adsabs/AstroCLIMB huggingface dataset:
Paper: Formation of Quiescent Prominence Magnetic Fields by Supergranulations
Authors: Qingjun Liu, Chun Xia
Figure caption: (a) Time evolution of the magnetic helicity fluxes as the total (solid line), the negative (dashed line), and the positive (dotted line) ones through the photosphere of model SR. (b) Similar curves as (a) for model SS. (c) Time evolution of the magnetic free energy of models SR (solid line) and SS (dashed line). (d) Magnetic helicity flux density on the photosphere overlaid with a horizontal velocity field as yellow arrows and contours of B  r  at ±16 G for model SR at time 36. (e) Similar plot to (d) for model SS.
Paper: Formation of Quiescent Prominence Magnetic Fields by Supergranulations
Authors: Qingjun Liu, Chun Xia
Figure caption: Comparative views of model SR and SS at times 15, 45, and 60. In panels (a)–(f), magnetic field lines, in rainbow colors, are integrated from uniformly sampled seed points along a radial white line starting from the cyan PIL at a fixed latitude. The photosphere is colored by a radial magnetic field saturated at ±20 G. Zoom-in views at time 15 are shown in panels (g) and (h), where gray arrows present the photospheric horizontal velocity field.
Paper: Formation of Quiescent Prominence Magnetic Fields by Supergranulations
Authors: Qingjun Liu, Chun Xia
Figure caption: Linking sheared loops to helical field lines via photospheric magnetic reconnection along the white PIL. (a) Top view of six selected magnetic field lines above the photospheric magnetogram with arrows presenting horizontal velocity. (b) Side view of the same magnetic field lines in (a) above a photospheric color map presenting supergranular cells. (c) Evolution of the total unsigned magnetic flux on the photosphere for models SR (solid line) and SS (dashed line).
Paper: XMM and NuSTAR Observations of an Optically Quiescent Quasar
Authors: Claire Greenwell, Poshak Gandhi, George Lansbury, Peter Boorman, Vincenzo Mainieri, Daniel Stern
Figure caption: Corner plot of results with (a) CABS∗ZWABS∗POW, restrictive prior on Γ (blue); (b) BNSPHERE, physically representative prior on Γ (orange), and (c) CABS∗ZWABS∗POW, fixed Γ = 1.9 (green). Best-fit values for each parameter are shown with a solid line. (Top right) L 2–10 vs. Γ contour with the IR-predicted luminosity shown (Stern 2015, dashed line)—the luminosity contours for the lightly obscured models are decisively below this level. Also shown are the results for the 12% scattered “leaky sphere”, which is closer to predicted (pink).
Paper: XMM and NuSTAR Observations of an Optically Quiescent Quasar
Authors: Claire Greenwell, Poshak Gandhi, George Lansbury, Peter Boorman, Vincenzo Mainieri, Daniel Stern
Figure caption: Spectra and ratio between data and model for (top) CABS∗ZWABS∗POW, Γ = 1.79; (middle) BNSPHERE, Γ = 1.35; (bottom) “leaky sphere”, Γ = 2.19. Shown is XMM-Newton-pn (black), XMM-Newton-MOS (red), and NuSTAR FPMA (blue), binned to a minimum of 2 counts per bin.
Paper: XMM and NuSTAR Observations of an Optically Quiescent Quasar
Authors: Claire Greenwell, Poshak Gandhi, George Lansbury, Peter Boorman, Vincenzo Mainieri, Daniel Stern
Figure caption: (left) XMM-Newton pn image; (right) PanSTARRS irg bands converted to RGB image. Green circles have a 20″ radius, and the cyan circle has a 6″ radius; all are centered on the optical source coordinates.
