adsabs/AstroCLIMB huggingface dataset:
Paper: Post-outburst Evolution of Bona Fide FU Ori-type V2493 Cygnus: A Spectro-photometric Monitoring
Authors: Arpan Ghosh, Saurabh Sharma, Joe P. Ninan, Devendra K. Ojha, Bhuwan C. Bhatt, D. K. Sahu, Tapas Baug, R. K. Yadav, Puji Irawati, A. S. Gour, Neelam Panwar, Rakesh Pandey, Tirthendu Sinha, Aayushi Verma
Figure caption: Folded phase plot of the W  λ  of the Ca II IRT lines. The periods obtained are 12.3, 9.5, and 10.2 days, respectively, for λ8498 Å, λ8542 Å, and λ8662 Å lines. The folding is done using the data obtained during our entire monitoring period. The obtained periodicities are calculated with a 2σ confidence label.
Paper: Post-outburst Evolution of Bona Fide FU Ori-type V2493 Cygnus: A Spectro-photometric Monitoring
Authors: Arpan Ghosh, Saurabh Sharma, Joe P. Ninan, Devendra K. Ojha, Bhuwan C. Bhatt, D. K. Sahu, Tapas Baug, R. K. Yadav, Puji Irawati, A. S. Gour, Neelam Panwar, Rakesh Pandey, Tirthendu Sinha, Aayushi Verma
Figure caption: Top panel shows the MRES absorption lines of Ca I λ6122 Å and Fe I λ6142 Å, which show the evidence of disk rotation. The gray plot represents the original spectra, and the darker plot is the 3 pixel smoothed spectra of the original spectra. Bottom panel shows the evolution of the W  λ  of O I λ7773 Å line, which acts as a tracer for disk turbulence.
Paper: Post-outburst Evolution of Bona Fide FU Ori-type V2493 Cygnus: A Spectro-photometric Monitoring
Authors: Arpan Ghosh, Saurabh Sharma, Joe P. Ninan, Devendra K. Ojha, Bhuwan C. Bhatt, D. K. Sahu, Tapas Baug, R. K. Yadav, Puji Irawati, A. S. Gour, Neelam Panwar, Rakesh Pandey, Tirthendu Sinha, Aayushi Verma
Figure caption: MRES spectra showing blueshifted absorption lines that are tracing the outflowing winds. The gray plot represents the original spectra, and the darker plot is the 3 pixel smoothed spectra of the original spectra.
Paper: Post-outburst Evolution of Bona Fide FU Ori-type V2493 Cygnus: A Spectro-photometric Monitoring
Authors: Arpan Ghosh, Saurabh Sharma, Joe P. Ninan, Devendra K. Ojha, Bhuwan C. Bhatt, D. K. Sahu, Tapas Baug, R. K. Yadav, Puji Irawati, A. S. Gour, Neelam Panwar, Rakesh Pandey, Tirthendu Sinha, Aayushi Verma
Figure caption: Figure showing the correlation between the W  λ  of the different spectroscopic features of V2493 Cyg.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Mass–luminosity relation, main-sequence lifetime, and effective temperatures of stars from Schaerer (2002). Formulations of the fitting results are given in the main text. The green line (Ekström et al. 2012; Georgy et al. 2013; invalid for ≳120M ⊙) is in good agreement with that of Schaerer (2002).
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Global SED of AGNs with star formation with extinction, which corresponds to Figure 7 (﹩{\dot{m}}_{{\rm{w}}}^{0}={10}^{-9}{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩). AGN disks have the same parameters as Figure 18.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Yields of Fe and Mg elements produced by the present model are shown by the left panel. We take ﹩{E}_{\mathrm{SN}}=30\times {10}^{51}\,﹩ergs in the model. The Fe and Mg abundances are about 10 times that of the solar at ∼107  yr, but Fe is just about the solar abundance before ∼5 × 106 yr. [α/Fe] is just the solar value. This result is generally in agreement with the Chandra observations of Hua et al. (2023).
