adsabs/AstroCLIMB huggingface dataset:
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: (a) GALEX observed flare frequency distribution in equivalent duration with 1σ error bars. The y-axis denotes frequency density d ν/d δ as defined in Equation (4), with the dashed line being the nominal power-law fit. The solid line is the corrected fit as described in Section 4.1. (b) Corrected GALEX equivalent duration FFD fits for individual M spectral types. Observed FFDs for individual spectral types are plotted in Figure D1. Fit parameters are given in Table 2.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Comparison of cumulative flare frequency distributions in equivalent durations. MUSCLES FFD is in the FUV (Loyd et al. 2018). TESS FFD is computed from Table 2 of Stelzer et al. (2022).
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: (a) GALEX flare frequency distribution in energy with 1σ error bars. The solid line denotes the power-law fit. The y-axis denotes frequency density dE/d δ as defined in Equation (5). (b) Energy FFD fits for individual M spectral types. Observed FFDs for individual spectral types are plotted in Figure D2. Fit parameters are given in Table 2.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Flare Length as a function of equivalent duration in sources binned at 10–30 s. Partially detected flares are excluded from this plot. The solid line shows a power-law fit with the 1σ error region shaded.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Comparison of flare relative amplitude frequency distributions used by Tilley et al. (2019) to those estimated from GALEX data. GALEX relative amplitude frequency distributions are obtained using the equivalent duration—flare length relation determined in Equation (3) and Figure 11.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: The cumulative fractional energy budget of M-dwarfs in the NUV as a function of local-to-quiescent flux ratios for different spectral types. The logarithm of equivalent durations corresponding to given flux ratios is shown on the top axis. The dashed line indicates the flux ratio of 2.66, which is 5σ above the quiescent for a source at the S/N = 3 threshold.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Occurrence rates of observed fluxes over 300 s greater than 5σ above quiescent (top), 10 times quiescent (middle) and 100 times the quiescent (bottom) as a function of spectral types. We consider flux 5σ above the quiescent over a period of 300 s to be a clear indication of high activity.
Paper: A Census of Near-UV M-dwarf Flares Using Archival GALEX Data and the gPHOTON2 Pipeline
Authors: Param Rekhi, Sagi Ben-Ami, Volker Perdelwitz, Yossi Shvartzvald
Figure caption: Flares detected on XMM-OM MoV source TIC 142206123 during observation ID 0148790101. The red regions are flares and suspect points not qualified as flares are plotted in yellow. The gray line shows the quiescent flux estimate modeled with FLAIIL.
Paper: The Role of Magnetic Shear in Reconnection-driven Flare Energy Release
Authors: J. Qiu, M. Alaoui, S. K. Antiochos, J. T. Dahlin, M. Swisdak, J. F. Drake, A. Robison, C. R. DeVore, V. M. Uritsky
Figure caption: (a) Evolution of the flare ribbon fronts, derived with the AIA 1600 Å images, superimposed on a radial photospheric magnetogram obtained from HMI/SHARP. (b) HXR 6–12 keV (RHESSI) centroids (diamonds; with f = 0.85, see the text) and the UV 1600 Å (AIA) centroids (pluses; with f = 0.7, see the text) superimposed on an EUV image in the AIA 171 Å passband. For clarity of display, we have reduced the cadence of the UV centroids to 72 s, or every third frame. (c) Total reconnection rate in terms of the flux change rate ﹩\dot{\psi }﹩ (black) measured in the positive field and negative field, respectively, the mean plane-of-sky motion velocity of the HXR 6–12 keV centroids, computed with the centroids measured with f = 0.75, 0.85, and 0.95 (red), and the HXR count rates at 35–80 keV (blue). (d) Close-up view of the footpoint (UV centroid, with f = 0.7, and at full cadence 24 s) trajectory and the looptop (X-ray 6–12 keV centroid, with f = 0.85) trajectory between 21:44-22:00 UT. In panels (a), (b), and (d), the colors represent the times of the observed signatures as indicated by the color bar. Note that the color code in (a) and (b) is the same as that in Figures 2, 5, and 6, but the color code in (d) is different. The curve in panels (a), (b), and (d) outlines the polarity inversion line of the radial magnetic field B  r . All images in this figure have been rotated to 21:00 UT, and measurements using these images reflect the coordinates at this reference time.