Paper: Third and Fourth Harmonics of Electromagnetic Emissions by a Weak Beam in a Solar Wind Plasma with Random Density Fluctuations
Authors: C. Krafft, P. Savoini
Figure caption: Inhomogeneous plasma (ΔN = 0.05) at asymptotic time ω  p  t = 7150: wave spectra in the plane (k  x , k  y ). (a) ∣E  xk ∣2 at ω  k  ≃ ω  p ;  the spectral domains of the waves ﹩{ \mathcal L }﹩ and ﹩{ \mathcal L }^{\prime\prime} ﹩ (k  x  > 0) are overlapped. (b) ∣E  xk ∣2 at ω  k  ≃ 2ω  p  with electric field contribution to ﹩{{ \mathcal H }}_{2}﹩ (central ring) and electrostatic harmonics ﹩{{ \mathcal L }}_{2}﹩ (k 2x  > 0) and ﹩{{ \mathcal L }}_{2}^{{\prime} }﹩ (﹩{k}_{2x}^{{\prime} }\lt 0﹩). (c) ∣B  zk ∣2 at ω  k  ≃ 3ω  p : wave ﹩{{ \mathcal H }}_{3}﹩. (d) ∣B  zk ∣2 at ω  k  ≃ 4ω  p : wave ﹩{{ \mathcal H }}_{4}﹩. (e) ∣E  xk ∣2 at ω  k  ≃ 3ω  p  with electric field contribution to ﹩{{ \mathcal H }}_{3}﹩ (central ring) and electrostatic harmonics ﹩{{ \mathcal L }}_{3}﹩ (k 3x  > 0) and ﹩{{ \mathcal L }}_{3}^{{\prime} }﹩ (﹩{k}_{3x}^{{\prime} }\lt 0﹩). (f) ∣E  xk ∣2 at ω  k  ≃ 4ω  p , with electric field contribution to ﹩{{ \mathcal H }}_{4}﹩ (central ring) and electrostatic harmonics ﹩{{ \mathcal L }}_{4}﹩ (k 4x  > 0) and ﹩{{ \mathcal L }}_{4}^{{\prime} }﹩ (﹩{k}_{4x}^{{\prime} }\lt 0﹩). All variables are normalized. Logarithmic scales are used.
Paper: Third and Fourth Harmonics of Electromagnetic Emissions by a Weak Beam in a Solar Wind Plasma with Random Density Fluctuations
Authors: C. Krafft, P. Savoini
Figure caption: Inhomogeneous plasma (ΔN = 0.05): time variations of wave energies (black curves) and products between them (color curves). (a)–(d): logarithmic scales; (e)–(f): linear scales. (a) Time variations of ﹩{W}_{{{ \mathcal H }}_{2}},﹩                    ﹩{W}_{{{ \mathcal H }}_{3}}﹩, and ﹩{W}_{{{ \mathcal H }}_{4}}﹩ (black). (b) Time variations of ﹩{W}_{{ \mathcal L }},﹩                    ﹩{W}_{{{ \mathcal L }}^{{\prime} }},﹩ and ﹩{W}_{{ \mathcal L }^{\prime\prime} }﹩ for ω  p  t > 4800 (black), and of ﹩{W}_{{{ \mathcal H }}_{3}}{W}_{{{ \mathcal H }}_{4}}﹩, ﹩{W}_{{{ \mathcal H }}_{2}}{W}_{{{ \mathcal H }}_{3}}﹩, and ﹩{W}_{{{ \mathcal H }}_{4}}{W}_{{{ \mathcal L }}_{3}^{{\prime} }}﹩, labeled by H 3 ∗ H 4 (green), H 2 ∗ H 3 (red), and ﹩{H}_{4}\ast {L}_{3}^{{\prime} }﹩ (orange); the green curve is duplicated to show both ﹩{W}_{{ \mathcal L }}\propto {W}_{{{ \mathcal H }}_{3}}{W}_{{{ \mathcal H }}_{4}}﹩ and ﹩{W}_{{ \mathcal L }^{\prime\prime} }\propto {W}_{{{ \mathcal H }}_{3}}{W}_{{{ \mathcal H }}_{4}}﹩. (c) Time variations of ﹩{W}_{{{ \mathcal L }}_{2}}﹩ and ﹩{W}_{{{ \mathcal L }}_{3}}﹩ (solid black), ﹩{W}_{{{ \mathcal L }}_{2}^{{\prime} }}﹩ and ﹩{W}_{{{ \mathcal L }}_{3}^{{\prime} }}﹩ (dotted black), and ﹩{W}_{{{ \mathcal H }}_{4}}{W}_{{ \mathcal L }}﹩, labeled by H 4 ∗ L (green). (d) Time variations of ﹩{W}_{{{ \mathcal H }}_{2}}﹩ (black), ﹩{W}_{{{ \mathcal H }}_{3}}{W}_{{ \mathcal L }},﹩                    ﹩{W}_{{{ \mathcal