Paper: White Dwarfs Revealed in Gaia’s Candidate Compact Object Binaries
Authors: Anindya Ganguly, Prasanta K. Nayak, Sourav Chatterjee
Figure caption: Top: M LC vs. M DR. Each blue dot represents a candidate from the ATF22 and SHA23 catalogs. Orange open circles show the candidates for which we found UV excess. The red line shows the Chandrasekhar mass limit and the red-shaded region represents the expected limiting mass for NSs. Bottom: P orb vs. distance for the same sources. All of them are in detached wide orbits and relatively close to us. Blue dots and orange circles have the same meaning.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the TWA 7 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 36 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the phase dispersion minimization periodogram for the HD 92945 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 9 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the HD 61005 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 7 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Evidence for Misalignment between Debris Disks and Their Host Stars
Authors: Spencer A. Hurt, Meredith A. MacGregor
Figure caption: Top left: the Lomb–Scargle periodogram for the TWA 25 TESS PDCSAP light curve is shown in black. The dashed gray line marks the 1% FAP level while the shaded red region denotes the 1σ confidence interval for the rotation period posterior. Top right: the phase-folded light curve using the peak period from the Lomb–Scargle periodogram. Bottom left: the black points show data from TESS Sector 10 while the red line and shaded region respectively mark the mean and 1σ confidence interval for the GP model. Bottom right: the histogram shows the rotation period posterior derived from the GP model while the dash red lines mark the median and 1σ interval.
Paper: Suprathermal Electron Transport and Electron Beam Formation in the Solar Corona
Authors: Bofeng Tang, Haihong Che, Gary P. Zank, Vladimir I. Kolobov
Figure caption: Radial evolution of the velocity of suprathermal electrons u b without scattering terms, normalized by v th0 and c in the rest frame of the Sun using a electron temperature T c0 = 107 K and ﹩{v}_{\mathrm{th}0}={\left(2{k}_{{\rm{B}}}{T}_{{\rm{c}}0}/m\right)}^{1/2}﹩ of the acceleration region. In the left panel, the electron VDF at the inner boundary is a Maxwellian only (δ = 1). In the right panel, the electron VDF at the inner boundary is a combination of a Maxwellian with weight δ = 0.8 and an isotropic power law with α = 4 and weight 0.2 (=1 − δ). The shaded areas indicate the distance range from 0.05 to 0.4 R s. The labels of the curves (G1–G6) represent the simulation runs and their parameters (α, U d, and n B), which are listed in Table 1.
Paper: Striped Jets in Post–Neutron Star Merger Systems
Authors: Emma Kaufman, I. M. Christie, A. Lalakos, A. Tchekhovskoy, D. Giannios
Figure caption: The dynamo-like action generates large-scale poloidal magnetic flux from a purely toroidal magnetic flux configuration and accretes it onto the BH (top panel, displaying the absolute value of magnetic flux in the northern hemisphere of the BH). Additionally, the dynamo-like action continuously generates flips in the magnetic flux (bottom panel, displaying magnetic flux normalized to the square root of the mass accretion rate). These flips in polarity result in the production of current sheets on the BH and hence striped jets. Interestingly, neglecting all nuclear physics and neutrino emission (BT-LDN model; see legend) results in stronger BH magnetic flux, as shown in the top panel, than all other models. However, the normalized flux is comparable across all models.
Paper: Suprathermal Electron Transport and Electron Beam Formation in the Solar Corona
Authors: Bofeng Tang, Haihong Che, Gary P. Zank, Vladimir I. Kolobov
Figure caption: Panels (A1) and (A2): radial evolution of the percentage increase in the beam velocity of suprathermal electrons χ  u . Panel (A1) corresponds to a Maxwellian velocity distribution (left panel of Figure 3), and panel (A2) corresponds to a Maxwellian with weight δ = 0.8 plus a power-law velocity tail (right panel of Figure 3). Panel (B): radial evolution of  ϵ  ⊥/ ϵ  ∥ for suprathermal electrons. Line colors and styles have the same meaning as in Figure 3. Panel (C): radial revolution of u b with different power-law indices α = 4, 6, and 8. The shaded areas indicate the distance range from 0.05 to 0.4 R s. The labels of the curve represent the simulation runs and their parameters (α, U d, and n B), which are listed in Table 1.
