adsabs/AstroCLIMB huggingface dataset:
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: Summed UVOT/W1 data (highly stretched) from AOs 5 to 17. Proxima’s proper motion (47.″56) over that time interval is shown in red. Green circles (radius of 6 pixels, or 3″) mark sources that can interfere with Proxima or its background-region annuli; UVOT PSF is ∼2.″5 FWHM. Rate corrections for interference were all below 2%.
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: X-ray cycle amplitude vs. Rossby number, using values listed in Table 5. Three stars have pairs of points, reflecting uncertainty in whether the local (tachocline) or global (full convective zone) dynamo is dominant (see Z. A. Irving et al. 2023). Amplitudes for Proxima and ϵ Eri have been slightly shifted for clarity.
Paper: X-Ray, UV, and Optical Observations of Proxima Centauri’s Stellar Cycle
Authors: Bradford J. Wargelin, Steven H. Saar, Zackery A. Irving, Jonathan D. Slavin, Peter Ratzlaff, José-Dias do Nascimento
Figure caption: Floating-mean Lomb–Scargle periodogram of the full optical data set showing periodogram power vs. period. The strongest rotational peak (83.3 days) and the cycle peak (2919 days) are labeled, as is the data time span (8464 days).
Paper: The SUPERCOLD-CGM Survey. II. [C I](1–0) Emission and the Physical Conditions of Cold Gas in Enormous Lyα Nebulae at z ∼ 2
Authors: Jianan Li, Bjorn H. C. Emonts, Zheng Cai, Jianrui Li, Ran Wang, Montserrat Villar-Martín, Fabrizio Arrigoni Battaia, Mingyu Li, Yunjing Wu, Ilsang Yoon, Matthew D. Lehnert, Kyle Massingill, Craig Sarazin, Jason X Prochaska, Mark Lacy, Brian Mason
Figure caption: [C I](1–0) intensity maps for the QSOs. Color bars show the scale in the unit of Jy beam−1 × km s−1. We show the contours with a factor of 2× increase, except for the last one which we highlight the peak of the emission. Contours denote [−2, 2, 4, 8, 16, 21] × σ (σ = 0.029 Jy beam−1 × km s−1) for Q0050+0051, [−2, 2, 4, 5] × σ (σ = 0.029 Jy beam−1 × km s−1) for Q0052+0140, [−2, 2, 4, 8, 16, 18] × σ (σ = 0.018 Jy beam−1 × km s−1) for Q0101+0201, [−2, 2, 4, 8] × σ (σ = 0.032 Jy beam−1 × km s−1) for Q0107+0314, [−2, 2, 4, 5] × σ (σ = 0.036 Jy beam−1 × km s−1) for Q1227+2848, [−2, 2, 4] × σ (σ = 0.058 Jy beam−1 × km s−1) for Q1228+3128, [−2, 2, 4, 8] × σ (σ = 0.025 Jy beam−1 × km s−1) for Q1230+3320, [−2, 2, 4, 5] × σ (σ = 0.019 Jy beam−1 × km s−1) for Q1416+2649, [−2, 2, 4, 6] × σ (σ = 0.018 Jy beam−1 × km s−1) for Q2121+0052, and [−2, 2, 3.3] × σ (σ = 0.029 Jy beam−1 × km s−1) for Q2123−0050. For Q2123−0050, we also show the velocity range for generating the intensity map.
Paper: The SUPERCOLD-CGM Survey. II. [C I](1–0) Emission and the Physical Conditions of Cold Gas in Enormous Lyα Nebulae at z ∼ 2
Authors: Jianan Li, Bjorn H. C. Emonts, Zheng Cai, Jianrui Li, Ran Wang, Montserrat Villar-Martín, Fabrizio Arrigoni Battaia, Mingyu Li, Yunjing Wu, Ilsang Yoon, Matthew D. Lehnert, Kyle Massingill, Craig Sarazin, Jason X Prochaska, Mark Lacy, Brian Mason
Figure caption: [C I](1–0) intensity maps for the companion galaxies in our QSO fields. X- and Y-axes show the positions of the companion galaxies relative to the QSOs. Color bars show the line flux scale in the unit of Jy beam−1 × km s−1. Contours denote the detections of [−2, 2, 4, 5] × σ (1σ = 0.019 Jy beam−1 × km s−1) for the companion galaxy C1 in the Q0050+0051 field, [−2, 2, 3] × σ (1σ = 0.043 Jy beam−1 × km s−1) for C1 in the Q0052+0140 field, [−2, 2, 4, 8, 10] × σ (1σ = 0.025 Jy beam−1 × km s−1) for C1 in the Q1230+3320 field, [−2, 2, 3.3] × σ (1σ = 0.030 Jy beam−1 × km s−1) for C1 in the Q2123−0050 field, and [−2, 2, 4] × σ (1σ = 0.041 Jy beam−1 × km s−1) for C2 in the Q2123−0050 field. For the companion galaxies C1 and C2 of Q2123−0050, we show the velocity ranges for generating the intensity maps. We show the position of the companion galaxy C1 of Q2123−0050 as a white cross.
