adsabs/AstroCLIMB huggingface dataset:
Paper: Spectroscopic Study of Heating Distributions and Mechanisms Using Hinode/EIS
Authors: Shun Ishigami, Hirohisa Hara, Takayoshi Oba
Figure caption: Top: EIS (Fe XIII 203.83 + 203.79 Å: left) and AIA (193 Å band, right) intensity images on 2012 October 20 (Loop 3). Bottom left: the enlarged view of the enclosed area by the green square in the top panels. The green arrows indicate the position of Loop 3. For our analysis, we use the intensity along the half of the loop outlined with a dashed turquoise line. One of the divided segments is marked with a solid turquoise line. Bottom right: the intensity profile across the loop and the background emission derived by the fitting shown by the red dashed line. The horizontal axis shows the number of pixels that a segment passes through in the cross-sectional direction of the loop, with a length of 40″ in this case. The data points are taken every 1″ in the direction. The bars indicate the ±1σ uncertainties resulting from the photon noise.
Paper: Spectroscopic Study of Heating Distributions and Mechanisms Using Hinode/EIS
Authors: Shun Ishigami, Hirohisa Hara, Takayoshi Oba
Figure caption: The intensity of Fe XIII (203.83 + 203.79 Å) along Loop 3 (left). The horizontal axis shows the EIS pixels through which the line tracing the loop (The green line in Figure 4) passes. The middle panel shows the intensity after dividing 10 segments and averaging in each segment. The right panel shows the intensity after the background emission is subtracted. The error bars indicate the ±1σ uncertainties resulting from the photon noise.
Paper: Spectroscopic Study of Heating Distributions and Mechanisms Using Hinode/EIS
Authors: Shun Ishigami, Hirohisa Hara, Takayoshi Oba
Figure caption: Left: emission line profiles of Fe XIII (203.83 Å), Fe XIII (203.79 Å), and Fe XII (203.73 Å). Middle: Fe XIII (202.04 Å). Right: Fe XII (196.64 Å) and Fe XIII (196.54 Å). The error bars indicate the ±1σ uncertainties resulting from the photon noise. The red lines are fitting results.
Paper: Spectroscopic Study of Heating Distributions and Mechanisms Using Hinode/EIS
Authors: Shun Ishigami, Hirohisa Hara, Takayoshi Oba
Figure caption: The electron temperature (left) and density (right) distributions of Loop 3. The error bars indicate the ±1σ errors resulting from the photon noise. The horizontal bar shows the length of the segment. The red lines are derived from the model for uniform heating. The observed loop-top temperature ﹩{T}_{\max }﹩ is used for the calculations. The origin of the horizontal axis is a height of 5 Mm from the photosphere.
Paper: Spectroscopic Study of Heating Distributions and Mechanisms Using Hinode/EIS
Authors: Shun Ishigami, Hirohisa Hara, Takayoshi Oba
Figure caption: EIS intensity images of Fe XIII (203.83 + 203.7 Å) on 2012 October 20 (Loop 3, left), 2018 August 12 (Loop 9, middle), 2015 December 25 (Loop 18, right), and the results of the fitting for measuring loop length (green lines). Enlarged views of the loops are included in the same figures as attached.
Paper: Spectroscopic Study of Heating Distributions and Mechanisms Using Hinode/EIS
Authors: Shun Ishigami, Hirohisa Hara, Takayoshi Oba
Figure caption: The theoretical variations of Fe XIII (203.83 + 203.79 Å)/Fe XIII (202.04 Å) and Fe XII (196.64 Å)/Fe XIII (196.54 Å) as functions of electron density (left) and electron temperature (right) based on CHIANTI version 10.0.1 (G. Del Zanna et al. 2021).
Paper: Cosmic-Ray Flux Correlation between MCMU and JBGO Neutron Monitors
Authors: A. Kittiya, W. Nuntiyakul, A. Seripienlert, S. Madlee, W. Sonsrettee, P. Evenson, D. Ruffolo, A. Sáiz, S. Oh, J. Jung, Q. Q. Shi, S. Wang, C. Y. Han, L. M. Zhai, K. Munakata
Figure caption: Lag offset, either for the peak offset or the cosine phase from cross correlations of the NM count rates, as a function of (a) geographic longitude difference and (b) calculated asymptotic longitude separation. The lines indicate exact equivalence, not a fit to the data. It can be seen that the peak offset closely follows the geographic longitude difference, while the cosine phase is more closely related to the asymptotic longitude.
Paper: Cosmic-Ray Flux Correlation between MCMU and JBGO Neutron Monitors
Authors: A. Kittiya, W. Nuntiyakul, A. Seripienlert, S. Madlee, W. Sonsrettee, P. Evenson, D. Ruffolo, A. Sáiz, S. Oh, J. Jung, Q. Q. Shi, S. Wang, C. Y. Han, L. M. Zhai, K. Munakata
Figure caption: Cross correlations of several station pairs. Data are shown together with fits employing constant, offset Gaussian, and phase-shifted cosine terms.
Paper: Spectroscopic Study of Heating Distributions and Mechanisms Using Hinode/EIS
Authors: Shun Ishigami, Hirohisa Hara, Takayoshi Oba
Figure caption: EIS intensity images of Fe XIII (203.83 + 203.79 Å) on 2015 December 25, (Loop 18) and the local intensity enhancement. Top right: the enlarged view of the enclosed area by the green square in the top left panel. We obtain the intensity along the half of the loop outlined with a dashed turquoise line. The green arrows show the position of Loop 18. Bottom: dividing the loop half-length into 10 segments and calculating the average intensity. The intensity along Loop 18 before (left) and after (middle) dividing 10 segments and averaging in each segment. The bars indicate the ±1σ uncertainties resulting from the photon noise.