H }}_{3}}{W}_{{{ \mathcal L }}^{{\prime} }}﹩, and ﹩{W}_{{{ \mathcal H }}_{3}}{W}_{{ \mathcal L }^{\prime\prime} }﹩, labeled by H 3 ∗ L (green), ﹩{H}_{3}\ast {L}^{{\prime} }﹩ (blue), and H 3 ∗ L″ (red). (e) Time variations of ﹩{W}_{{{ \mathcal H }}_{3}}﹩ (black), ﹩{W}_{{{ \mathcal H }}_{2}}{W}_{{ \mathcal L }}﹩, ﹩{W}_{{{ \mathcal H }}_{2}}{W}_{{{ \mathcal L }}^{{\prime} }}﹩, and ﹩{W}_{{{ \mathcal H }}_{4}}{W}_{{ \mathcal L }}﹩, labeled by H 2 ∗ L (red), ﹩{H}_{2}\ast {L}^{{\prime} }﹩ (blue), and H 4 ∗ L (green); the green (red) straight line results from the linear interpolation of ﹩{W}_{{{ \mathcal H }}_{4}}{W}_{{ \mathcal L }}﹩ (﹩{W}_{{{ \mathcal H }}_{2}}{W}_{{ \mathcal L }}﹩). (f) Time variations of ﹩{W}_{{{ \mathcal H }}_{4}}﹩ (black) and ﹩{W}_{{{ \mathcal H }}_{3}}{W}_{{ \mathcal L }}﹩, interpolated by a green line labeled by H 3 ∗ L. Energies are normalized by the initial beam kinetic energy.
Paper: A Search of TESS Full-frame Images for an Optical Counterpart of the Repeating FRB 20180916B
Authors: Steven J. Tingay
Figure caption: Corrected and flattened lightcurves for the coordinates of FRB 20180916B for the three sectors of observation, as described in the text. Figure 2(a), top left, Sector 18. Figure 2(b), top right, Sector 24. Figure 2(c), bottom left, Sector 25. In each case, the blue points with error bars represent the corrected and flattened TESS lightcurves; the green dashed lines indicate the limits described in the text for 60 s, 290 s, 900 s, and 1426 s assumed transient durations, with the limit corresponding to 1426 s extended across the duration of the data. In Figure 2(b), the two vertical black dotted lines indicate the two epochs of AT2020hur discovery. The filled gray boxes indicate the FRB 20180916B activity periods. The red solid lines denote ±3σ for the flattened data.
Paper: A Search of TESS Full-frame Images for an Optical Counterpart of the Repeating FRB 20180916B
Authors: Steven J. Tingay
Figure caption: Expanded view of four days of data across two FRB activity periods during Sector 25 observations. Markers and lines have the same meanings as in Figure 2.
Paper: A Search of TESS Full-frame Images for an Optical Counterpart of the Repeating FRB 20180916B
Authors: Steven J. Tingay
Figure caption: The first frame in each sequence of FFIs (sector). From left to right, Sector 18, Sector 24, and Sector 25. The 3 × 3 pixel mask centered at the FRB 20180916B location is shown in red in the upper three panels. The mask generated to create the background lightcurve, as described in the text, for each sector is shown in red in the bottom three panels.
Paper: The Circumstellar Material around the Type IIP SN 2021yja
Authors: Alexandra Kozyreva, Jakub Klencki, Alexei V. Filippenko, Petr Baklanov, Alexey Mironov, Stephen Justham, Andrea Chiavassa
Figure caption: Bolometric, U, V, and R light curves for the models in Table 1 and in Figure 9. The colors represent the same models as in Figure 9.