Paper: The SUPERCOLD-CGM Survey. II. [C I](1–0) Emission and the Physical Conditions of Cold Gas in Enormous Lyα Nebulae at z ∼ 2
Authors: Jianan Li, Bjorn H. C. Emonts, Zheng Cai, Jianrui Li, Ran Wang, Montserrat Villar-Martín, Fabrizio Arrigoni Battaia, Mingyu Li, Yunjing Wu, Ilsang Yoon, Matthew D. Lehnert, Kyle Massingill, Craig Sarazin, Jason X Prochaska, Mark Lacy, Brian Mason
Figure caption: Molecular gas masses derived based on the CO(4−3), [C I](1–0), and dust continuum emission. We use α CO = 0.8 M ☉                      ﹩{[{\rm{K}}\ \mathrm{km}\,{{\rm{s}}}^{-1}\ {\mathrm{pc}}^{2}]}^{-1}﹩, R 41 = 0.87, and X [C I] = 8.4 × 10−5 to estimate the molecular gas mass using the CO(4−3) and [C I](1–0) lines for the QSOs. We consider all the companion galaxies as either starbursts (a) or star-forming galaxies (b), and the parameters adopted are α CO = 0.8 M ☉                      ﹩{[{\rm{K}}\ \mathrm{km}\,{{\rm{s}}}^{-1}\ {\mathrm{pc}}^{2}]}^{-1}﹩, R 41 = 0.85, and X [C I] = 8.4 × 10−5 (for starbursts), and α CO = 3.6 M ☉                      ﹩{[{\rm{K}}\ \mathrm{km}\,{{\rm{s}}}^{-1}\ {\mathrm{pc}}^{2}]}^{-1}﹩, R 41 = 0.17, and X [C I] = 3.0 × 10−5 (for star-forming galaxies). For the molecular gas masses derived from the ALMA continuum, we adopt ﹩{\delta }_{\mathrm{DGR}}\,=\,\tfrac{1}{100}﹩ and T dust = 47 K (c), ﹩{\delta }_{\mathrm{DGR}}\,=\,\tfrac{1}{50}﹩ and T dust = 47 K (d), and ﹩{\delta }_{\mathrm{DGR}}\,=\,\tfrac{1}{100}﹩ and T dust = 80 K (e) for the QSOs and companions.
Paper: The SUPERCOLD-CGM Survey. II. [C I](1–0) Emission and the Physical Conditions of Cold Gas in Enormous Lyα Nebulae at z ∼ 2
Authors: Jianan Li, Bjorn H. C. Emonts, Zheng Cai, Jianrui Li, Ran Wang, Montserrat Villar-Martín, Fabrizio Arrigoni Battaia, Mingyu Li, Yunjing Wu, Ilsang Yoon, Matthew D. Lehnert, Kyle Massingill, Craig Sarazin, Jason X Prochaska, Mark Lacy, Brian Mason
Figure caption:  L CO(4−3)/L [C I](1−0) vs. L [C I](1−0)/L FIR(SF) ratios for the QSOs (red-filled diamonds), and companion galaxies (blue-filled squares), and the tentative detection of the CGM (black-filled square) in our sample. The comparison samples in the literature are the same as those presented in Figure 6. The isocontours are from the PDR models generated by the PhotoDissociation Region Toolbox adopting the “wk2000” model (M. J. Kaufman et al. 2006; M. G. Wolfire et al. 2010; D. A. Neufeld & M. G. Wolfire 2016). The pink solid contours represent the modeled [C I](1–0)/CO(4−3) luminosity ratio with different molecular hydrogen densities, and the gray dashed contours represent the modeled [C I](1–0)/L FIR(SF) ratio for different ionization parameters.
