adsabs/AstroCLIMB huggingface dataset:
Paper: Eccentric Dust-ring Formation in Kozai–Lidov Gas Disks
Authors: Rebecca G. Martin, and Stephen H. Lubow
Figure caption: The surface density (in units of M⊙ au−2), eccentricity, argument of periapsis, inclination, and nodal phase angle from top to bottom in each panel at times t = 7.6 (top left), 9.5 (top right), 12.3 (bottom left), and 21.4 Porb (bottom right) for the gas (red lines) and dust (blue lines).
Paper: Eccentric Dust-ring Formation in Kozai–Lidov Gas Disks
Authors: Rebecca G. Martin, and Stephen H. Lubow
Figure caption: Surface-density profile for the gas (red lines) and dust (blue lines) for three different simulations at a time of 9.5 Porb. The upper panels the disk are coplanar, in the middle panels i0 = 30°, and in the lower panels i0 = 60° (this is the same as the top right panel in Figure 3). Note that the upper two simulations have a sink size of 5 au while the lower one has a sink size of 2 au.
Paper: Testing Self-organized Criticality across the Main Sequence Using Stellar Flares from TESS
Authors: Adina D. Feinstein, Darryl Z. Seligman, Maximilian N. Günther, Fred C. Adams
Figure caption: The cumulative flare frequency distributions (FFDs) in our sample of stars binned by the flare amplitude and subdivided into different mass bins; the slope, α, and error is given in the upper-right corner of each subpanel. The bins are the FFD for flares with a probability ≥0.9. The upper and lower errors on the FFD are defined as flares with probability ≥0.99 and ≥0.5. All bins exhibit clear power laws, although some bins are incomplete for low-amplitude flares (e.g., 0.05 ≤ M/M ⊙ ≤ 0.3) or high-amplitude flares (e.g., red giant branch).
Paper: Testing Self-organized Criticality across the Main Sequence Using Stellar Flares from TESS
Authors: Adina D. Feinstein, Darryl Z. Seligman, Maximilian N. Günther, Fred C. Adams
Figure caption: Comparison of measured cumulative distribution flare rate slopes, α, as a function of stellar mass. Our rates are plotted as stars. Literature values are plotted as circles and colored by the number of flares in the given sample; they range from 1 to 104 stars (Shibayama et al. 2013; Howard et al. 2019; Ilin et al. 2019, 2021; Lin et al. 2019; Yang & Liu 2019; Feinstein et al. 2020b; Günther et al. 2020; Raetz et al. 2020; Aschwanden & Güdel 2021). The highest-mass stars have higher flare rate indices (light green) than previously measured. Our RGB star (yellow) slope is within 1σ of that of main-sequence stars in the same mass range. The remaining data points fall within the expected range of self-organized critical systems. We estimate the masses of our RGB stars using results from Wu et al. (2019).
Paper: Testing Self-organized Criticality across the Main Sequence Using Stellar Flares from TESS
Authors: Adina D. Feinstein, Darryl Z. Seligman, Maximilian N. Günther, Fred C. Adams
Figure caption: A color–magnitude diagram (Gaia B  p  − R  p  color and absolute Gaia G magnitude, M  G ) for our sample colored by flare rate. The flare rate was calculated by weighting each flare by its output “probability” from stella. Here, we accounted for all identified flares, not just flares with probabilities ≥ 0.9. Stars toward the top of the main sequence tend to have higher flare rates. This trend could be due to being young and metal-rich or being binaries.
Paper: Homologous Coronal Mass Ejections Caused by Recurring Formation and Disruption of Current Sheet within a Sheared Magnetic Arcade
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Formation of the CS and trigger of reconnection in the first and third eruptions. (A) Current density   J  normalized by magnetic field strength  B  on the central vertical slice, the x = 0 slice, at different times in the simulation. The height of maximum current density is denoted in each panel. (B) A 1D profile of the magnetic field component B  z  and current density J along a horizontal line crossing perpendicular to the CS center (that is, the point with the largest J/B). The diamonds denote values on the grid nodes. The thickness of the CS is denoted, which is defined by the FWHM of a Gaussian function fitting (the thin black curve) of the profile of current density. (C) Distribution of vertical velocity on the same cross section shown in (A). The magnitudes of maximal Alfvénic Mach number are also given. Panels (D), (E), and (F) are the same as (A), (B), and (C), respectively, but at different times. Panels (A), (B), and (C) show the first eruption, and (D), (E), and (F) show the third.
