adsabs/AstroCLIMB huggingface dataset:
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: Distributions of the posterior samples from the Method 1 intensity localizations of sample pulses from PSRs B0329+54 and B0531+21 and for the sidelobe FRBs 20190125B and 20190202B.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: Distributions of the posterior samples from the Method 1 intensity localizations of sample pulses for the sidelobe FRBs 20190210D, 20191104B, 20191202A, and 20191219E.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption: Distributions of the posterior samples from the Method 1 intensity localizations for the sidelobe FRBs 20201105A, 20201129A, 20210310B, and 20210810A.
Paper: Do All Fast Radio Bursts Repeat? Constraints from CHIME/FRB Far Sidelobe FRBs
Authors: Hsiu-Hsien Lin, Paul Scholz, Cherry Ng, Ue-Li Pen, Mohit Bhardwaj, Pragya Chawla, Alice P. Curtin, Dongzi Li, Laura Newburgh, Alex Reda, Ketan R. Sand, Shriharsh P. Tendulkar, Bridget Andersen, Kevin Bandura, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Matt Dobbs, Fengqiu Adam Dong, Gwendolyn Eadie, Emmanuel Fonseca, B. M. Gaensler, Utkarsh Giri, Antonio Herrera-Martin, Alex S. Hill, Jane Kaczmarek, Joseph Kania, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Calvin Leung, Kiyoshi W. Masui, Juan Mena-Parra, Bradley Ward Meyers, Daniele Michilli, Nikola Milutinovic, Anna Ordog, Aaron B. Pearlman, Ziggy Pleunis, Masoud Rafiei-Ravandi, Mubdi Rahman, Scott Ransom, Pranav Sanghavi, Kaitlyn Shin, Kendrick Smith, Ingrid Stairs, David C Stenning, Keith Vanderlinde, Dallas Wulf
Figure caption:  I(f) of the far sidelobe event of B0329+54 (left) and B0531+21 (right). The solid and dashed lines represent the data and the Gaussian model, respectively.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: Top: FUV-BaF2 flux in units of 10−14  erg cm−2 s−1 Å−1. Middle: NUV-B15 filter flux in units of 10−14 erg cm−2 s−1 Å−1. Bottom: unabsorbed X-ray flux in the 2–10 keV energy band in units of 10−10 erg cm-2  s−1. The black vertical lines are the error on the FUV/NUV fluxes.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: Total unabsorbed continuum model for all the observations. The shaded energy bands show the NUV-B15 (gray), FUV-G1/G2 (sky blue), SXT (green), LAXPC (yellow), and CZTI (pink).
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: The black solid line shows the final best-fit unabsorbed total model and the gray line is the same for the absorbed model. The different unabsorbed components are shown by green dashed–dotted: accretion disk emission; red dashed: Comptonized disk emission; blue dotted: soft excess and the Compton hump (reflection emission); fuchsia: host galaxy (sb_temp) template. The dereddened and unabsorbed spectral data are shown by the orange star (NUV-B15), yellow-filled squares (FUV-G1), green-filled circles (SXT), blue-filled diamonds (LAXPC), and red-filled triangles (CZTI).
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: UV and X-ray joint final best-fit model for the five observations. For each figure, the upper panel shows the best-fit model and data. The dashed lines show the emission line components. The lower panel shows the (data-model)/error. The data are rebinned for plotting purposes. UVIT/FUV-G1 and FUV-G2 spectra are in orange and cyan, NUV-B15 and FUV-BaF2 data points are represented by the triangle and star symbols, respectively, SXT spectrum in green, LAXPC spectrum in red, and CZTI spectrum in blue.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: Upper panels: for clarity, only the UVIT/FUV-G1 spectrum with the best-fit total model is shown (red). The model components are the intrinsic and Galactic absorbed power law (green solid line), Gaussian emission lines (cyan dashed line), and host galaxy template model (black dotted line). Lower panels: (data-model)/error. The green triangle and yellow star show the NUV-B15 and FUV-BaF2 photometric flux points.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: Variation in the UV color FUV–NUV with the observed FUV flux.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: FUV-G1 image of NGC 4151. The background can be seen to be significantly contaminated by the emission from the spiral arms. The cyan rectangular box shows the background extraction region for FUV-G1 in obs4.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: Obs1: the (data-model)/error before (top) and after (bottom) using the XABS model component.