Paper: The Role of Magnetic Shear in Reconnection-driven Flare Energy Release
Authors: J. Qiu, M. Alaoui, S. K. Antiochos, J. T. Dahlin, M. Swisdak, J. F. Drake, A. Robison, C. R. DeVore, V. M. Uritsky
Figure caption: Left: evolution of flare ribbon fronts (color symbols) derived from the UV 1600 Å images by AIA during the (a) elongation, (b)–(c) fast-expansion, and (d)–(e) slow-expansion phases. Superimposed are the EUV images from AIA that show PRFLs anchored at the ribbon fronts and the hard X-ray sources at ≥30 keV (color contours) obtained from RHESSI. The colors of the ribbon fronts and HXR contours indicate the times given in the color bar at the right. Middle: PRFLs identified from AIA 304 Å images, superimposed with the ribbon fronts (pink symbols) during (a) elongation, (b), (c) fast-expansion, and (d), (e) slow expansion, on a pre-flare magnetogram of the photospheric radial magnetic field from HMI. The colors of the PRFLs indicate the times the PRFLs are identified in the AIA 304 Å images minus 15 minutes, the nominal cooling time (see the text in Section 4.2), which are the same colors used in Figure 6. Right: magnetic loops from the potential field extrapolation projected to the AIA image plane, superimposed on a pre-flare magnetogram of the photospheric radial magnetic field from HMI. Potential field loops are traced from ribbon fronts (pink symbols) during the different stages of the flare evolution. The colors of the potential field loops (right panels) indicate the times at which the ribbon fronts formed (left panels); see the color bar at the right.
Paper: The Role of Magnetic Shear in Reconnection-driven Flare Energy Release
Authors: J. Qiu, M. Alaoui, S. K. Antiochos, J. T. Dahlin, M. Swisdak, J. F. Drake, A. Robison, C. R. DeVore, V. M. Uritsky
Figure caption: Top panels: the shear angle θ lp of the PRFLs (1320 measurements) identified from AIA 304 Å images with respect to the vertical of the PIL of the photospheric radial magnetic field, measured at where the PRFLs cross the PIL, vs. the x position on the PIL (a) or times they are identified (b). The colors indicate the times PRFLs are identified in the AIA 304 Å images minus 15 minutes (see Section 4.2), which are the same as in the middle panels in Figure 5. The solid black curve in (b) presents the median θ lp every minute. For comparison, the dashed black curve shows the median θ lp every minute of PRFLs identified in the AIA 171 Å images. Bottom panels: the shear angle θ pot of the potential field lines (769 measurements) rooted at the flare ribbon fronts and projected to the AIA image plane with the vertical of the PIL, vs. the x position along the PIL (c) or the time (d) of the ribbon fronts. The color coding is the same as in the right panels of Figure 5. The solid black curve shows the median θ pot every two minutes.
Paper: The Role of Magnetic Shear in Reconnection-driven Flare Energy Release
Authors: J. Qiu, M. Alaoui, S. K. Antiochos, J. T. Dahlin, M. Swisdak, J. F. Drake, A. Robison, C. R. DeVore, V. M. Uritsky
Figure caption: Guide field and shear angle evolution in the ARMS eruptive flare model. (a) Guide-field ratio (−B  ϕ /B  r ) calculated upstream of the reconnecting current sheet at ϕ = 0 (black) and rate of total reconnected flux (red). Guide field ratio vs. the mean shear angle (θ) is shown in (b) and vs. its tangent in (c). The mean shear angle is the angle between the footpoints of a newly reconnected flare loop and the direction normal to the PIL, averaged over the region ∣ϕ∣ < 2°. The guide field is calculated at ϕ = 0, and the upstream is taken to be the location where the current density first attains 25% of its peak value when approaching the current sheet. The color indicates the time when the newly reconnected flare loops are identified and the corresponding guide field is calculated. The solid line in the center panel is a parabolic fit and the dashed line in the right panel corresponds to ﹩-{B}_{\phi }/| {B}_{r}| =\tan (\theta ).﹩
Paper: The Role of Magnetic Shear in Reconnection-driven Flare Energy Release
Authors: J. Qiu, M. Alaoui, S. K. Antiochos, J. T. Dahlin, M. Swisdak, J. F. Drake, A. Robison, C. R. DeVore, V. M. Uritsky
Figure caption: (a) Soft X-ray (1–8 Å) and its time derivative, hard X-ray (6–12 and 35–80 keV), and UV 1600 Å light curves of the flare obtained by GOES, RHESSI, and AIA, respectively. The solid vertical lines divide the flare evolution into three stages (see the text). (b) RHESSI X-ray 6–12 keV 80% contours plotted over an AIA 131 Å image at 22:40:59 UT. The colors indicate the midpoint of the RHESSI integration time interval; see the color bar above panel (a). The black arrows indicate the apparent motion of the HXR centroids over time. (c)–(f) HXR >30 keV contours superimposed on AIA 1600 Å images. RHESSI contour colors correspond to the color bar above panel (a) to easily follow the time evolution.