Paper: The SUPERCOLD-CGM Survey. II. [C I](1–0) Emission and the Physical Conditions of Cold Gas in Enormous Lyα Nebulae at z ∼ 2
Authors: Jianan Li, Bjorn H. C. Emonts, Zheng Cai, Jianrui Li, Ran Wang, Montserrat Villar-Martín, Fabrizio Arrigoni Battaia, Mingyu Li, Yunjing Wu, Ilsang Yoon, Matthew D. Lehnert, Kyle Massingill, Craig Sarazin, Jason X Prochaska, Mark Lacy, Brian Mason
Figure caption:  L CO(4−3)/L FIR(SF) and L [C I](1−0)/L FIR(SF) ratios for the QSOs and companion galaxies in our sample and samples of galaxies in the literature. Literature galaxy samples are local (U)LIRGs (cyan-filled circles), z = 1.1–6.4 AGN or QSOs (magenta down-triangles), z = 2.0–4.8 SMGs (orange-filled pentagons), and z = 0.8–2.2 MS galaxies (green-filled stars) from F. Valentino et al. (2020) and G. Gururajan et al. (2023). The z = 1.1–6.4 AGN or QSOs are from F. Walter et al. (2011), but only the CO (3–2) line is observed. We convert the CO(3–2) luminosity to CO (4–3) luminosity, adopting an ﹩{L}_{\mathrm{CO}(4-3)}^{{\prime} }/{L}_{\mathrm{CO}(3-2)}^{{\prime} }﹩ ratio of 0.9 typical of high-z QSOs (C. L. Carilli & F. Walter 2013). Pink dotted and gray solid lines represent linear fits to the data without and with the QSOs and companion galaxies of this work included.
Paper: The SUPERCOLD-CGM Survey. II. [C I](1–0) Emission and the Physical Conditions of Cold Gas in Enormous Lyα Nebulae at z ∼ 2
Authors: Jianan Li, Bjorn H. C. Emonts, Zheng Cai, Jianrui Li, Ran Wang, Montserrat Villar-Martín, Fabrizio Arrigoni Battaia, Mingyu Li, Yunjing Wu, Ilsang Yoon, Matthew D. Lehnert, Kyle Massingill, Craig Sarazin, Jason X Prochaska, Mark Lacy, Brian Mason
Figure caption: [C I](1–0) spectra for QSOs. Left column: the CO(4−3) (solid blue lines) and [C I](1–0) (gray histograms) spectra normalized to the peak flux densities. Red solid lines represent Gaussian profile fit to the [C I](1–0) lines. Note that the [C I](1–0) and CO(4−3) are from the 12 m array data of ALMA. Right column: the [C I](1–0) spectra obtained using 12 m array data of ALMA (gray histograms) and 7 m+12 m array data of ALMA after uv-tapering (solid black lines). Gaussian fit to the spectra extracted from the 7 m+12 m array data after uv-tapering are denoted as solid magenta lines.
Paper: The SUPERCOLD-CGM Survey. II. [C I](1–0) Emission and the Physical Conditions of Cold Gas in Enormous Lyα Nebulae at z ∼ 2
Authors: Jianan Li, Bjorn H. C. Emonts, Zheng Cai, Jianrui Li, Ran Wang, Montserrat Villar-Martín, Fabrizio Arrigoni Battaia, Mingyu Li, Yunjing Wu, Ilsang Yoon, Matthew D. Lehnert, Kyle Massingill, Craig Sarazin, Jason X Prochaska, Mark Lacy, Brian Mason
Figure caption:                         Similar to Figure 3 (left column) but showing the [C I](1–0) spectra for the companion galaxies in the QSO fields. For the companion galaxy C1 in the Q0050+0051 field, we also show the [C I](1–0) spectrum after uv-tapering.
Paper: The SUPERCOLD-CGM Survey. II. [C I](1–0) Emission and the Physical Conditions of Cold Gas in Enormous Lyα Nebulae at z ∼ 2
Authors: Jianan Li, Bjorn H. C. Emonts, Zheng Cai, Jianrui Li, Ran Wang, Montserrat Villar-Martín, Fabrizio Arrigoni Battaia, Mingyu Li, Yunjing Wu, Ilsang Yoon, Matthew D. Lehnert, Kyle Massingill, Craig Sarazin, Jason X Prochaska, Mark Lacy, Brian Mason
Figure caption: A comparison between the [C I](1–0) flux measured from the 12 m array data (S  ν  d ν [C I]) and the 7 m+12 m array data after uv-tapering (﹩{S}_{\nu }d{\nu }_{[{\rm{C}}\ {\rm{I}}]}^{{\rm{taper}}}﹩). The red-filled squares represent the measured [C I](1–0) fluxes, and the S  ν  d ν [C I] = ﹩{S}_{\nu }d{\nu }_{[{\rm{C}}\ {\rm{I}}]}^{{\rm{taper}}}﹩ relation is shown as a solid black line.