Paper: XMM and NuSTAR Observations of an Optically Quiescent Quasar
Authors: Claire Greenwell, Poshak Gandhi, George Lansbury, Peter Boorman, Vincenzo Mainieri, Daniel Stern
Figure caption: A comparison between OQQ J0751+4028 and QSO2s: (left) unabsorbed 2–10 keV luminosity against 12 μm luminosity. X-ray luminosities for QSO2s are from Vignali et al. (2006) (V06; green diamonds), Vignali et al. (2010) (V10; orange diamonds), and Lamastra et al. (2009) (L09; pink diamonds). Relationships from Asmus et al. (2015, A15) and Stern (2015, S15; 12 μm luminosities were converted to 6 μm luminosities using a relationship derived from the QSO template of Hao et al. 2007) are shown as gray lines. (right) Unabsorbed 2–10 keV luminosity against [O III] luminosity, with the relationship from Lamastra et al. (2009, L09).
Paper: First Report of a Solar Energetic Particle Event Observed by China’s Tianwen-1 Mission in Transit to Mars
Authors: Shuai Fu, Zheyi Ding, Yongjie Zhang, Xiaoping Zhang, Cunhui Li, Gang Li, Shuwen Tang, Haiyan Zhang, Yi Xu, Yuming Wang, Jingnan Guo, Lingling Zhao, Yi Wang, Xiangyu Hu, Pengwei Luo, Zhiyu Sun, Yuhong Yu, Lianghai Xie
Figure caption: Locations of TW-1 (gray point), Mars (red point), Earth (blue point), STA (purple point), PSP (yellow point), and SolO (green point) at 12:00 UT on 2020 November 29 (a). The black arrow indicates the location of the active region associated with the event. The hourly averaged proton time–intensity profiles as measured by near-Earth missions (b) and TW-1/MEPA (c). The vertical dashed line indicates the onset of the flare (12:34 UT on 2020 November 29).
Paper: Radio Constraints on r-process Nucleosynthesis by Collapsars
Authors: K. H. Lee, I. Bartos, A. Eddins, A. Corsi, Z. Márka, G. C. Privon, S. Márka
Figure caption: Simulated radio lightcurve from the collapsar wind ejecta of GRB 060505 with example parameters. We considered two possible ejecta velocity profiles, “GRMHD” and “Power law” (see the legend and text), two possible values for the electron Lorentz factor power-law index p (see the legend), and two possible ejecta masses: 10−1 M ⊙ (solid) and 10−2 M ⊙ (dotted). Lightcurves are at 6  GHz. Also shown is an observational constraint obtained by VLA in 2018 (black arrow). The early first peak in the “Power law” case is due to the GRB afterglow, while in the “GRMHD” case the collapsar wind ejecta is much brighter, making the afterglow’s effect negligible.
Paper: Radio Constraints on r-process Nucleosynthesis by Collapsars
Authors: K. H. Lee, I. Bartos, A. Eddins, A. Corsi, Z. Márka, G. C. Privon, S. Márka
Figure caption: Lower limit of circumburst medium density n for which 0.1 M⊙ ejecta mass can be ruled out as a function of ϵ e and ϵ B. We show results for the “GRMHD” ejecta profile; we obtain similar results for the “Power law” ejecta profile. We show results for the electron Lorentz factor power-law index p = 2.2 (left) and p = 2.5 (right).
Paper: The ALMA REBELS Survey: The Cosmic H I Gas Mass Density in Galaxies at z ≈ 7
Authors: K. E. Heintz, P. A. Oesch, M. Aravena, R. J. Bouwens, P. Dayal, A. Ferrara, Y. Fudamoto, L. Graziani, H. Inami, L. Sommovigo, R. Smit, M. Stefanon, M. Topping, A. Pallottini, P. van der Werf
Figure caption: Redshift evolution of the cosmic H I gas mass density in galaxies, ρ HI . Measurements for this work (red squares) are based on the estimated [C II] luminosity densities at z ∼ 5 and z ∼ 7, converted to ρ HI . These results are largely dependent on the exact [C II] LF and may include significant systematic biases (see text). The blue hexagon shows the average measurement of galaxies at z ∼ 1 from stacking of the 21 cm H I signal (Chowdhury et al. 2020) and purple squares show the results from a survey of intervening 21 cm H I absorption systems covering 0 < z < 0.69 and 0.69 < z < 2.74 (Grasha et al. 2020). The DLA measurements compiled by Walter et al. (2020) are shown by the gray dots, corrected by 20% to account for the contribution to H I from sub-DLAs and Lyman-limit systems. The green curve shows the best-fit evolution of ρ HI,DLA(z) by Péroux & Howk (2020) based on DLA measurements and extrapolated beyond z ≳ 5 (shown as the dashed curve). The cyan curves show the ρ HI,tot(z) predicted by hydrodynamical simulations using various prescriptions (HM, P19, and FG20; see Maio et al. 2022 and the main text). The orange and red dashed curves show the predictions for the evolution of H I inside galaxies from the default and modified model (DM, MM) of the L-Galaxies simulations by Yates et al. (2021). The black solid line shows the combined redshift evolution of the stellar-mass density ρ ⋆(z) determined by Walter et al. (2020) and the H I gas excess M HI /M ⋆ derived in this work (see Section 3 and Figure 2), with the gray-shaded region marking the ≈ 35% uncertainty on this evolutionary curve. The approximate end of the epoch of reionization is marked at z ∼ 6.