Paper: The Role of Magnetic Shear in Reconnection-driven Flare Energy Release
Authors: J. Qiu, M. Alaoui, S. K. Antiochos, J. T. Dahlin, M. Swisdak, J. F. Drake, A. Robison, C. R. DeVore, V. M. Uritsky
Figure caption: (a) Photospheric radial magnetogram obtained from HMI/SHARP. Color contours indicate magnetic flux density of ±200, 400, 800, and 1600 Mx cm−2. (b) 2D histogram of photospheric radial magnetic flux density (grayscale) on the southern (positive B  r ) and northern (negative B  r ) ribbons, respectively, integrated every 2 minutes. Red curves represent the mean magnetic field 〈B  r 〉 on the photosphere (solid) and the mean magnetic field extrapolated to 1 Mm above the photosphere (dashed) on the ribbons. These are compared with the total HXR count rates at 35–80 keV (blue; arbitrary units), and the total UV emissions (black) integrated on the positive and negative ribbons separately.
Paper: The Role of Magnetic Shear in Reconnection-driven Flare Energy Release
Authors: J. Qiu, M. Alaoui, S. K. Antiochos, J. T. Dahlin, M. Swisdak, J. F. Drake, A. Robison, C. R. DeVore, V. M. Uritsky
Figure caption: Left: temporal evolution of the nonthermal electron flux ﹩{{ \mathcal F }}_{e}﹩ as deduced from RHESSI spectral fits (black curve with gray uncertainties), and the modulated magnetic flux change rate using the deduced shear from ribbon fronts (orange) and the shear deduced from the PRFLs (red), which are shifted backward by a nominal cooling time of 15 minutes. Right: the modulated reconnection rate ﹩{\dot{\psi }}_{\mathrm{mod}}﹩ (blue), or the model-predicted nonthermal electron flux, calculated from Equation (2), using the reconnection rate ﹩\dot{\psi }﹩ (solid black) and the relative guide field ﹩{ \mathcal R }﹩ (dashed black) from the numerical simulation shown in Figure 9(a).
Paper: The Role of Magnetic Shear in Reconnection-driven Flare Energy Release
Authors: J. Qiu, M. Alaoui, S. K. Antiochos, J. T. Dahlin, M. Swisdak, J. F. Drake, A. Robison, C. R. DeVore, V. M. Uritsky
Figure caption: (a) The light curve of total UV 1600 Å emission from the flare ribbons (black), in comparison with that of the total emission of the EUV 304 Å (red) or the EUV 171 Å (blue) at locations along the PIL. (b) Histograms of the rise times of UV 1600 Å emission at 5800 ribbon-front pixels, as either the time it takes for the UV emission to rise from 6 times the pre-flare quiescent brightness to its peak (solid), or as the width of the half-Gaussian used to approximate the UV light curve from its rise to peak (dashed). (c) Histograms of the cooling times of PRFLs to the EUV 304 and 171 Å passbands estimated with the UFC model.
Paper: Using Tianwen-1 Differential One-way Range Signals to Probe Corotating Interaction Regions: Case Studies
Authors: Qingbao He, Zhichao Wang, Qinghui Liu, Kaijun Liu, Li Guo
Figure caption: Differential phase delays and their corresponding TEC changes (right axes) on 2021 February 11 (a), February 18 (b), and February 19 (c), respectively. The contribution of the Earth’s ionosphere has been removed.
Paper: Proton Synchrotron Origin of the Very-high-energy Emission of GRB 190114C
Authors: Hebzibha Isravel, Asaf Pe'er, Damien Bégué
Figure caption: Resulting spectra for parameters in our case (i): ξ  e  = ξ  p  plotted on top of the data of GRB 190114C at 90 and 120 s. The SED obtained from our model for the time bins (a) [T 0 + 68 − T 0 + 110] and (b) [T 0 + 110 − T 0 + 180]. Continuous line: electron synchrotron; dashed line: proton synchrotron; and dotted–dashed line: IC. The data are from Acciari et al. (2019) and are displayed to guide the eye. The parameters are E 53 = 40, n 0 = 80, ϵ  p,−1 = 8, p = 2.2, and α = 35, resulting in ϵ  B,−2 = 15.2, ξ  e  = ξ  p  = 0.026, and ϵ  e,−1 = 0.0385. The cutoff at ﹩{\gamma }_{p,\max }﹩ is attained by ﹩\exp (-\nu /{\nu }_{\max })﹩.