Paper: The SUPERCOLD-CGM Survey. II. [C I](1–0) Emission and the Physical Conditions of Cold Gas in Enormous Lyα Nebulae at z ∼ 2
Authors: Jianan Li, Bjorn H. C. Emonts, Zheng Cai, Jianrui Li, Ran Wang, Montserrat Villar-Martín, Fabrizio Arrigoni Battaia, Mingyu Li, Yunjing Wu, Ilsang Yoon, Matthew D. Lehnert, Kyle Massingill, Craig Sarazin, Jason X Prochaska, Mark Lacy, Brian Mason
Figure caption: A comparison between the [C I](1–0) source sizes convolved with the beam and the beam sizes for the 12 m array data. The red-filled squares represent the sizes of the major axis, and the blue-filled diamonds represent the sizes of the minor axis. We show the source size equal to the beam size as a solid black line. We highlight the source with significant CGM emission (Q0050+0051) in magenta circles.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: PDs and PAs as functions of time T for Model I1 at ν opt (optical, purple line) and ν radio (radio, orange line) during T = 0.1–4.0 days. The top and bottom panels represent the PD curves and the PA curves, respectively. (Left) PDs and PAs are calculated with one realization set of random numbers for the turbulence creation. (Right) Averaged PDs and PAs (the purple square for ν opt and the orange circle for ν radio) and the standard deviations (the error bars) for 100 realization sets.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Local PA ϕ  p  and the normalized polarized intensity PI  ν  in Models I1 (top) and A1 (bottom). The direction and length of each of the thin black bars indicate ϕ  p  and the value of normalized PI  ν  at the EATS with θ = 1/γ  l  (left) and θ = 0.4/γ  l  (right). The jet axis marked with a black plus symbol and the line of sight is marked with an orange plus symbol. We show just for reference the thin black bars outside the jet (thick black circle) from which no emission comes.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Dependence of the PA flip ratio on ξ 2. The orange, gray, and black marks represent the flip ratios in the large-scale field model with f  B  = 1.0 for different criteria of flip. The horizontal solid orange line and blue dashed line show the flip ratio in the microscopic-scale field model with uniform jets and that with structured jets, respectively, for which the PDs are always 0% if ξ 2 = 1.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Dependence of the optical PD at T = 1.3  days on ξ 2. The orange marks show the averaged PDs over 100 turbulent realizations and their variances in the large-scale turbulence model with f  B  = 1.0. The blue marks show PDs in the microscopic turbulence model with uniform jets.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Same as Figure 3, but for Model A1.
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Schematic diagram of the blast wave and the xy plane. (Left) The thick black solid sector represents the collimated blast wave with the opening angle of 2θ j. The solid orange line in the egg-like shape represents the emission region, which has the same arrival time T in the thin shell approximation (i.e., EATS). (Right) The projected plane transverse to the line of sight (z-axis). The transformation from the coordinate (x, y) to ﹩({\tilde{x}}_{n},{\tilde{y}}_{n})﹩ is described by Equation (3).
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Light curves at frequencies 1015 Hz (optical, purple line) and 100 GHz (radio, orange line). The solid line corresponds to the on-axis observer (models I1 and A1), and the dashed line corresponds to the off-axis observer (models I2 and A2).
Paper: Large-scale Magnetic Field Model of GRB Afterglow Polarization: Effects of Field Anisotropy, Off-axis Viewing Angle, and Ordered Field
Authors: Asuka Kuwata, Kenji Toma, Sara Tomita, Jiro Shimoda
Figure caption: Same as Figure 3, but for Model I2.