Paper: Suprathermal Electron Transport and Electron Beam Formation in the Solar Corona
Authors: Bofeng Tang, Haihong Che, Gary P. Zank, Vladimir I. Kolobov
Figure caption: Electron beam velocities (red dots) as a function of distance from the Sun for coronal type III bursts given by Reid & Kontar (2018a). Blue, black, and red solid/dotted lines represent the magnetic field decrease as r −5, r −3, and r −1. The temperatures of the coronal background and acceleration region are 106 and 107 K, respectively. Calculated bulk velocities are normalized by the electron thermal velocity of the acceleration region (u b/v th0; left black y-axis) and coronal background (u b/v the,cb; right green y-axis). The shaded area indicates the distance beyond 0.6 R s (400–700 Mm) where coronal type III radio bursts are frequently observed.
Paper: Suprathermal Electron Transport and Electron Beam Formation in the Solar Corona
Authors: Bofeng Tang, Haihong Che, Gary P. Zank, Vladimir I. Kolobov
Figure caption: Radial evolution of the bulk velocity of suprathermal electrons u b with scattering, normalized by v th0 and c in the rest frame of the Sun using a temperature T c0 = 107 K. The shaded areas indicate the distance range from 0.05 to 0.4 R s. The labels of the curves (G10–G16) denote the simulation runs and their parameters (magnetic configurations, plasma parameters, and scatterings), which are listed in Table 2.
Paper: Suprathermal Electron Transport and Electron Beam Formation in the Solar Corona
Authors: Bofeng Tang, Haihong Che, Gary P. Zank, Vladimir I. Kolobov
Figure caption: The 2D contour plots of the normalized electron VDF (﹩f/{f}_{\max }﹩) in the moving frame at 0.05, 0.2, and 0.4 R s in the case of δ = 0.8, α = 4, U d = 1v th0, and B = B 0/r 2. The influence of magnetic focusing on the radial evolution of the electron VDF is obvious. The maximum pitch angle of the electron VDF decreases, while the parallel part does not change.
Paper: Suprathermal Electron Transport and Electron Beam Formation in the Solar Corona
Authors: Bofeng Tang, Haihong Che, Gary P. Zank, Vladimir I. Kolobov
Figure caption: Schematic illustration of suprathermal electron transport and coronal electron beam formation inside the solar corona along a radial magnetic field. Initially, suprathermal electrons are accelerated during a solar flare eruption in the low corona. After the suprathermal electrons propagate upward several hundred megameters away from the acceleration region, coronal electron beams form due to magnetic focusing. These coronal electron beams have high bulk velocities and, therefore, can trigger ETSI and produce coronal type III radio bursts.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: The evolving AMS MFs. The panels are arranged as follows: horizontal rows from left to right with increases with β for a given ﹩{\dot{m}}_{0}﹩, and the vertical with increases of ﹩{\dot{m}}_{0}﹩ from upper to below. Stellar populations are evolving in the context of the dense environment of AGN accretion disks. Whatever the input stars are, the MFs rapidly evolve from the IMFs. AMS MF is significantly changed by their accretion, not only the slope but also the maximum mass of stars. The dotted lines mean MFs beyond t AGN, namely, the MFs cannot reach a stationary state. The time in years marked in the panels is the time attaining the stationary state of MFs.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Same as Figure 4, but the evolving AMS has high-winds of ﹩{\dot{m}}_{{\rm{w}}}^{0}={10}^{-9}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩, showing very strong cutoff features. The cutoff due to stellar winds is too strong to produce iron.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: The global scenario of parsec-scale CNRs. R SG is the self-gravitating radius, and R dust is the sublimating radius of dust particles. The black dots represent stellar-mass black holes (sMBHs), ★ symbols does accreting stars, and their sizes indicate magnitude of mass. The shallow blue and red clouds are ionized gaseous clouds in the normal BLRs and intermediate-line regions (ILRs; i.e., beyond R dust). The observed emission line spectra comprise two components with varying widths that originate from the BLR and ILR. The CNR is a complex environment consisting of accreting SMBHs, stars, and SNe. Both sMBHs and stars are accreting gas from the AGN disk. All of them are called AMSs in this series of papers. The inner part of accretion disks is responsible for powerful radiation, and the outer part acts as an Alchemy furnace of metals.