Paper: Homologous Coronal Mass Ejections Caused by Recurring Formation and Disruption of Current Sheet within a Sheared Magnetic Arcade
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Evolution of magnetic field lines and velocity during the first and third eruptions of the entire simulation process. (A) Top view of magnetic field lines. The colored thick lines represent magnetic field line and the colors denote the value of a nonlinear force-free factor defined as α =  J  · B/B 2, which indicates how much the field lines are nonpotential. (B) A 3D prospective view of the same field lines shown in (A). (C) Distribution of velocity on the central cross section, i.e., the x = 0 slice. The largest velocity and Alfvénic Mach number are also denoted. Panels (D), (E) and (F) are the same as (A), (B) and (C), respectively, but at different times. Panels (A), (B) and (C) show the first eruption, and (D), (E) and (F) show the third. In first two panels of (F), the largest velocity and Alfvénic Mach number are only denoted below the reconnection region, i.e., below 100 Mm of the first panel and 150 Mm of the second panel.
Paper: Homologous Coronal Mass Ejections Caused by Recurring Formation and Disruption of Current Sheet within a Sheared Magnetic Arcade
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: The CS intensity, magnetic field, and decay index around the onset time of the three eruptions. (A) Evolution of maximum current density J (solid) on the x = 0 slice and its height (dotted) with time. Note that here time t = 0 represents the onset time of the three eruptions, that is, t = 78 for the first, t = 123 for the second, and t = 175 for the third. Red, blue, and gold represent the first, second, and third eruptions, respectively. Panels (B) and (C) are shown for the magnetic field component B  y  and the decay index of B  y , respectively, along the z axis at the onset of the three eruptions.
Paper: Homologous Coronal Mass Ejections Caused by Recurring Formation and Disruption of Current Sheet within a Sheared Magnetic Arcade
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: Temporal evolution of magnetic and kinetic energies in the simulation. (A) Evolution of magnetic energy E  M  (black line) and kinetic energy E  K  (blue line). The dotted curve shows the energy injected into the volume (that is, a time integration of the total Poynting flux) from the bottom boundary through the surface flow. The horizontal dashed line denotes the value of the total magnetic energy for an open force-free field with the same magnetic flux distribution on the bottom surface. (B) Releasing rate of magnetic energy (black line) and the increasing rate of kinetic energy (blue line). In all of the panels, the red, green, and orange lines denote the onset time of three different eruptions, respectively.
Paper: Homologous Coronal Mass Ejections Caused by Recurring Formation and Disruption of Current Sheet within a Sheared Magnetic Arcade
Authors: Xinkai Bian, Chaowei Jiang, Xueshang Feng, Pingbing Zuo, Yi Wang
Figure caption: The initial conditions of the simulation. (A) Magnetic flux distribution and surface flow (shown by the arrows) at the bottom surface. (B) The 3D prospective view of the field lines of the initial potential field. The colors denote the value of the height. (C) Profile of the magnetic vertical component B  z  and the velocity along the (x, z) = 0 line, i.e., the white dotted line in (A). (D) Same as (C), but along the ﹩(y=y{| }_{{B}_{z,\max }},z=0)﹩ line, i.e., the black dashed line in (A).