Paper: The ALMA REBELS Survey: The Cosmic H I Gas Mass Density in Galaxies at z ≈ 7
Authors: K. E. Heintz, P. A. Oesch, M. Aravena, R. J. Bouwens, P. Dayal, A. Ferrara, Y. Fudamoto, L. Graziani, H. Inami, L. Sommovigo, R. Smit, M. Stefanon, M. Topping, A. Pallottini, P. van der Werf
Figure caption: H I gas and stellar-mass distributions of the REBELS sample galaxies at z ∼ 6.5–7.8 (red squares). The inferred H I gas and stellar masses based on the β [CII] calibration of other high-redshift galaxy samples, color-coded as a function of redshift, are shown for comparison (see text and Heintz et al. 2021 for references), in addition to the average H I gas mass excess inferred by Chowdhury et al. (2020, 2021) from a stack of the 21 cm signal from galaxies at z ≈ 1–1.3 (blue hexagons). The uncertainties on the REBELS sources are marked individually, and typical uncertainties for the other samples relying on β [CII] are shown as well. The xGASS sample represents galaxies at z ∼ 0 with direct 21 cm H I observations. Diagonal lines mark M HI /M ⋆ = 1–10.
Paper: The ALMA REBELS Survey: The Cosmic H I Gas Mass Density in Galaxies at z ≈ 7
Authors: K. E. Heintz, P. A. Oesch, M. Aravena, R. J. Bouwens, P. Dayal, A. Ferrara, Y. Fudamoto, L. Graziani, H. Inami, L. Sommovigo, R. Smit, M. Stefanon, M. Topping, A. Pallottini, P. van der Werf
Figure caption: Redshift evolution of M HI /M ⋆. The symbol notation follows Figure 1. The uncertainties on the REBELS sources (red squares) are marked individually, and typical uncertainties for the other samples relying on β [CII] are shown as well. The red- and purple-colored boxes mark vertically the 68% and 95% distributions of the REBELS and xGASS samples, respectively, and horizontally span the full redshift distribution. The average M HI /M ⋆ ratio is observed to gradually increase from z ∼ 0 to z ∼ 7, following approximately M HI /M ⋆ ∝ (1 + z)1.6±0.2 (black dashed line).
Paper: The ALMA REBELS Survey: The Cosmic H I Gas Mass Density in Galaxies at z ≈ 7
Authors: K. E. Heintz, P. A. Oesch, M. Aravena, R. J. Bouwens, P. Dayal, A. Ferrara, Y. Fudamoto, L. Graziani, H. Inami, L. Sommovigo, R. Smit, M. Stefanon, M. Topping, A. Pallottini, P. van der Werf
Figure caption: Fraction of H I in galaxies, ρ HI,ISM/ρ HI,tot, as a function of redshift. ρ HI,ISM measures the H I associated with star formation in the neutral ISM probed by [C II], whereas ρ HI,tot measures the total H I both in the ISM and the extended halos of galaxies probed by random quasar sight lines. Solid blue lines show the relative function and the dark- and light-shaded regions at the 1σ and 2σ confidence intervals. At z ≲ 2, most (≳70%) of the H I gas has accreted into galaxies.