Paper: Proton Synchrotron Origin of the Very-high-energy Emission of GRB 190114C
Authors: Hebzibha Isravel, Asaf Pe'er, Damien Bégué
Figure caption: Parameter space for the dominant component at 0.2 TeV. In the gray region, electron-IC dominates where ϵ  B  ≪ ϵ  e , while proton synchrotron dominates below the solid lines if ϵ  B  ≫ ϵ  e , which colors correspond to the value of ϵ  p  as indicated in the legend. The other parameters are set to p = 2.2, ξ  e  = ξ  p  = 0.026, E 53 = 40, and n 0 = 80 (case (i)). The forbidden zones for each value of ϵ  p  are shown with the hatched regions in their respective colors. It is apparent that a proton-synchrotron model requires small ϵ  e  and large ϵ  p . The star represents the parameters for case (i).
Paper: Proton Synchrotron Origin of the Very-high-energy Emission of GRB 190114C
Authors: Hebzibha Isravel, Asaf Pe'er, Damien Bégué
Figure caption: Case (iii). ξ  e  = ξ  p  = 0.023, and p  e  = 2.2 while p  p  = 2.1. Same as Figure 2. The parameters we used here are E 53 = 30, n 0 = 15, ϵ  p,−1 = 8, and α = 41.45, ϵ  B,−2 = 12 and ϵ  e,−1 = 0.047. The cutoff at ﹩{\gamma }_{p,\max }﹩ is attained by ﹩\exp (-\nu /{\nu }_{\max })﹩.
Paper: Proton Synchrotron Origin of the Very-high-energy Emission of GRB 190114C
Authors: Hebzibha Isravel, Asaf Pe'er, Damien Bégué
Figure caption: Afterglow light curve in several energy bands, from X-ray to teraelectronvolt. The parameters for case (iii) are used to compute the model. These are E 53 = 30, n 0 = 15, ϵ  p,−1 = 8, resulting in α = 41.45, ϵ  B,−2 = 12, and ϵ  e,−1 = 0.047. The model and data for the LAT and MAGIC band are shifted by factors of 10−2 and 10−3, respectively. The dashed line shows the division between the prompt phase (T 0 ≤ 25 s) and the afterglow (T 0 > 25 s).
Paper: Proton Synchrotron Origin of the Very-high-energy Emission of GRB 190114C
Authors: Hebzibha Isravel, Asaf Pe'er, Damien Bégué
Figure caption: Case (ii). Same as Figure 2. The parameters are E 53 = 50, n 0 = 130, ϵ  p,−1 = 8, p = 2.2, α = 34 and ξ  p  = 0.2, ϵ  B,−2 = 13, ϵ  e,−1 = 0.0308, ξ  e  = 0.02 and so ξ  e /ξ  p  ≃ 0.1. The cutoff at ﹩{\gamma }_{p,\max }﹩ is attained by ﹩\exp (-\nu /{\nu }_{\max })﹩.
Paper: Using Tianwen-1 Differential One-way Range Signals to Probe Corotating Interaction Regions: Case Studies
Authors: Qingbao He, Zhichao Wang, Qinghui Liu, Kaijun Liu, Li Guo
Figure caption: Solar wind structures on 2021 February 11 (a) and 2021 February 18 (b) predicted by the WSA-Enlil model. The Earth, Mars, and STEREO-A positions and the corresponding DOR signal path are also marked.
Paper: Proton Synchrotron Origin of the Very-high-energy Emission of GRB 190114C
Authors: Hebzibha Isravel, Asaf Pe'er, Damien Bégué
Figure caption: The proton synchrotron component for our model in case (iii), together with the data from the three additional MAGIC observations (Acciari et al. 2019). The depletion of the observed flux is in agreement with our model.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: 3D representation of the magnetic configuration of the initial spheromak. We represent three sets of magnetic field lines: the blue ones correspond to the outer edge of the spheromak, the red ones to the axis of the internal flux rope, and the white ones to the orientation of the flux rope field lines. In the left panel, the handedness is positive since the flux rope corresponds to a right-handed helix. In the right panel, the handedness is negative since the flux rope corresponds to a left-handed helix. Credits: Camilla Scolini.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Comparison of the meridional profile of the ICME for positive (left panel) and negative (middle panel) handedness. We show the x–z plane in HEEQ coordinates when the ICME reaches Earth (blue point at 1 au). We show the proton number density per cubic centimeter. We can see that for the negative handedness case, the CME is elongated with a double sheath, probably due to the acceleration it gets from initial reconfiguration at 0.1 au. In the right panel, we show the radial evolution of the mean speed inside the ejecta for positive (green) and negative handedness (red).
