, D24). The red circles with errors indicate the Kaplan–Meier (K-M) means of the H I mass of the O32 < 10 and O32 > 10 subsamples. The median error bar (i.e., 2× median error) for the H I masses is indicated at the top left.
Paper: The Atomic Gas Properties of Green Pea Galaxies: Connections to Lyman Continuum Leakage
Authors: Archishman Khasnovis, Nissim Kanekar, Sangeeta Malhotra, James Rhoads
Figure caption: GBT H I 21 cm spectra for the 17 nondetections of the sample, ordered by R.A. In each panel, the x-axis shows velocity, in km s−1, relative to the GP redshift, while the y-axis is flux density, in mJy. The horizontal dashed black lines in each panel indicate the ±1σ error on the spectrum, at a velocity resolution of 10 km s−1. For J0130+1746 and J0822+1042, the vertical gray bands indicate regions of the spectra that were affected by RFI and that have not been used in the rms noise estimates.
Paper: The Atomic Gas Properties of Green Pea Galaxies: Connections to Lyman Continuum Leakage
Authors: Archishman Khasnovis, Nissim Kanekar, Sangeeta Malhotra, James Rhoads
Figure caption: The H I-to-stellar mass ratio fHI, or the 3σ upper limits to fHI, plotted against the O32 ratio for the 60 GPs of the sample. The symbols are the same as those in Figure 4. The median error bar (i.e., 2× median error) for the HI-to-stellar mass ratios is indicated at the top left.
Paper: The Atomic Gas Properties of Green Pea Galaxies: Connections to Lyman Continuum Leakage
Authors: Archishman Khasnovis, Nissim Kanekar, Sangeeta Malhotra, James Rhoads
Figure caption: The H I depletion timescale (τdep = MHI/SFR), in yr, plotted against the O32 ratio for the 60 GPs of the sample. The symbols are the same as those in Figure 4. The median error bar (i.e., 2× median error) for the H I depletion timescales is indicated at the top left.
Paper: The Atomic Gas Properties of Green Pea Galaxies: Connections to Lyman Continuum Leakage
Authors: Archishman Khasnovis, Nissim Kanekar, Sangeeta Malhotra, James Rhoads
Figure caption: GBT H I 21 cm spectra for the seven GPs of the sample with detections of H I 21 cm emission, ordered by R.A. In each panel, the x-axis shows velocity, in km s−1, relative to the GP redshift, while the y-axis is flux density, in mJy. The horizontal dashed black lines in each panel indicate the ±1σ error on the spectrum, at a velocity resolution of 10 km s−1.
Paper: The Atomic Gas Properties of Green Pea Galaxies: Connections to Lyman Continuum Leakage
Authors: Archishman Khasnovis, Nissim Kanekar, Sangeeta Malhotra, James Rhoads
Figure caption: Histograms showing the distributions of ((A)) the stellar masses and ((B)) the SFRs of the final sample of 60 GPs. In both panels, the red histogram is for GPs with O32 < 10, and the green one is for those with O32 > 10, with the dashed olive region indicating the region of overlap.
Paper: Coexistence of Longitudinal and Transverse Oscillations in Polar Plumes Observed with Solar Orbiter/Extreme Ultraviolet Imager
Authors: Upasna Baweja, Vaibhav Pant, S. Krishna Prasad, Arpit Kumar Shrivastav, Tom Van Doorsselaere, Nancy Narang, Cis Verbeeck, M. Saleem Khan, David Berghmans
Figure caption: Propagating disturbances: panels (A)–(E) show the extracted TD maps for the selected plumes. The slit numbers are mentioned at the top of each TD map. Cyan lines are fitted on the ridges, depicting the speeds of the propagating disturbances in the slits. Panels (F) and (G) represent the TD maps and the fitted ridges of the two fine-scale substructures (“SS 1” and “SS 2”) corresponding to Slit 1. Panels (H) and (I) represent the same for the fine-scale substructures of Slit 5.
Paper: Coexistence of Longitudinal and Transverse Oscillations in Polar Plumes Observed with Solar Orbiter/Extreme Ultraviolet Imager
Authors: Upasna Baweja, Vaibhav Pant, S. Krishna Prasad, Arpit Kumar Shrivastav, Tom Van Doorsselaere, Nancy Narang, Cis Verbeeck, M. Saleem Khan, David Berghmans
Figure caption: Damping lengths and periodicity: panels (A)–(E) show the relative amplitudes of the selected plumes as a function of the distance along the slits. The slit numbers are mentioned at the top of each profile. The gray error bars represent the associated uncertainties. The green stars and magenta plus signs represent the Gaussian and exponential fits to the decaying spatial profiles. Panels (F)–(J) represent the average Fourier power spectra at different heights of the different plumes. The red stars represent the dominant frequencies for these plumes.