Paper: V1298 Tau with TESS: Updated Ephemerides, Radii, and Period Constraints from a Second Transit of V1298 Tau e
Authors: Adina D. Feinstein, Trevor J. David, Benjamin T. Montet, Daniel Foreman-Mackey, John H. Livingston, Andrew W. Mann
Figure caption: The TESS tica FFI target pixel file (TPF) overlaid with a sky image of V1298 Tau taken with the Digitized Sky Survey (DSS) r-band. V1298 Tau is highlighted by the white circle; nearby sources with TESS magnitudes <14 are marked with x’s. The two stars with white x’s (TICs 15756226 and 15756240) were simultaneously fit during our PSF modeling. The one star with black x (TIC 15756236) is a bright nearby source that was not included in our PSF modeling. While aperture photometry would be feasible for this system (yellow square), we found fitting three point-spread functions to the brightest stars extracted the cleanest light curve for V1298 Tau (https://github.com/afeinstein20/v1298tau_tess/blob/main/src/figures/tpf.py).
Paper: V1298 Tau with TESS: Updated Ephemerides, Radii, and Period Constraints from a Second Transit of V1298 Tau e
Authors: Adina D. Feinstein, Trevor J. David, Benjamin T. Montet, Daniel Foreman-Mackey, John H. Livingston, Andrew W. Mann
Figure caption: V1298 Tau extracted light curve from the SPOC-processed light curve for Sectors 43 and 44, with transits of V1298 Tau bcde highlighted by color. Each subplot contains the raw, normalized TESS flux (top) and the GP model removed flux (de-trended flux; bottom). Top row: extracted light curve with overplotted with our best-fit GP model for stellar variability (black). Bottom three rows: zoomed-in regions around the transits present in the TESS data. The GP best-fit model is overplotted on the raw, normalized flux. The best-fit transit models are overplotted on the de-trended flux. For overlapping transits (subpanel “Planets b, c, and e”), the sum of the transits is blotted in black.
Paper: V1298 Tau with TESS: Updated Ephemerides, Radii, and Period Constraints from a Second Transit of V1298 Tau e
Authors: Adina D. Feinstein, Trevor J. David, Benjamin T. Montet, Daniel Foreman-Mackey, John H. Livingston, Andrew W. Mann
Figure caption: Our calculated posterior probability to constrain the period of V1298 Tau e using transit timings from K2 and TESS. We tested discrete periods from q = 38–56 days and find the most likely period to be 44.17 days. The 2:1 resonance (48.28 days) with V1298 Tau b is plotted as the dashed vertical line (https://github.com/afeinstein20/v1298tau_tess/blob/main/src/figures/period_e.py).
Paper: V1298 Tau with TESS: Updated Ephemerides, Radii, and Period Constraints from a Second Transit of V1298 Tau e
Authors: Adina D. Feinstein, Trevor J. David, Benjamin T. Montet, Daniel Foreman-Mackey, John H. Livingston, Andrew W. Mann
Figure caption: Left: phase-folded TESS data (gray) with the new best-fit model (color) compared to the original K2 data (black). The residuals between the TESS data and each fit are shown underneath. Top right: the percent difference in measured R  p /R ⋆ from K2 vs. TESS R  p /R ⋆. A dashed line is shown at 0% to help visually differentiate between measured increases and decreases in planetary radii. The transit depths for V1298 Tau bcd are shallower in the new TESS data, while the transit depth for V1298 Tau e is deeper. Bottom right: the change in R  p /R ⋆ as a function of pixel for V1298 Tau b (left) and V1298 Tau e (right) overlaid with a sky image of V1298 Tau taken with the Digitized Sky Survey (DSS) r-band. We speculate the variation in transit depths could be due to contamination from nearby bright stars or starspot crossing events (https://github.com/afeinstein20/v1298tau_tess/blob/main/src/figures/dilution_check.py).
Paper: Double-power-law Feature of Energetic Particles Accelerated at Coronal Shocks
Authors: Feiyu Yu, Xiangliang Kong, Fan Guo, Wenlong Liu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: (a) DSA theory predicts a single power law for particles accelerated by a 1D planar shock, while the particle energy spectra often exhibit an exponential rollover at high energies (Ellison & Ramaty 1985). The fluence spectra in some large SEP events are better fitted by double power laws (Band et al. 1993). (b) A superposition scenario to explain the formation mechanism of the double-power-law energy spectrum. The blue solid line is obtained by the superposition of two energy spectra of “power law × exponential” form but with different break energies (E  B  = 10, 50 MeV nuc−1). The superposed energy spectrum resembles a double power law below a certain energy (∼200 MeV nuc−1).
