adsabs/AstroCLIMB huggingface dataset:
Paper: Early TeV Photons of GRB 221009A Were Absorbed by the Prompt MeV Photons
Authors: Duan-Yuan Gao, Yuan-Chuan Zou
Figure caption: TeV light curve and the optical depth. The upper panel represents the light curve recorded by LHAASO Collaboration (2023) within the initial 7 s, which includes the energy range from 0.63 to 1 TeV. Data points with central values below 0 have been excluded as they are not suitable for calculating the optical depth. Employing a logarithmic scale, the horizontal axis denotes time, while the vertical axis signifies energy flux. The orange points denote the data points, accompanied by the error bars from LHAASO Collaboration (2023). The blue line corresponds to the linear fit undertaken by LHAASO. The blue curve reflects the luminosity of TeV photons before the γ–γ annihilation, leveraging it to determine the optical depth of the data points. This is accomplished by assessing the variance between the intermediate data points and the blue curve, as depicted in the lower panel. The lower panel delineates the temporal evolution of the optical depth. Utilizing the same horizontal axis as above, the vertical axis now represents optical depth. The blue curve shows the results derived from our model, with parameters R M = 5.5 × 1015 cm, ΓM = 100, and ΓT = 400.
Paper: Early TeV Photons of GRB 221009A Were Absorbed by the Prompt MeV Photons
Authors: Duan-Yuan Gao, Yuan-Chuan Zou
Figure caption: A schematic diagram illustrates the difference in the time delay between MeV and TeV photons caused by geometric factors, as well as the correlation among various angles. We assume that MeV photons emanate from the widest angle, denoted as θ M, where the angle between the radial direction and the photon’s trajectory is also maximized, at 1/ΓM. Conversely, we assume that TeV photons traverse the path that extends from the central engine to Earth, implying θ T = 0. Consequently, the collision angle between the TeV and MeV photons is θ. It is important to note that the MeV photons colliding with the TeV photons do not reach Earth. However, we can calculate their particle density using photons arriving at Earth at the same retarded time. In the illustration, the TeV and MeV photons share the same temporal moment, resulting in the retarded time difference being contingent upon the distance. MeV photons originate from point A; hence, their retarded time hinges on the distance to point A, d. On the contrary, TeV photons are directed toward Earth, causing their retarded time to be influenced by projection in this direction, ﹩d\cos \theta ﹩.
Paper: Discovery of a Large-scale H I Plume in the NGC 7194 Group
Authors: Mina Pak, Junhyun Baek, Joon Hyeop Lee, Aeree Chung, Matt Owers, Hyunjin Jeong, Eon-Chang Sung, Yun-Kyeong Sheen
Figure caption: (a) The DECaLS image of the NGC 7194 group. North is at the top and east is to the left. White dotted circles are the five previously known members of the group. Cyan circles are blue knots. The long arrow is drawn parallel with the long diffuse and blue stream, and the small arrows mark diffuse blue branches in the southwestern outskirts of the N7194. (b) H I distributions from VLA D-configuration is overlaid on the DECaLS image. Circle in the right-bottom corner denotes the beam size of D-configuration. The contour levels of H I column density go from 1.5 to 47.0 × 1019 cm−2 in the interval with 10 steps in linear scale. The DECaLS images (70″ × 70″) of five quiescent galaxies are shown in the bottom panel. The IDs of NSA 24868 and NSA 24889 are taken from the NASA-Sloan Atlas catalog (NSA; Blanton et al. 2011).