Paper: Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection
Authors: Sripan Mondal, Abhishekh Kumar Srivastava, David I. Pontin, Eric R. Priest, R. Y. Kwon, Ding Yuan
Figure caption: Three slits, s1,s2, and s3, are taken in three different directions to capture the dynamics of fronts. The orientations of the slits are shown in panel (a). Distance–time diagrams in density show slanted features, which are signatures of outwardly propagating waves (see the top panels of panels (b), (c), and (d)). The estimated propagation speeds are consistent with the characteristic fast-mode speed shown in Figure 4. The perturbations in thermal pressure (P  T ) and magnetic pressure (P  M ) exhibited in the bottom panels of panels (b), (c), and (d) are in phase with one another, which also confirms the fast-mode nature of the waves. The profiles are measured at a distance 60 Mm along slits s1, s2, and s3 (corresponding to locations I, II, and III) starting from 1587 s, as shown by horizontal dotted lines. The small-scale fluctuations in thermal and magnetic pressure are extracted by subtracting the long-term background trends shown as red and blue-dotted curves.
Paper: Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection
Authors: Sripan Mondal, Abhishekh Kumar Srivastava, David I. Pontin, Eric R. Priest, R. Y. Kwon, Ding Yuan
Figure caption: Panels (a), (c), and (e) exhibit the temporal variation of the inclination of the magnetic field to the positive x-direction at locations I, II, and III, respectively. Panels (b), (d), and (f) plot the local sound speed (c  S ) (dotted curves), Alfvén speed (v A) (dashed curves), the fast-mode speed (V  f,⊥) perpendicular to the magnetic field (solid black curves), and the fast-mode speed (V  f,θ ) along the slits at locations I, II, and III. At location II on slit s2, the direction of propagation is almost perpendicular to the magnetic field, and so the black solid curve is almost the same as the red solid curve in panel (d) (V  f,θ  ≈ V  f,⊥).
Paper: Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection
Authors: Sripan Mondal, Abhishekh Kumar Srivastava, David I. Pontin, Eric R. Priest, R. Y. Kwon, Ding Yuan
Figure caption: Panels (a), (c), and (e) exhibit the temporal variation of WEDs estimated using Equation (13) at locations I, II, and III, respectively, while panels (b), (d), and (f) give the corresponding WEFs using Equation (14). The dashed curves show the profiles of magnetic energy, whereas the dotted curves show the profiles of kinetic energy. Solid curves denote the resultant wave energy quantities. The values of magnetic and kinetic energies are highly time dependent. The shaded time windows in panels (a), (c), and (e) basically correspond to different coalescence events, as discussed in Section 3.3.1.
Paper: Generation of Fast Magnetoacoustic Waves in the Corona by Impulsive Bursty Reconnection
Authors: Sripan Mondal, Abhishekh Kumar Srivastava, David I. Pontin, Eric R. Priest, R. Y. Kwon, Ding Yuan
Figure caption: The fluctuations in density and v  y  are obtained by subtracting the long-term background trends from the original profiles at locations I, II, and III in Figure 3(a). Panels (a), (c), and (e) show the time series of fluctuations in density and their corresponding wavelet distributions, which exhibit dominant periods of 59.06, 70.23, and 91.08 s at locations I, II, and III, respectively. Panels (b), (d), and (f) show similar characteristics for v  y . In all of these figures, 0 s on the time axis stands for 1587 s, which is the same starting time as in the bottom panels of panels (b), (c), and (d) of Figure 3. The unique randomization technique (A. F. Linnell Nemec & J. M. Nemec 1985; E. O’Shea et al. 2001) estimates the significance levels of oscillations between 93.5% and 99.5%. Similar characteristics for B  x  are explicitly discussed in Appendix D.
Paper: On the Possible Mechanisms of the SEP Event and Electron Enhancement over the SEP Decay Phase on 2023 August 5
Authors: Kazi A. Firoz, Y. P. Li, W. Q. Gan
Figure caption: Temporal profiles of 5 minute resolution data plotted for 01:00 UT 2023 August 5 to 17:55 UT 2023 August 6. (a)–(b) Solar proton fluxes (cm−2 sr−1 s−1) of the energies 12 MeV through 99 MeV and electron fluxes (cm−2 sr−1 s−1) of the energies 53 keV through 315 keV smoothed earlier in Figures 1–2, (c) radio dynamic spectra (SWAVES; kHz) of STEREO-A (left y-axis) overplotted with the SXR flare component (1–8 Å) of GOES-16 (right y-axis), and (d) CME heights (R ⊙) recorded by SOHO/LASCO. In (c), the oblique black arrows indicate the M1.6 and X1.6 flare peaks. In (d), the vertical black arrow indicates the onset of m-type II burst, and the vertical red arrow indicates the onset of DH-type II burst. The solid, dashed, dashed–dotted, and dotted lines indicate the PAs of the CMEs, while the red and blue colors indicate the west and east, respectively. In (a)–(d), the two orange vertical lines mark the M1.6 and X1.6 flare peaks.