Paper: TeV and keV–MeV Excesses as Probes for Hadronic Process in BL Lacertaes
Authors: Ji-Gui Cheng, Xiao-Li Huang, Ze-Rui Wang, Jian-Kun Huang, En-Wei Liang
Figure caption: The EBL absorption-corrected SEDs (solid black dots with error bars) and our leptohadronic model results (solid black curves). The gray points are the observed data without the EBL absorption correction. The purple inverted triangles indicate the upper limit of the Fermi/LAT observations from Tavecchio et al. (2010). Color lines represent the different radiation processes: blue for synchrotron, green for SSC, and red for π 0 decay. Solid lines are for the emission of the primary electrons and dashed lines are for the emission of the cascade electrons. The hadronic emission without considering the internal γγ absorption are also drawn with red translucent solid/dashed lines for demonstration.
Paper: Double-power-law Feature of Energetic Particles Accelerated at Coronal Shocks
Authors: Feiyu Yu, Xiangliang Kong, Fan Guo, Wenlong Liu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: (a) Spatial distribution of accelerated protons with energies >10 MeV as the shock propagates to 4.0 R ⊙. The shock front is indicated by the black circle. (b) Energy spectra of different ions (H, He, O, Mg, and Fe) accelerated by the shock in a Kolmogorov turbulence spectrum. The solid curves are the fitting energy spectra using the Band function (Band et al. 1993) with low-energy indices γ 1 ∼ 1.3 and high-energy indices γ 2 ∼ 2.4. (c) Spectral break energy E  B  vs. the ion charge-to-mass ratio Q/A. The solid line shows the fitting with a power-law function E  B  ∼ (Q/A) α .
Paper: TeV and keV–MeV Excesses as Probes for Hadronic Process in BL Lacertaes
Authors: Ji-Gui Cheng, Xiao-Li Huang, Ze-Rui Wang, Jian-Kun Huang, En-Wei Liang
Figure caption: Examination of the detection capability of some instruments for the TeV and MeV excesses in the TeV and MeV bands. The solid lines are our model results presented in Figure 1 by considering the EBL absorption. The dashed lines mark the EBL-absorbed SSC component of the primary electron population. The one-year sensitivities of the instruments are plotted with dashed–dotted lines in different colors as marked in the plot.
Paper: TeV and keV–MeV Excesses as Probes for Hadronic Process in BL Lacertaes
Authors: Ji-Gui Cheng, Xiao-Li Huang, Ze-Rui Wang, Jian-Kun Huang, En-Wei Liang
Figure caption: Intrinsic (black dots) and observed (gray dots) SEDs of Mrk 421 and our theoretical modeling (showing with the same symbols as that in Figure 1) together with examination of detection capability with some instruments for the TeV and MeV excesses in the TeV and MeV bands (showing with the same symbols as that in Figure 4).
Paper: TeV and keV–MeV Excesses as Probes for Hadronic Process in BL Lacertaes
Authors: Ji-Gui Cheng, Xiao-Li Huang, Ze-Rui Wang, Jian-Kun Huang, En-Wei Liang
Figure caption: The cooling rates of the primary synchrotron and SSC as well as the primary pγ components. The upper panel and the lower panel are the cooling rates of the primary electrons and protons for the 4 BL Lacs.
Paper: Double-power-law Feature of Energetic Particles Accelerated at Coronal Shocks
Authors: Feiyu Yu, Xiangliang Kong, Fan Guo, Wenlong Liu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: Panel (a): as in Figure 2(a), the spatial distribution of accelerated protons with energies >10 MeV as the shock propagates to 4.0 R ⊙. Panels (b) and (c): energy spectra of accelerated protons in regions I and II, and region III, respectively. Solid lines are the fits to the spectra using the exponential rollover function in regions I and II, and the Band function in region III. Panel (d): energy spectra in regions IV and V, and the superposed energy spectrum of these two regions. Panel (e): energy spectra in regions IV and II, and the superposed energy spectrum of region IV and 0.05 × region II.