Paper: Coexistence of Longitudinal and Transverse Oscillations in Polar Plumes Observed with Solar Orbiter/Extreme Ultraviolet Imager
Authors: Upasna Baweja, Vaibhav Pant, S. Krishna Prasad, Arpit Kumar Shrivastav, Tom Van Doorsselaere, Nancy Narang, Cis Verbeeck, M. Saleem Khan, David Berghmans
Figure caption: Panels (A)–(C) present box and whisker plots of the wave parameters obtained from all the selected plumes at different heights. Each box’s upper and lower bounds correspond to the third and first data quartiles. The horizontal lines indicate the median values. Panels (D)–(F) present histograms of the displacement amplitudes, periods, and velocity amplitudes for all the heights from 3 to 20 Mm above the solar limb for all the selected plumes. The purple curves represent the log-normal distributions obtained from the data using arithmetic moments. The light coral, forest green, and dark red colored straight lines represent the mode, median, and mean values of the parameters obtained from the log-normal distributions.
Paper: Coexistence of Longitudinal and Transverse Oscillations in Polar Plumes Observed with Solar Orbiter/Extreme Ultraviolet Imager
Authors: Upasna Baweja, Vaibhav Pant, S. Krishna Prasad, Arpit Kumar Shrivastav, Tom Van Doorsselaere, Nancy Narang, Cis Verbeeck, M. Saleem Khan, David Berghmans
Figure caption: (A) The TD map for the transverse slit at h = 8.4 Mm in Slit 4. The dotted magenta curves correspond to the detected transverse waves fitted, as mentioned in Section 3.2. (B)–(E) Zoomed-in view of the visually detected transverse waves. The error bars represent the uncertainty on the mean of the fitted Gaussian at each time. The magenta curves show the corresponding fitted oscillations. The amplitude (A) and period (p) are mentioned for each fitted curve.
Paper: Coexistence of Longitudinal and Transverse Oscillations in Polar Plumes Observed with Solar Orbiter/Extreme Ultraviolet Imager
Authors: Upasna Baweja, Vaibhav Pant, S. Krishna Prasad, Arpit Kumar Shrivastav, Tom Van Doorsselaere, Nancy Narang, Cis Verbeeck, M. Saleem Khan, David Berghmans
Figure caption: Relative variation in electron density with height obtained from observations in coronal plumes. Data has been normalized by their value at ≈12 Mm. The red dashed line corresponds to the polynomial fit.
Paper: Explaining the Weak Evolution of the High-redshift Mass–Metallicity Relation with Galaxy Burst Cycles
Authors: Andrew Marszewski, Claude-André Faucher-Giguère, Robert Feldmann, Guochao Sun
Figure caption: Average inflow metallicity ﹩{Z}_{{\rm{in}}}^{{\rm{avg}}}﹩ (left), metal production efficiency εZ (middle), and their sum (right) as a function of stellar mass at z ∼ 5.5 (blue), 6.5 (orange), 8.0 (green), and 10.5 (red). Open squares represent stellar-mass-binned median values. Smaller, transparent points represent the measured quantities of individual galaxies at each time step within a burst cycle. At fixed stellar mass, the average inflow metallicity decreases with increasing redshift, while the metal production efficiency increases. The evolutions of these two quantities largely cancel one another out in their sum, resulting in the prediction of weak evolution in the MZR.