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Same as Figure 4, but the evolving AMS has very-high-winds of ﹩{\dot{m}}_{{\rm{w}}}^{0}={10}^{-8}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩. The cutoff due to stellar winds is too strong to produce abundant iron.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Same as Figure 4, but the evolving AMS has with mid-winds of ﹩{\dot{m}}_{{\rm{w}}}^{0}={10}^{-10}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩. This still allows for the formation of very massive stars for iron.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Characteristic structure of AMSs formed in AGN accretion disks. The AGN disk is so dense that the stellar winds of the host stars are choked, forming a massive envelope. The envelope stalls somewhere and returns to the host stars. The shocked (choked) envelope could be hot enough to trigger hydrogen burning, leading to an increase in the helium cores of the stars due to the falling back of helium. We note that due to the high number density of AMSs, their envelopes can overlap and become clumpy.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Growth rate curves with different characteristic parameters. We fix stellar wind rates but adjust the accretion of the AMS. We plot stellar winds for four ﹩{\dot{m}}_{{\rm{w}}}^{0}﹩ values (in units of M ⊙ yr−1: very-high-winds in blue, high-winds in yellow, mid-winds in green, and low-winds in red, respectively). The shaded regions are the ranges of PISNe.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: Same as Figure 4, but the AMS is undergoing low-winds of ﹩{\dot{m}}_{{\rm{w}}}^{0}={10}^{-11}\,{M}_{\odot }\,{\mathrm{yr}}^{-1}﹩. This is the case with weak winds, but the MFs begin to show the pile-up features with a cutoff, in particular, for the cases with high ﹩{\dot{m}}_{\mathrm{ac}}^{0}﹩.
Paper: Star Formation in Self-gravitating Disks in Active Galactic Nuclei. III. Efficient Production of Iron and Infrared Spectral Energy Distributions
Authors: Jian-Min Wang, Shuo Zhai, Yan-Rong Li, Yu-Yang Songsheng, Luis C. Ho, Yong-Jie Chen, Jun-Rong Liu, Pu Du, Ye-Fei Yuan
Figure caption: An application to the young stellar disk in the GC. Panel (a) shows the MF evolution of AMSs when the central SMBH was active. Panel (b) shows the star injection stopped at t * = 8.5 × 106  yr. Panel (c) shows the evolution of AMSs after the SMBH quenches accretion, where the red line represents an interval of 106  yr after ﹩\dot{{\mathscr{M}}}=0﹩.
Paper: Influence of Solar Wind Variations on the Shapes of Venus’ Plasma Boundaries Based on Venus Express Observations
Authors: C. Signoles, M. Persson, Y. Futaana, S. Aizawa, N. André, S. Bergman, A. Fedorov, V. Lindwall, N. Martinez, C. Mazelle, S. Rojas Mata, A. Wolff, T. L. Zhang
Figure caption: Time series of upstream parameters and BS and ICB extrapolated terminator distances over the VEX mission. The corresponding orbit number is shown at the top of the figure. (a) Daily averaged (yellow) and monthly smoothed (red) SSN values. The vertical dotted pink line spawning the whole figure marks the separation between periods of low and high solar activity, on 2011 January 1 (VEX orbit 1716). (b) Extrapolated BS radius (using method II; see Section 2.5). (c) Extrapolated ICB radius at the terminator (see Section 2.5). (d) Measured dynamic pressure of the solar wind. (e) Measured IMF magnitude. (f) Measured Alfvén Mach number, as used in this study. The black lines in (b) and (c) show the trend of the median radius over intervals 100 days wide; the dashed red line represents the general median; and the blue envelope provides the 25th and 75th quartile. A histogram of the values at solar minimum and maximum for each panel is plotted to the right of each time series.