Paper: Inefficient Growth of SiOx Grains: Implications for Circumstellar Outflows
Authors: Yuki Kimura, Kyoko K. Tanaka, Yuko Inatomi, Frank T. Ferguson, Joseph A. Nuth
Figure caption: Schematics of the experimental system. (A) Configuration and optical path of the double-wavelength, Mach–Zehnder-type laser interferometer and the nucleation chamber. The red and green lines show the optical paths of the red and green lasers, respectively. The interference fringes and real image are recorded with CMOS cameras (cam 1 and 2, respectively). The evaporation source and a sample collector are shown as the black solid (es) and dotted (sc) lines, respectively, in the nucleation chamber (n). The other labels are as follows: b, beam splitter; c, collimator; d, dichroic mirror; e, electrode; l, lens; m, mirror; o, optical fiber; p, polarizer; s, short-pass filter; v, vacuum gauge; gl, green laser; ph, pyrometer head; rl, red laser; va, valve with a gas line; vp, view port. (B) Top view in drawing by three-dimensional CAD. All optics and the chamber are on a base plate of ϕ 405 mm.
Paper: Radio Detection of an Elusive Millisecond Pulsar in the Globular Cluster NGC 6397
Authors: Lei Zhang, Alessandro Ridolfi, Harsha Blumer, Paulo C. C. Freire, Richard N. Manchester, Maura McLaughlin, Kyle Kremer, Andrew D. Cameron, Zhiyu Zhang, Jan Behrend, Marta Burgay, Sarah Buchner, David J. Champion, Weiwei Chen, Shi Dai, Yi Feng, Xiaoting Fu, Meng Guo, George Hobbs, Evan F. Keane, Michael Kramer, Lina Levin, Xiangdong Li, Mengmeng Ni, Jingshan Pan, Prajwal V. Padmanabh, Andrea Possenti, Scott M. Ransom, Chao-Wei Tsai, Vivek Venkatraman Krishnan, Pei Wang, Jie Zhang, Qijun Zhi, Yongkun Zhang, Di Li
Figure caption: (a) The discovery diagnostic plot of MSP NGC 6397B, showing the result of 1.7 hr of folded search-mode data recorded by the Parkes UWL on 2019 April 12. The white horizontal stripe indicates a portion of data excised due to radio frequency interference. (b) Timing residuals versus orbital phase for NGC 6397B. The pulsar is regularly eclipsed for 50% of the orbit around its superior conjunction (i.e., around orbital phase 0.25), and it is therefore visible only when it is on the near side of the orbit (orbital phase range 0.5–1.0).
Paper: Radio Detection of an Elusive Millisecond Pulsar in the Globular Cluster NGC 6397
Authors: Lei Zhang, Alessandro Ridolfi, Harsha Blumer, Paulo C. C. Freire, Richard N. Manchester, Maura McLaughlin, Kyle Kremer, Andrew D. Cameron, Zhiyu Zhang, Jan Behrend, Marta Burgay, Sarah Buchner, David J. Champion, Weiwei Chen, Shi Dai, Yi Feng, Xiaoting Fu, Meng Guo, George Hobbs, Evan F. Keane, Michael Kramer, Lina Levin, Xiangdong Li, Mengmeng Ni, Jingshan Pan, Prajwal V. Padmanabh, Andrea Possenti, Scott M. Ransom, Chao-Wei Tsai, Vivek Venkatraman Krishnan, Pei Wang, Jie Zhang, Qijun Zhi, Yongkun Zhang, Di Li
Figure caption: Orbital period and companion median mass of radio MSPs in GCs and the Galactic field. Pentagons: MSP with a white dwarf systems; Diamonds: MSP with a main-sequence star systems; Squares: MSP with an ultralight companion or planet mass <<0.08M⊙ systems; Small circles: Black widow systems; Middle circles: Redback systems; Big circles: Transitional pulsar (tMSP) systems.