Paper: Explaining the Weak Evolution of the High-redshift Mass–Metallicity Relation with Galaxy Burst Cycles
Authors: Andrew Marszewski, Claude-André Faucher-Giguère, Robert Feldmann, Guochao Sun
Figure caption: The scaling relations of ﹩{\dot{M}}_{{\rm{Z}},{\rm{in}}}﹩ (left), ﹩{\dot{M}}_{{\rm{Z}},{\rm{R}}}﹩ (middle), and ﹩{\dot{M}}_{{\rm{in}}}﹩ (right) with stellar mass at z ∼ 5.5 (blue), 6.5 (orange), 8.0 (green), and 10.5 (red). Smaller, transparent points represent the measurements of individual galaxies at each snapshot within the burst cycles. Open squares represent stellar-mass-binned median values. Solid black lines are meant to guide the eye toward the approximate slope of each scaling relation. The slope values for these guidelines (﹩\int {\dot{M}}_{{\rm{Z}},{\rm{in}}}dt﹩, ﹩\int {\dot{M}}_{{\rm{Z}},{\rm{R}}}dt\propto {M}_{\star }^{1.12}﹩, and ﹩\int {\dot{M}}_{{\rm{in}}}dt\propto {M}_{\star }^{0.75}﹩) are chosen to demonstrate the ability of these scaling relations within our reduced burst model to reproduce the FIRE-2 MZR slope at high redshift measured by A. Marszewski et al. (2024): ﹩{Z}_{{\rm{gas}}}\propto {M}_{\star }^{1.12}/{M}_{\star }^{0.75}={M}_{\star }^{0.37}﹩.
Paper: Explaining the Weak Evolution of the High-redshift Mass–Metallicity Relation with Galaxy Burst Cycles
Authors: Andrew Marszewski, Claude-André Faucher-Giguère, Robert Feldmann, Guochao Sun
Figure caption: Signal for an FMR-like relation with SFRHα (top) and SFRUV (bottom) as the secondary parameters for our complete sample of galaxies (left) and for an “observable” (L1560 > 2 × 1043 erg s−1, representative of a JADES-Deep-like survey) sample of galaxies (right). Within each stellar mass bin, we plot the median metallicity of galaxies in the highest (blue), second-highest (green), third-highest (yellow), fourth-highest (orange), and lowest (red) SFR quintiles. For our mass-complete sample, the lowest SFRHα quintiles have elevated median metallicities, consistent with the existence of an FMR-like relation. This signal weakens significantly when only considering the “observable” galaxies in the sample. There is little evidence for an FMR-like relation when using SFRUV as the secondary predictor for both the mass-complete and “observable” sample.
Paper: Explaining the Weak Evolution of the High-redshift Mass–Metallicity Relation with Galaxy Burst Cycles
Authors: Andrew Marszewski, Claude-André Faucher-Giguère, Robert Feldmann, Guochao Sun
Figure caption: The stellar-mass-binned median burst cycle (squares with solid lines) and evacuation (circles with dashed lines) timescales for galaxies in our sample at z ∼ 5.5 (blue), 6.5 (orange), 8.0 (green), and 10.5 (red). Both timescales are weakly dependent on stellar mass but show mild redshift evolution, typically increasing with cosmic time. The timescale for ISM evacuation (tEvac ∼ 10–30 Myr) is much shorter than the timescale of complete burst cycles (tBurst ∼ 70–200 Myr).
Paper: Explaining the Weak Evolution of the High-redshift Mass–Metallicity Relation with Galaxy Burst Cycles
Authors: Andrew Marszewski, Claude-André Faucher-Giguère, Robert Feldmann, Guochao Sun
Figure caption: SFE (defined here as SFE = ∫SFR dt/﹩\int {\dot{M}}_{\mathrm{in}}﹩ dt) as a function of stellar mass at z  ∼ 5.5 (blue), 6.5 (orange), 8.0 (green), and 10.5 (red). Smaller, transparent points represent the measured quantities integrated over individual galaxy burst cycles. Open squares represent stellar-mass-binned median values. At fixed stellar mass, the SFE increases with increasing redshift. This increase results in the increase of εZ with increasing redshift.
Paper: Neutron-quark Stars: Discerning Viable Alternatives for the Higher-density Part of the Equation of State of Compact Stars
Authors: Sudipta Hensh, Yong-Jia Huang, Toru Kojo, Luca Baiotti, Kentaro Takami, Shigehiro Nagataki, Hajime Sotani
Figure caption: Upper panel: the M-R relation for the NS and NQS models in this work, as well as the 68% confidence interval from some observations. Open circles represent the theoretical NSs whose central density is 2n0. Lower panel: the square of the sound speed as a function of baryon number density nB for the various EOSs. The dashed line represents the conformal limit ﹩{({c}_{s}/c)}^{2}=1/3﹩ (P. Bedaque & A. W. Steiner 2015).