Paper: Double-power-law Feature of Energetic Particles Accelerated at Coronal Shocks
Authors: Feiyu Yu, Xiangliang Kong, Fan Guo, Wenlong Liu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: Panels (a), (c) and (e): energy spectra of accelerated particles, with the spectral indices of magnetic turbulence being 1.9, 1.1, and 0.5, respectively. The solid curves are fits to the spectra using the Band function. Panels (b), (d), and (f): spectral break energy E  B  vs. the ion charge-to-mass ratio Q/A.
Paper: Double-power-law Feature of Energetic Particles Accelerated at Coronal Shocks
Authors: Feiyu Yu, Xiangliang Kong, Fan Guo, Wenlong Liu, Zelong Jiang, Yao Chen, Joe Giacalone
Figure caption: Panels (a) and (b): spatial distributions of Fe and O with energies >10 MeV nuc−1 as the shock propagates to 3.5 R ⊙. Panels (c) and (d): variations of Fe/O with energy in regions I and II when the shock moves to 3.5 R ⊙, and in region III when the shock moves to 3 R ⊙ and 3.5 R ⊙. The values in each curve have been normalized to that at 100 keV nuc−1.
Paper: Rapid Bursts of Magnetically Gated Accretion in the Intermediate Polar V1025 Cen
Authors: Colin Littlefield, Jean-Pierre Lasota, Jean-Marie Hameury, Simone Scaringi, Peter Garnavich, Paula Szkody, Mark Kennedy, and McKenna Leichty
Figure caption: The combined CRTS, ASAS-SN, and ATLAS light curve of V1025 Cen. The timespan of the TESS observations is indicated in red. V1025 Cen experienced a low-accretion state between 2015 and 2018, and we believe that the unblended ATLAS data offer a better measurement of its depth compared to the blended ASAS-SN data. A single outburst, with a minimum amplitude of 0.6 mag, was detected by ASAS-SN during the TESS observations. There were several additional bursts in the months before and after the TESS observation, and the CRTS data show a single burst of unknown duration in 2009.
Paper: Rapid Bursts of Magnetically Gated Accretion in the Intermediate Polar V1025 Cen
Authors: Colin Littlefield, Jean-Pierre Lasota, Jean-Marie Hameury, Simone Scaringi, Peter Garnavich, Paula Szkody, Mark Kennedy, and McKenna Leichty
Figure caption: TESS light curve of V1025 Cen, with simultaneous ASAS-SN observations overlaid on the secondary y-axis. Each TESS datum is a 30 minute integration, while the ASAS-SN observations are 90 s exposures.
Paper: Rapid Bursts of Magnetically Gated Accretion in the Intermediate Polar V1025 Cen
Authors: Colin Littlefield, Jean-Pierre Lasota, Jean-Marie Hameury, Simone Scaringi, Peter Garnavich, Paula Szkody, Mark Kennedy, and McKenna Leichty
Figure caption: An enlargement of each outburst (blue markers) from Figure 3, superimposed upon the other 11 outbursts (gray lines). The approximate midpoint of each outburst is shown in each panel. Each burst lasted for fewer than six hours, with a mean full width at half-maximum of 3.0 ± 1.0 hr.
Paper: Rapid Bursts of Magnetically Gated Accretion in the Intermediate Polar V1025 Cen
Authors: Colin Littlefield, Jean-Pierre Lasota, Jean-Marie Hameury, Simone Scaringi, Peter Garnavich, Paula Szkody, Mark Kennedy, and McKenna Leichty
Figure caption: Power spectrum of V1025 Cen during the intervals between the bursts. fs refers to the sampling frequency of 48 cycles d−1, while ω is the WD spin frequency and Ω is the binary orbital frequency. Because ω (40.25 cycles d−1) is above the Nyquist frequency of the data (24 cycles d−1), it produces an alias at a frequency of fs − ω = 7.75 cycles d−1. The power near 5 cycles d−1 is of unknown origin.