Paper:  r-process Viable Outflows are Suppressed in Global Alpha-viscosity Models of Collapsar Disks
Authors: O. Just, M. A. Aloy, M. Obergaulinger, S. Nagataki
Figure caption: Global properties as functions of time characterizing the disk evolution, namely (a) disk mass, (b) neutrino-emission efficiency (ratio of total neutrino luminosity to accreted rest-mass energy per time), (c) minimum Y  e  within the global domain (solid lines) and within only the gravitationally unbound material (dashed lines), (d)–(f) mass-weighted averages of temperature, electron-degeneracy parameter, and Y  e , respectively, over all disk material, (g) shock radii at the equator (solid lines) and north pole (dashed lines), (h) mass (solid lines) and total energy (dashed lines) instantaneously carried by all gravitationally unbound material, as well as the time- and volume-integrated net neutrino-heating rate in regions where neutrino cooling is subdominant, (i) estimated power of a jet launched via the Blandford–Znajek process (Equation (2)). Missing data points for disk-related quantities indicate that no material fulfills the disk-definition criteria at these times.
Paper:  r-process Viable Outflows are Suppressed in Global Alpha-viscosity Models of Collapsar Disks
Authors: O. Just, M. A. Aloy, M. Obergaulinger, S. Nagataki
Figure caption: Left panel: Global properties as functions of time, namely, from top to bottom, maximum density on the computational domain, radius r in of the inner BH boundary, mass-accretion rate through the inner boundary, and mass, M BH, and spin parameter, A BH, of the central BH. The time t = 0 corresponds to the initialization of the stellar progenitor. The vertical dashed, dotted, and dotted–dashed lines mark the time of core bounce, the time when r in is moved to a radius well below the ISCO, and the disk-formation time, respectively. Right panel: Comparison between our model (black lines), which ignores the evolution of the proto-NS, and model 16TI (orange lines; Obergaulinger & Aloy 2022), which self-consistently follows the proto-NS evolution. From top to bottom, the density, electron fraction, entropy per baryon, radial mass flux, and specific angular momentum are depicted.
Paper: First Report of a Solar Energetic Particle Event Observed by China’s Tianwen-1 Mission in Transit to Mars
Authors: Shuai Fu, Zheyi Ding, Yongjie Zhang, Xiaoping Zhang, Cunhui Li, Gang Li, Shuwen Tang, Haiyan Zhang, Yi Xu, Yuming Wang, Jingnan Guo, Lingling Zhao, Yi Wang, Xiangyu Hu, Pengwei Luo, Zhiyu Sun, Yuhong Yu, Lianghai Xie
Figure caption: (a) Comparison of the SEP peak intensities between TW-1/MEPA and SOHO/ERNE (A). The scatter points are from spacecraft observations, and the curves are from a Band-function fit. (b) Calculated values of the index α (solid line) and β (dashed line). See the text for details.
Paper: First Report of a Solar Energetic Particle Event Observed by China’s Tianwen-1 Mission in Transit to Mars
Authors: Shuai Fu, Zheyi Ding, Yongjie Zhang, Xiaoping Zhang, Cunhui Li, Gang Li, Shuwen Tang, Haiyan Zhang, Yi Xu, Yuming Wang, Jingnan Guo, Lingling Zhao, Yi Wang, Xiangyu Hu, Pengwei Luo, Zhiyu Sun, Yuhong Yu, Lianghai Xie
Figure caption: Comparisons of the proton fluence spectra with a 12 hr interval increase between TW-1/MEPA (red points) and near-Earth spacecraft (blue points). The starting time for these spectra is 2020-11-30 00:03:20 UT, and the ending times are marked in each panel. The horizontal bar represents the range of each energy interval.
Paper: First Report of a Solar Energetic Particle Event Observed by China’s Tianwen-1 Mission in Transit to Mars
Authors: Shuai Fu, Zheyi Ding, Yongjie Zhang, Xiaoping Zhang, Cunhui Li, Gang Li, Shuwen Tang, Haiyan Zhang, Yi Xu, Yuming Wang, Jingnan Guo, Lingling Zhao, Yi Wang, Xiangyu Hu, Pengwei Luo, Zhiyu Sun, Yuhong Yu, Lianghai Xie
Figure caption: Comparisons of the observed proton time–intensity profiles between TW-1/MEPA and SOHO/EPHIN (a)–(c), and between TW-1/MEPA and SOHO/ERNE (d)–(f), at similar energies. The observations of TW-1 are in red, and the observations near Earth are in blue.