Paper: Pinching of ICME Flux Rope: Unprecedented Multipoint Observations of Internal Magnetic Reconnection during Gannon’s Superstorm
Authors: Shibotosh Biswas, Ankush Bhaskar, Anil Raghav, Ajay Kumar, Kalpesh Ghag, Smitha V. Thampi, Vipin K Yadav
Figure caption: Panel (I) displays the observations recorded by the ACE spacecraft from May 10, 12:00 to 23:59:59 UT. Subpanels (a) to (i) represent IMF intensity, IMF components, IMF azimuth, elevation, solar wind bulk velocity, proton density, temperature, plasma beta (proton), and Sym-H. The yellow-shaded region marks the region of interest. Panel (II) shows MMS1 and OMNI data of the highlighted region of panel (I) with additional information about dynamic pressure, ASY-H, AL, and AU indices related to geomagnetic storms.
Paper: Pinching of ICME Flux Rope: Unprecedented Multipoint Observations of Internal Magnetic Reconnection during Gannon’s Superstorm
Authors: Shibotosh Biswas, Ankush Bhaskar, Anil Raghav, Ajay Kumar, Kalpesh Ghag, Smitha V. Thampi, Vipin K Yadav
Figure caption: The time-shifted magnetic field observation from STEREO-A to match the MC initiation at 21:39:22 UT with ACE in panel (a) in RTN coordinates, followed by Aditya-L1 and THEMIS-C/ARTEMIS-P2 observation of the reconnection, respectively. The areas marked in antique white and magenta are two successive Ejectas/MCs, E1 and E2. Panels (c) and (d) describe the azimuth vs. elevation angle and 2D magnetic field hodogram result from MVA analysis of STEREO-A and ACE magnetic field data corresponding to E1 MC.
Paper: Pinching of ICME Flux Rope: Unprecedented Multipoint Observations of Internal Magnetic Reconnection during Gannon’s Superstorm
Authors: Shibotosh Biswas, Ankush Bhaskar, Anil Raghav, Ajay Kumar, Kalpesh Ghag, Smitha V. Thampi, Vipin K Yadav
Figure caption: Artistic illustration of the ICME–ICME interaction and embedded magnetic reconnection site. Panel (a) describes the interaction of two ICME MCs on 2024 May 10. Two prominent MCs (E1 and E2) are marked with green and yellow, respectively, in the GSE coordinate system, with all the tentative positions of the spacecraft (Appendix D). The internal magnetic reconnection current sheet is marked with a black dashed line inside E1 MC spanning 203 RE along the dawn–dusk direction. Panel (b) represents the cross-sectional view of the reconnection site, indicating the structural deformation of E1 due to intense compression from the trailing MC E2. Panel (c) displays the 3D reconnection geometry in the GSE and local boundary-normal coordinate system (LMN, Appendix A.1). All spacecraft around the L1 point probed the same reconnection outflow jet. The ecliptic plane is visualized in green, while the sky-blue plane represents the plane containing the reconnection X-LINE, which is along the M direction, inclined to -ZGSE at an angle of 12°. This sketch is for illustration purposes only and not to scale.
Paper: Pinching of ICME Flux Rope: Unprecedented Multipoint Observations of Internal Magnetic Reconnection during Gannon’s Superstorm
Authors: Shibotosh Biswas, Ankush Bhaskar, Anil Raghav, Ajay Kumar, Kalpesh Ghag, Smitha V. Thampi, Vipin K Yadav
Figure caption: This figure shows, from the top, time-series data of IMF magnitude (B-field) and components, solar wind ion energy spectrogram (Eion), electron energy spectrogram (Ee, normalized by 21:00 UT flux, outside the MC), and solar wind suprathermal electron pitch-angle distribution (634 and 432 eV), respectively, from 21:50 UT to 22:30 UT on May 10 from Wind spacecraft data. The other suprathermal electron channels (>60 eV) show similar behavior. The white bands represent data gaps. Two black vertical lines mark the region of interest.
Paper: Pinching of ICME Flux Rope: Unprecedented Multipoint Observations of Internal Magnetic Reconnection during Gannon’s Superstorm
Authors: Shibotosh Biswas, Ankush Bhaskar, Anil Raghav, Ajay Kumar, Kalpesh Ghag, Smitha V. Thampi, Vipin K Yadav
Figure caption: Wind spacecraft observation of the complex magnetic cloud structure. Panels display the magnetic field, ion, and electron omnidirectional energy flux, as well as the suprathermal electron pitch-angle distribution, in two separate channels. The yellow and pink shaded regions represent two different flux ropes.