Paper: Observational Signatures of Tearing Instability in the Current Sheet of a Solar Flare
Authors: Lei Lu, Li Feng, Alexander Warmuth, Astrid M. Veronig, Jing Huang, Siming Liu, Weiqun Gan, Zongjun Ning, Beili Ying, and Guannan Gao
Figure caption: Snapshots of the eruption recorded by the 131 Å filter of SDO/AIA. West is rotated to the top and south to the right. Panel (a) shows the flux rope formed in an earlier confined C4.5 flare. Panels (b)–(r) show the eruption and evolution of the flux rope and the associated M7.7 flare. “S1” and “S2” in panel (c) indicate two slits placed along and perpendicular to the current sheet. Panels (d)–(l) are running ratio images, showing motions of two blob-like plasmoids. “R1” and “R2” in panel (f) indicate two subregions used for the DEM analysis. The arrow in panel (r) refers to the long current sheet. The contours overplotted in panels (m)–(r) show the RHESSI X-ray sources at 6–12 keV (blue) and 25–50 keV (cyan) reconstructed with the “clean” algorithm. The percentages define the contour levels.
Paper: Observational Signatures of Tearing Instability in the Current Sheet of a Solar Flare
Authors: Lei Lu, Li Feng, Alexander Warmuth, Astrid M. Veronig, Jing Huang, Siming Liu, Weiqun Gan, Zongjun Ning, Beili Ying, and Guannan Gao
Figure caption: Temporal evolution of plasma inflows and outflows during magnetic reconnection as observed in EUV by SDO/AIA. (a) Time–distance plot in AIA 131 Å along the current sheet (S1), showing the eruption of the flux rope and the bidirectional reconnection outflows. (b) Time–distance plot in AIA 171 Å along S2 (perpendicular to the current sheet), showing the separation (blue lines) and approach (cyan lines) of oppositely directed magnetic structures (the numbers denote the average speeds in units of km s−1). The horizontal white dashed line denotes the position of the current sheet. (c) Time profiles of the RHESSI X-ray emission in different energy bands and time derivative of GOES flux in 1–8 Å. The two vertical dashed lines indicate the flare impulsive phase.
Paper: Observational Signatures of Tearing Instability in the Current Sheet of a Solar Flare
Authors: Lei Lu, Li Feng, Alexander Warmuth, Astrid M. Veronig, Jing Huang, Siming Liu, Weiqun Gan, Zongjun Ning, Beili Ying, and Guannan Gao
Figure caption: Temporal evolution of the physical parameters of Blob1. (a) Intensity distributions along S1 at eight selected times. The curves are shifted vertically to avoid overlap. “h1” and “h2” indicate the lower and upper boundaries of the blob. (b) Evolution of the blob height (h = (h1 + h2)/2). The size (h2 − h1) of the blob is regarded as the uncertainties (error bars). (c) The electron density inside the blob. (d) The DEM-weighted temperature of the blob. The error bars in (c) and (d) are obtained from 100 Monte Carlo simulations.
Paper: Observational Signatures of Tearing Instability in the Current Sheet of a Solar Flare
Authors: Lei Lu, Li Feng, Alexander Warmuth, Astrid M. Veronig, Jing Huang, Siming Liu, Weiqun Gan, Zongjun Ning, Beili Ying, and Guannan Gao
Figure caption: The X-ray and radio observations of the flare impulsive phase. (a) GOES soft X-ray fluxes in 1–8 Å (red line) and 0.5–4 Å (blue line), the two vertical dashed lines indicate the flare impulsive phase from 05:16 to 05:43 UT. (b) Combined radio dynamic spectra obtained by the Yunnan (yellow vertical bar) and Culgoora (magenta vertical bar) spectrographs, showing drifting pulsation structures (DPSs). The overplotted magenta and white light curves show the hard X-ray (50–100 keV) and time derivative of GOES 1–8 Å fluxes, respectively. (c) Zoomed-in view of a pair of oppositely drifting structures. The arrows points to some spike-like structures.