Paper: Early TeV Photons of GRB 221009A Were Absorbed by the Prompt MeV Photons
Authors: Duan-Yuan Gao, Yuan-Chuan Zou
Figure caption: Illustration on the impact of selecting different parameters on the optical depth. The three subplots on the left (a), center (b), and right (c), respectively, demonstrate the influence of changes in the Lorentz factor of the TeV emission region, the ratio of radius between MeV and TeV, and the Lorentz factor of the MeV emission region on the optical depth curve. The default values are ΓT = 400, f R = 0.573, and ΓM = 100, respectively. In each subplot, we show the variation of the optical depth curve when each corresponding parameter is increased or decreased by 10%. The original curve is represented by the solid orange line, the curve with parameters decreased by 10% is shown by the dashed blue line, and the curve with parameters increased by 10% is depicted by the dashed–dotted green line, respectively. The red points with error bars in the figure represent the optical depth estimated based on measurements by LHAASO in the energy range from 0.3 to infinity. It can be observed that the Lorentz factor of the TeV emission region significantly affects the peak value of the optical depth, while the other two parameters mainly influence the peak time.
Paper: Tilted Circumbinary Planetary Systems as Efficient Progenitors of Free-floating Planets
Authors: Cheng Chen, Rebecca G. Martin, Stephen H. Lubow, C. J. Nixon
Figure caption: Stability maps for planetary systems with two equal-mass circumbinary planets around a binary system with e b = 0.0 (left panels) and 0.8 (right panels). The inner planet has initial semimajor axis a p1 = 5 a b. The pixel colors are as described in Figure 1. From top to bottom panels, the two planets are Earth mass, super-Earth mass (10 times Earth mass), Neptune mass, and Saturn mass.
Paper: Early TeV Photons of GRB 221009A Were Absorbed by the Prompt MeV Photons
Authors: Duan-Yuan Gao, Yuan-Chuan Zou
Figure caption: Similar to Figure 2. The upper panel displays the light curve data recorded by LHAASO Collaboration (2023) spanning the initial 7 s, encompassing the energy range from 0.3 TeV to infinity. Using a methodology similar to Figure 2, we generated a comparable plot with the intention of introducing supplementary data points and highlighting the rapid decrease in optical depth.
Paper: Discovery of a Large-scale H I Plume in the NGC 7194 Group
Authors: Mina Pak, Junhyun Baek, Joon Hyeop Lee, Aeree Chung, Matt Owers, Hyunjin Jeong, Eon-Chang Sung, Yun-Kyeong Sheen
Figure caption: The H I intensity weighted velocity (left panel) and velocity dispersion (right panel) from VLA D-configuration. H I column density contours are overlaid with solid lines on both maps. The H I velocities increase smoothly from 7200 km s−1 in the south to 8200 km s−1 in the north.
Paper: Protoplanetary Disk Size under Nonideal Magnetohydrodynamics: A General Formalism with Inclined Magnetic Field
Authors: Yueh-Ning Lee, 悅寧 李, Barshan Ray, Pierre Marchand, Patrick Hennebelle
Figure caption: Disk size distribution for varied values of r h/r v. Misalignment angle following uniform distribution, ﹩P(i)\propto \sin (i)﹩, is plotted with solid lines, and a more aligned distribution, P(i) ∝ 1, is plotted with dashed lines.
Paper: Protoplanetary Disk Size under Nonideal Magnetohydrodynamics: A General Formalism with Inclined Magnetic Field
Authors: Yueh-Ning Lee, 悅寧 李, Barshan Ray, Pierre Marchand, Patrick Hennebelle
Figure caption: Magnetic field strength–density relation for collapsing envelope around various central stellar mass, from Equations (C7) and (C8). The gray line shows the relation from Equation (C5), which seperates different regimes of η A behaviors. The kink is due to the discontinuous expression in Equation (C6), which can be easily removed by applying some smoothing.
Paper: Protoplanetary Disk Size under Nonideal Magnetohydrodynamics: A General Formalism with Inclined Magnetic Field
Authors: Yueh-Ning Lee, 悅寧 李, Barshan Ray, Pierre Marchand, Patrick Hennebelle
Figure caption: The disk radius, divided by r v, plotted against the inclination angle i. Several values of r h/r v are shown, while 2.8 is characteristic of the common disk parameters.