Paper: Multi-epoch UV–X-Ray Spectral Study of NGC 4151 with AstroSat
Authors: Shrabani Kumar, G. C. Dewangan, P. Gandhi, I. E. Papadakis, N. P. S. Mithun, K. P. Singh, D. Bhattacharya, A. A. Zdziarski, G. C. Stewart, S. Bhattacharyya, S. Chandra
Figure caption: The NUV photometric data and the FUV-grating (left), and SXT, LAXPC and CZTI (right) count spectra from all five observations.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: Heliographic coordinates of the HXR flares observed by STIX (magenta and teal triangles), EUV jets/brightenings (small orange and black circles), and of the magnetic connection points of, from left to right, SolO (blue symbols), STA (red symbols), and L1 (green symbols) estimated using the Parker-PFSS-ADAPT (PPA) method (crosses) or just a Parker spiral configuration (solid lines). Magenta (teal) triangles indicate when the HXR flare occurred in AR 13141 (AR 13140). Small orange (black) circles indicate when the EUV jets and/or brightenings occurred in the vicinity of AR 13141 (AR 13140). The vertical dotted–dashed lines indicate the SRT of the >65 keV SEE events observed by SolO (left column), STA (middle column), and Wind (right column). The shaded areas highlight the clusters of footpoints at similar longitudes that evolve together in time as obtained by the PPA method.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: From top to bottom: Time profiles of 0.23–0.32 MeV nucleon−1 H (red), 3He (black), 4He (blue), O (green), and Fe (orange) ion intensities; mass spectrogram for elements from He to Fe for ions with energies 0.3–10 MeV nucleon−1; and 1/ion speed vs. time of arrival for ions of mass 10–70 AMU. The dashed oblique lines indicate ion increases with velocity dispersion signatures. The dispersionless low-energy ion intensity enhancement late on November 12 is due to a local spatial magnetic field enhancement (see Figure A1(c1)) whereas at higher energies were due to the onset of the ion event #4.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: (a) 10 minute averages of the electron intensities measured by the sunward apertures of EPT (three top traces) and of HET (orange trace); (b) 10 minute ion intensities measured by the sunward aperture of EPT (three top traces) and proton intensities measured by the sunward aperture of HET (orange and black traces); (c)–(e) 30 minute averages of the H (red), 3He (black), 4He (blue), O (green), and Fe (orange) ion intensities at (c) ∼250 keV nucleon−1, (d) ∼700 keV nucleon−1, and (e) ∼2 MeV nucleon−1. In panel (d), the numbers 1 through 6 identify the distinctive low-energy ion intensity enhancements observed during this period, whereas 3He identifies an extremely 3He-rich intensity enhancement observed early on November 10.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: SDO/AIA 193 Å running difference images shortly after the origin of the ion events #4 (a), #5 (b), and #3 (c) as identified in Figure 5. The solar eruption and CF in panel (d) was not associated with any particle event. The eruptions in panels (a) and (b) were associated with white-light SOHO/LASCO CMEs. No white-light CMEs were identifiable in association with the eruptions in panels (c) and (d).
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: From top to bottom: (a) Intensity of the type III radio emissions detected by STA/SWAVES at 1 MHz; (b) 304 Å EUV intensity integrated over the indicated area where the main jets were detected using STA/EUVI observations (details are given in the text); (c) ∼75 keV electron intensities as measured by the sunward apertures of STA/SEPT (red) and SolO/EPD/EPT (blue); (d) ∼6–10 MeV proton intensities detected by STA/LET (red) and SolO/EPD/HET (blue); (e) 1–8 Å SXR intensities measured by GOES (black) and 12–25 keV HXR count rates provided by SolO/STIX (teal). The vertical dotted–dashed lines indicate the estimated electron release times as listed in column (8) of Table 1. The red circles in panels (a) indicate the type III radio bursts for which Langmuir waves were observed in situ by STA/SWAVES (see Section 3.2).
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: The same as Figure 7 but using SDO/AIA 304 Å observations in panels (b).
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: (a) Electron spectrograms combining intensities collected by the sunward aperture of EPT (at energies ≳35 keV) and by STEP (at energies ≲35 keV) on board Solar Orbiter. A total of 32 > 10 keV electron events with discernible onsets can be distinguished (see text for details). (b) Radio dynamic spectrum obtained from the SWAVES instrument on board STA showing the sequence of type III radio bursts (see Section 3.2).