Paper: Influence of Solar Wind Variations on the Shapes of Venus’ Plasma Boundaries Based on Venus Express Observations
Authors: C. Signoles, M. Persson, Y. Futaana, S. Aizawa, N. André, S. Bergman, A. Fedorov, V. Lindwall, N. Martinez, C. Mazelle, S. Rojas Mata, A. Wolff, T. L. Zhang
Figure caption: Dependence of the BS shape on both solar activity and shock geometry. BS crossings (gray dots) at solar minimum (panels (a) and (b), blue lines) or maximum (panels (c) and (d), orange lines) and for the q ∥ (panels (a) and (c), dashed lines) or q ∥ (panels (b) and (d), dashed–dotted lines) shock crossings, with the corresponding and general fitted lines (colored and black lines, respectively). A comparison between all fits is shown in panel (e).
Paper: Influence of Solar Wind Variations on the Shapes of Venus’ Plasma Boundaries Based on Venus Express Observations
Authors: C. Signoles, M. Persson, Y. Futaana, S. Aizawa, N. André, S. Bergman, A. Fedorov, V. Lindwall, N. Martinez, C. Mazelle, S. Rojas Mata, A. Wolff, T. L. Zhang
Figure caption: Ions, electrons, and magnetic field measurements recorded on 2013 November 21, near the pericenter. Panels (a) and (b) show the energy–time spectrograms of ASPERA-4 ions (IMA) and electrons (ELS), respectively; panel (c) shows the MAG magnetic field measurements in the VSO coordinates; and panel (d) shows the VEX altitude above the Venus radius (i.e., Rv = 6052 km). The dashed vertical lines show the identified boundary crossing locations: red for the BS and yellow for the ICB.
Paper: The LIGO HET Response (LIGHETR) Project to Discover and Spectroscopically Follow Optical Transients Associated with Neutron Star Mergers 
Authors: M. J. Bustamante-Rosell, Greg Zeimann, J. Craig Wheeler, Karl Gebhardt, Aaron Zimmerman, Chris Fryer, Oleg Korobkin, Richard Matzner, V. Ashley Villar, S. Karthik Yadavalli, Kaylee M. de Soto, Matthew Shetrone, Steven Janowiecki, Pawan Kumar, David Pooley, Benjamin P. Thomas, Hsin-Yu Chen, Lifan Wang, Jozsef Vinkó, David J. Sand, Ryan Wollaeger, Frederic V. Hessman, Kristen B. McQuinn
Figure caption: Sample output from combining localization information for LIGO event S190425z as illustrated in Figure 1 with the GLADE galaxy catalog to produce a list of 20 galaxies prioritized by the likelihood of being the host of a LIGO alert burst of gravitational waves. The vertical scale gives the log of the probability, and the horizontal scale gives the position in hour of R.A. Blue (single bands between the east and west extremes) shows galaxies available on a single track, red (right bands) and green (left bands) show the time when a given galaxy can be observed on the west track and the east track, respectively.
Paper: Influence of Solar Wind Variations on the Shapes of Venus’ Plasma Boundaries Based on Venus Express Observations
Authors: C. Signoles, M. Persson, Y. Futaana, S. Aizawa, N. André, S. Bergman, A. Fedorov, V. Lindwall, N. Martinez, C. Mazelle, S. Rojas Mata, A. Wolff, T. L. Zhang
Figure caption: BS fits and comparison with other BS models. (a) BS crossings and least-squares fits in aberrated axisymmetric VSO coordinates, at solar minimum (blue dots, dashed black line) and solar maximum (orange dots, dashed–dotted black line). The solid black line is the fitted curve for all crossings. (b) BS fit comparison with other models at solar minimum (Smin) and solar maximum (Smax).