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption:  g-band absolute magnitude of transients compared to the g-band absolute magnitude of their host galaxies. All the data points are nuclear transients (813 classified in green and 630 unclassified in blue). The box in the lower left corner represents the intrinsically low-luminosity transients in low-luminosity host galaxies, where Ia-TDEs are expected to occur. There are 136 transients in the selection box, 46 classified and 90 unclassified. The star markers show the most likely nuclear Ia-TDE candidates, and the diamond markers show the less likely off-nuclear Ia-TDE candidates.
Paper: Impact of the Solar Activity on the Propagation of ICMEs: Simulations of Hydro, Magnetic and Median ICMEs at the Minimum and Maximum of Activity
Authors: Barbara Perri, Brigitte Schmieder, Pascal Démoulin, Stefaan Poedts, Florian Regnault
Figure caption: Examples of detection of the shock, sheath, and magnetic cloud for various cases. For each case, the first row is the total magnetic amplitude in nanotesla, the second row the total velocity amplitude in kilometers per second, the third row the temperature in 10,000 kelvin, the fourth row the number density for the protons per cubic centimeter, and the last row β parameter of the plasma. The left panel shows the median case at the minimum of activity at 1 au. The right panel shows the same case, but at 0.4 au instead of 1 au. A yellow rectangle highlights the region corresponding to the sheath, and a blue rectangle the region corresponding to the magnetic cloud.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption: Top row: ZTF photometry in g and r band compared to the best-fit Ia-TDE model from M16, in terms of observing geometry angles θ and ϕ. Middle row: spectra of the best Ia-TDE candidates, corresponding to the model from M16, and comparisons with SNe Ia and an SN Iax from Nugent et al. (2011) and Blondin et al. (2012) at a similar phase to that of the candidate. Bottom row: r-band PS1/3π  images of the host galaxies of the Ia-TDE candidates; the red cross marks the center of the transient and its size corresponds to the 3σ  position uncertainties.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption: Top row: ZTF photometry in g and r band compared to the best-fit Ia-TDE model from M16, in terms of observing geometry angles θ and ϕ. Bottom row: r-band PS1/3π  images of the host galaxies of the Ia-TDE candidates; the red cross marks the center of the transient and its size corresponds to the 3σ  position uncertainties.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption:  g − r color measured during peak and at 15 days post peak for the Ia-TDE candidates, the models from M16, and a sample of SNe Ia and SNe Iax. The stars denote the best nuclear Ia-TDE candidates, while the diamonds are for the off-nuclear Ia-TDE candidates.
Paper: The Search for Thermonuclear Transients from the Tidal Disruption of a White Dwarf by an Intermediate-mass Black Hole
Authors: Sebastian Gomez, Suvi Gezari
Figure caption: The peak r-band absolute magnitude as a function of Δm 15 for the Ia-TDE candidates, the M16 models, and a sample of SNe Ia and SNe Iax. The stars denote the best nuclear Ia-TDE candidates, while the diamonds are for the off-nuclear Ia-TDE candidates.
Paper: Comprehensive Radiative MHD Simulations of Eruptive Flares above Collisional Polarity Inversion Lines
Authors: Matthias Rempel, Georgios Chintzoglou, Mark C. M. Cheung, Yuhong Fan, Lucia Kleint
Figure caption: Cross section from setup (A) along the cut indicated in Figure 1(b). Left panels show the strength of B  x  (field component along PIL), middle panels the vertical component of the field-line curvature, and right panels the mass density. Top to bottom, we show the time evolution as indicated. The red lines indicate the T = 50,000 K contour, the orange lines the B  z  = 0 contour. Field lines of the magnetic field within the y–z plane are shown in white. The thick white contour of the corrugated τ = 0.1 level is plotted to indicate the photosphere (at y > 30 Mm the coherent and strong positive polarity causes slight Wilson depression of the τ surface). A MFR carrying very little mass is formed mostly during the eruption.