Paper: Cosmic Censorship in Sgr A* and M87*: Observationally Excluding Naked Singularities
Authors: Avery E. Broderick, Kiana Salehi
Figure caption: Effective potentials for three representative cases of the 4D EGBQ naked singularity with comparisons to the astrophysically relevant range of energies for accreting particles. Shown are ﹩{V}_{\mathrm{eff}}^{t}﹩ for orbits with ﹩{\ell }=\sqrt{12}M﹩ in a black hole spacetime with γ = 0.8 and Q = 0.2 (dark red), with the radius of the horizon marked by the black point and the potential shown by a dotted line inside; orbits with ℓ given by that at the outermost innermost stable circular orbit (ISCO, light blue dot) in a naked singularity spacetime (γ = 1 and Q = 0.2, light blue); and orbits with ℓ = 0 in a naked singularity spacetime (γ = 1 and Q = 1, dark blue). For comparison, in green the values of e 2 at the ISCO of the first singular spacetime (dashed) and e 2 = 1 (solid) are indicated. While all examples have singularities at r * > 0, only in the last case is the singularity visible in the plotted range (large dark blue point).
Paper: Cosmic Censorship in Sgr A* and M87*: Observationally Excluding Naked Singularities
Authors: Avery E. Broderick, Kiana Salehi
Figure caption: Spectral energy density of M87* from a structured, nonthermal synchrotron-emitting region (black dotted) and a thermal bump due to an optically thick settling flow (red) for ﹩\dot{M}﹩ ranging from 10−3 M ⊙ yr−1 to 10−1 M ⊙ yr−1. For comparison, the 2017 EHT 230 GHz (1.3 mm) compact flux estimate (open blue square; M87* Paper VI), contemporaneous broadband SED (open black points; EHT MWL Science Working Group et al. 2021), and historical NIR–optical–UV fluxes from A. E. Broderick et al. (2015; gray closed points) are shown.
Paper: Cosmic Censorship in Sgr A* and M87*: Observationally Excluding Naked Singularities
Authors: Avery E. Broderick, Kiana Salehi
Figure caption: SED of Sgr A* from a radially structured, nonthermal synchrotron-emitting region (black dotted) and a thermal bump due to an optically thick settling flow (red) for ﹩\dot{M}﹩ ranging from 10−9 M ⊙ yr−1 to 10−7 M ⊙ yr−1. For comparison, the 2017 EHT 230 GHz (1.3 mm) compact flux estimate (open blue square; M. Wielgus et al. 2022), contemporaneous broadband SED (open black points; Sgr A* Paper II), and historical NIR upper limits from A. E. Broderick et al. (2009b) on the quiescent flux (gray closed points) are shown.
Paper: On the Possible Mechanisms of the SEP Event and Electron Enhancement over the SEP Decay Phase on 2023 August 5
Authors: Kazi A. Firoz, Y. P. Li, W. Q. Gan
Figure caption: Plotted for the duration of 21:00–∼23:59 UT on 2023 August 5 are the (a) solar radio spectrograph (25–180 MHz) from the KP solar radio observatory and (b) the sfu from NoRP; (c) SXR (W m−2) of λ ∼ 1–8 Å from GOES/NASA and the derivative of SXR (d(SXR)/dt) (W m−2 s−1), and (d) HXR bursts for 25–50 keV from HXI/ASO-S and Fermi/NASA and 19–79 keV from Konus-Wind.
Paper: Cosmic Censorship in Sgr A* and M87*: Observationally Excluding Naked Singularities
Authors: Avery E. Broderick, Kiana Salehi
Figure caption: Null (dotted) and time-like (solid) effective potentials for Schwarzschild (dark red) and Reissner–Nordström (blue) spacetimes for Q = 1.01M and ﹩{\ell }=0.5\sqrt{27}﹩. The trajectory for an infalling particle with e = m at infinity is shown schematically in green, including the reflection at the inner turning point (open point), associated accretion shock when the outgoing and infalling flows collide, and the ultimate settling flow (dashed) depositing material at the potential minimum (solid point).