Paper: Protoplanetary Disk Size under Nonideal Magnetohydrodynamics: A General Formalism with Inclined Magnetic Field
Authors: Yueh-Ning Lee, 悅寧 李, Barshan Ray, Pierre Marchand, Patrick Hennebelle
Figure caption: Disk size distribution for a complete population following IMF distribution. Blue curves correspond to a population that follows a lognormal around 0.2 M ⊙ and a power law of slope −1.35 (Chabrier 2005), and orange curves have the IMF slope changed to −0.75. Misalignment angle following uniform distribution, ﹩P(i)\propto \sin (i)﹩, is plotted with solid lines, and a more aligned distribution, P(i) ∝ 1, is plotted with dashed lines.
Paper: Protoplanetary Disk Size under Nonideal Magnetohydrodynamics: A General Formalism with Inclined Magnetic Field
Authors: Yueh-Ning Lee, 悅寧 李, Barshan Ray, Pierre Marchand, Patrick Hennebelle
Figure caption: Relative strength of the magnetic field components. Colored lines show ﹩{(r/{r}_{{\rm{v}}})}^{-5/4}﹩, which are representative of the azimuthal field strength. Solid black line shows ﹩\cos (i)﹩ (z-component) and dashed black line shows ﹩\sin (i)2/\pi ﹩ (r-component). The azimuthal field is dominant in most of the cases.
Paper: Baryon-induced Collapse of Dark Matter Cores into Supermassive Black Holes
Authors: C. R. Argüelles, J. A. Rueda, R. Ruffini
Figure caption: Dark matter+baryonic equilibrium configurations for m = 100 keV/c 2. The black dashed curve shows the equilibrium configurations at a constant total fermion number. The lighter and darker gray curves are the equilibrium sequences η = 0 and 0.8. The red curve is the secular instability limit for gravitational collapse. The black dashed sequence starts with a pure-dark-matter core (χ = 0) of M dm = 2.03 × 107 M ⊙ and radius R  c  = 6.67 × 10−5 pc, i.e., the degenerate core of the configuration shown in Figure 1. As baryons sink in the core, the configuration follows the black dashed sequence to the right (see the arrow) until it reaches the critical mass for gravitational collapse (black dot). The critical configuration has a baryon-to-dark-matter mass ratio χ BH ≈ 0.56, so baryons contribute 36% and the dark matter 64% to the critical mass, M BH ≈ 3.19 × 107 M ⊙, i.e., M dm,crit = 2.04 × 107 M ⊙ and M  b,crit ≈ 1.15 × 107 M ⊙.
Paper: Baryon-induced Collapse of Dark Matter Cores into Supermassive Black Holes
Authors: C. R. Argüelles, J. A. Rueda, R. Ruffini
Figure caption: Left: time for SMBH formation by baryon-induced collapse as a function of ﹩{\bar{Q}}_{b}﹩, for two selected examples of initial pure-dark-matter cores: M dm = 2.03 × 107 M ⊙ (blue curve) and M dm = 2.93 × 107 M ⊙ (red curve) that reach, respectively, the critical mass M BH = 3.19 × 107 M ⊙ (dot in Figure 2) and M BH = 3.98 × 107 M ⊙. The gray filled region shows the elapsed cosmological time from an initial redshift of 12 ≤ z 0 ≤ 15 to a final redshift z  f  = 10.3, relevant for the analysis of UHZ1*. Likewise, the green filled region from z 0 = 15 to 4 ≤ z 0 ≤ 6 is relevant for analyzing the so-called little red dots. Right: time evolution of the dark matter core mass while accreting baryonic matter, given by Equation (6), for the two examples in the left panel, for the values of ﹩{\bar{Q}}_{b}﹩ in the legend. The dashed lines indicate the SMBH mass formed. Details are given in Sections 3 and 4.
Paper: Baryon-induced Collapse of Dark Matter Cores into Supermassive Black Holes
Authors: C. R. Argüelles, J. A. Rueda, R. Ruffini
Figure caption: Pure-dark-matter equilibrium configuration with central density ρ = 0.0068 g cm−3 = 1.01 × 1020 M ⊙  pc−3, for a fermion m = 100 keV/c 2. The total halo mass is 5 × 1011 M ⊙. The degenerate quantum core (filled gray region) has a mass M dm = 2.03 × 107 M ⊙ and radius R  c  = 6.67 × 10−5 pc.