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: SDO/AIA 193 Å image taken on 2022 November 11 at 11:41 UT. At that time, NOAA ARs 13140 and 13141 were located close to central meridian. An EUV jet is observed at the southwestern edge of AR 13141. The red contours identify coronal holes (CH) surrounding the ARs. The blue, red, and green dots indicate the footpoint locations of the nominal field lines connecting to SolO, STA, and L1, respectively.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: Distributions of the time delays between electron SRTs and the onset of the associated (a) EUV emissions, (b) HXR flares, and (c) type III radio bursts as listed in Table 1. The times listed in Table 1 have been rounded to 1 minute resolution, and the bins used in the histograms are 2 minute wide. The gray (black) histograms are for >10 keV (>65 keV) SEE events observed by SolO. Positive delays indicate that the estimated SRT occurred after the onset of the associated (a) EUV emission, (b) HXR flare, and (c) type III radio burst.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Normalized density perturbation for runs with different disk aspect ratios. The parameters are identical to those in the representative runs (NL-hm runs) in Section 3, except for the disk aspect ratio. Detailed parameter settings are provided in Table 1. (a): snapshot with P orb = 20000P 0 for run NL-hs-S-NR (h 0 = 0.05, σ  ϕ  = 0.236, ϵ = 0.8, α = 10−3, β = 10, p = −1.0). (b): snapshot with P orb = 20000P 0 for run NL-hs-R-NR (h 0 = 0.05, σ  ϕ  = 0.236, ϵ = 0.5, α = 10−4, β = 1, p = −1.0). (c): snapshot with P orb = 20000P 0 for run NL-hs-V-NR (h 0 = 0.05, σ  ϕ  = 0.236, ϵ = 0.5, α = 0, β = 0.001, p = −1.0). (d): snapshot with P orb = 3000P 0 for run NL-hl-S-NR (h 0 = 0.15, σ  ϕ  = 0.236, ϵ = 0.8, α = 10−3, β = 10, p = −1.0). (e): snapshot with P orb = 10000P 0 for run NL-hl-R-NR (h 0 = 0.15, σ  ϕ  = 0.236, ϵ = 0.5, α = 10−4, β = 1, p = −1.0). (f): snapshot with P orb = 1500P 0 for run NL-hl-V-NR (h 0 = 0.15, σ  ϕ  = 0.236, ϵ = 0.5, α = 0, β = 0.001, p = −1.0).
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Statistics of the vortices's aspect ratio, rings’s eccentricity, and spirals’s pitch angles for 160 simulations. The structure of the figure is same as Figure 14.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: The demonstration of the vortex−ring transition situation. The parameters of these four plots are σ  ϕ  = 0.236, p = −0.5, ϵ = 0.5, α = 0.0001, β = 1; σ  ϕ  = 0.236, p = −0.5, ϵ = 0.8, α = 0.01, β = 0.001; σ  ϕ  = 0.236, p = −1.0, ϵ = 0.8, α = 0.01, β = 0.001; σ  ϕ  = 0.079, p = −0.5, ϵ = 0.8, α = 0, β = 0.1, respectively. All these cases can be found in Figures 14 and 15 as vortex or ring blocks covered by red hatch lines.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: The demonstration of the ring−spiral transition situation. The parameters of these four plots are σ  ϕ  = 0.236, p = −0.5, ϵ = 0.8, α = 0, β = 10; σ  ϕ  = 0.079, p = −1.0, ϵ = 0.8, α = 0.001, β = 1; σ  ϕ  = 0.079, p = −0.5, ϵ = 0.5, α = 0, β = 10; σ  ϕ  = 0.079, p = −0.5, ϵ = 0.5, α = 0.001, β = 1, respectively. All these cases can be found in Figures 14 and 15 as ring or spiral blocks covered by blue hatch lines.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Statistics of a substructures' vorticity and density ratio for 160 simulations. The structure of the figure is described in Appendix B and is similar to Figure 5.
Paper: Dynamical Consequence of Shadows Cast to the Outer Protoplanetary Disks. I. Two-dimensional Simulations
Authors: Zehao Su, Xue-Ning Bai
Figure caption: Normalized density perturbation for one-sided shadow. Left panel: spiral-forming disk with parameter taken to be same as run NL-hm-S-NR (Figure 2). Middle panel: ring-forming disk with parameter taken to be same as run NL-hm-R-NR (Figure 3). Right panel: vortex-forming disk with parameter taken to be same as run NL-hm-V-NR (Figure 4).
Paper: Almost All Carbon/Oxygen White Dwarfs Can Host Double Detonations
Authors: Ken J. Shen, Samuel J. Boos, Dean M. Townsley
Figure caption: Composition profiles vs. mass below the surface of our WD models with total masses given in the upper left corner of each panel. Mass fractions are as labeled in the 1.0 M ⊙ panel.
Paper: Almost All Carbon/Oxygen White Dwarfs Can Host Double Detonations
Authors: Ken J. Shen, Samuel J. Boos, Dean M. Townsley
Figure caption: Same as Figure 1 but vs. distance below the surface.