Paper: SuNeRF: 3D Reconstruction of the Solar EUV Corona Using Neural Radiance Fields
Authors: Robert Jarolim, Benoit Tremblay, Andrés Muñoz-Jaramillo, Kyriaki-Margarita Bintsi, Anna Jungbluth, Miraflor Santos, Angelos Vourlidas, James P. Mason, Sairam Sundaresan, Cooper Downs, Ronald M. Caplan
Figure caption: Overview of the proposed method for 3D reconstruction of the solar EUV corona. Our method consists of five steps. (1) For each pixel in the input video sequence, we sample points along the ray path ranging from −1.3 to 1.3 R ⊙. The endpoints of the rays passing through the Sun are fixed to the solar surface to account for its opaqueness. (2) The sampled points are passed through the neural network, which outputs the emission ϵ and absorption κ coefficient per point. (3) For each ray, we construct the emission and absorption along the ray. (4) The total observed intensity is then computed by integrating all sampled points, where each intensity value is reduced by absorption along the path of propagation (from the origin to the observer). (5) The predicted intensity value is then compared to the actual pixel value, which serves as a loss function for our model training. Per update step, we optimize a set of 32,768 rays. By iteratively fitting all pixel values, we obtain a complete spatial and temporal representation of the solar corona.
Paper: SuNeRF: 3D Reconstruction of the Solar EUV Corona Using Neural Radiance Fields
Authors: Robert Jarolim, Benoit Tremblay, Andrés Muñoz-Jaramillo, Kyriaki-Margarita Bintsi, Anna Jungbluth, Miraflor Santos, Angelos Vourlidas, James P. Mason, Sairam Sundaresan, Cooper Downs, Ronald M. Caplan
Figure caption: Emission profile of the solar corona as estimated by SuNeRFs. (a) Intercalibrated STEREO-A observation, where the red line indicates the analyzed slice through the solar atmosphere (fixed longitude). The blue and orange segments indicate the coronal hole and the filament channel, respectively. (b) SuNeRF-rendered view, rotated such that the atmospheric slice in (a) coincides with the limb. In the solar atmosphere above said slice, we compute the emission at each height. The 2D atmospheric profile clearly shows the bright active region close to the equator. The coronal holes (blue line and south pole) show a strong decrease in intensity. The black dashed line indicates the radial average height of channel-specific emission, which varies between 15 and 50 Mm (0.02–0.07 R ⊙). (c) Square root of the normalized integrated channel-specific emission in the analyzed slice. The emission refers to the radially outgoing total emission, which we use as a proxy for the plasma density distribution. The blue segment shows the exact coronal hole profile. The orange segment is associated with the solar filament and appears as a sharp drop in the profile (coronal cavity).
Paper: SuNeRF: 3D Reconstruction of the Solar EUV Corona Using Neural Radiance Fields
Authors: Robert Jarolim, Benoit Tremblay, Andrés Muñoz-Jaramillo, Kyriaki-Margarita Bintsi, Anna Jungbluth, Miraflor Santos, Angelos Vourlidas, James P. Mason, Sairam Sundaresan, Cooper Downs, Ronald M. Caplan
Figure caption: Comparison of synchronic maps on 2012 August 30 00:00 (UT). (a) Conventional synchronic map combining three simultaneous observations from different viewpoints using the reproject function by SunPy. (b) Adjusted synchronic map optimized for coronal hole detections (see Caplan et al. 2016). (c) SuNeRF synchronic map. Reprojected maps can result in poor alignment of features, while our SuNeRF approach consistently combines the three observations (blue circle). Reprojection effects at higher latitudes are corrected by our approach, leading to a clearer identification of the polar coronal hole boundary (green circle). Note that the resolution of our SuNeRF reconstruction is reduced as compared to the synchronic maps, which is related to the limited capacity of the neural representation. The values are given in units of DN s−1.