Paper: Spectroscopic Study of Heating Distributions and Mechanisms Using Hinode/EIS
Authors: Shun Ishigami, Hirohisa Hara, Takayoshi Oba
Figure caption: The relation for E 0, B  c , and L half based on the reconnection heating model of E. N. Parker (1983). The bars indicate the 95% credible intervals of E 0 distributions. The solid lines are obtained from Equation (10).
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: Schematic illustration of the interchange slingshot. (a) The magnetospheric boundary is inside the corotation radius, and therefore a perturbation of stellar field into the disk slows down the disk material, causing it to spiral inward and erase the perturbation. (b) When the boundary lies near or outside corotation, the stellar field can accelerate the disk gas, leading it to spiral outward, enlarging the perturbation. Arc lengths show the relative magnitudes of the angular velocities of the magnetosphere (Ω*) and accretion flow (Ωdisk) at their interface. Purple arrows show the direction of the Lorentz force F L exerted by the magnetospheric perturbation on the disk, and red arrows show the resulting velocity vectors of the nearby disk material.
Paper: Modeling and Subtracting Diffuse Cluster Light in JWST Images: A Relation between the Spatial Distribution of Globular Clusters, Dwarf Galaxies, and Intracluster Light in the Lensing Cluster SMACS 0723
Authors: Nicholas S. Martis, Ghassan T. E. Sarrouh, Chris J. Willott, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Gabriel B. Brammer, Guillaume Desprez, Anishya Harshan, Adam Muzzin, Gaël Noirot, Gregor Rihtaršič, Marcin Sawicki, Victoria Strait
Figure caption: Effect of including PSF convolution in the isophote modeling process. Left: original F356W image. Center: residual after subtracting a model without PSF convolution. Right: residual after subtracting a model with PSF convolution. This process significantly reduces the area contaminated by the residual, allowing for the reliable photometry of sources closer to the MCGs’ centers.
Paper: Modeling and Subtracting Diffuse Cluster Light in JWST Images: A Relation between the Spatial Distribution of Globular Clusters, Dwarf Galaxies, and Intracluster Light in the Lensing Cluster SMACS 0723
Authors: Nicholas S. Martis, Ghassan T. E. Sarrouh, Chris J. Willott, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Gabriel B. Brammer, Guillaume Desprez, Anishya Harshan, Adam Muzzin, Gaël Noirot, Gregor Rihtaršič, Marcin Sawicki, Victoria Strait
Figure caption: Final results of our galaxy and background subtraction process. For each band we show the original image on the left, the galaxy isophote model in the center-left, cleaned image after subtracting the galaxy and background model on the center right, and a zoomed version of the cleaned image on the BCG region on the right. All images for a given filter are on the same brightness scale. NIRISS filters are indicated by the “nis” suffix.
Paper: Modeling and Subtracting Diffuse Cluster Light in JWST Images: A Relation between the Spatial Distribution of Globular Clusters, Dwarf Galaxies, and Intracluster Light in the Lensing Cluster SMACS 0723
Authors: Nicholas S. Martis, Ghassan T. E. Sarrouh, Chris J. Willott, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Gabriel B. Brammer, Guillaume Desprez, Anishya Harshan, Adam Muzzin, Gaël Noirot, Gregor Rihtaršič, Marcin Sawicki, Victoria Strait
Figure caption: Final results of our galaxy and background subtraction process shown as a composite image using all six NIRCam filters. The top left panel shows the original image, the top right the total MCG+ICL model, and the bottom the residual obtained by subtracting the model from the original image.
Paper: Modeling and Subtracting Diffuse Cluster Light in JWST Images: A Relation between the Spatial Distribution of Globular Clusters, Dwarf Galaxies, and Intracluster Light in the Lensing Cluster SMACS 0723
Authors: Nicholas S. Martis, Ghassan T. E. Sarrouh, Chris J. Willott, Roberto Abraham, Yoshihisa Asada, Maruša Bradač, Gabriel B. Brammer, Guillaume Desprez, Anishya Harshan, Adam Muzzin, Gaël Noirot, Gregor Rihtaršič, Marcin Sawicki, Victoria Strait
Figure caption: Figure 2 continued.
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Average Hubble residuals (left) and rms error of the Hubble residuals (right) of the DES-SN sample as a function of the SALT3 color c (residuals are measured without applying any bias correction, i.e., in the “BBC0D” approach). The sample is split between high and low host mass galaxies (upper panels) and between intrinsically redder (rest-frame u − r > 1) and intrinsically bluer (rest-frame u − r < 1) galaxies (lower panels). Data are presented with upper-pointing and down-pointing triangles for high- and low-mass subsamples, respectively. Simulations are presented with solid and dashed lines for high-mass/red and low-mass/blue subsamples, respectively. The models used to generate simulations are described in Section 6.2.1. Equivalent plots for low-z are shown in Figure 19.
Paper: Lyman Limit System with O VI in the Circumgalactic Environment of a Pair of Galaxies
Authors: Dheerajkumar Khonde, Purvi Udhwani, Anand Narayanan, Sowgat Muzahid, Vikram Khaire, Martin Wendt
Figure caption: The rotation curve of galaxy G1 is shown in the left panel and the velocity profiles of the H I, Si II, and O VI lines in the right panel. v = 0 km s−1 in the vertical axis corresponds to z = 0.38988, the redshift of G1. The horizontal axis in the left panel is projected galactocentric distance, and in the right panel, it is the continuum normalized flux, offset deliberately to view the absorption features created by different species clearly. The low-ionization gas, traced by Si II and the LLS component of H I, is offset from the systemic velocity of the galaxy toward the positive velocity side (see Figure 8). The line-of-sight velocity of the absorbing material (QSO line of sight, which is positioned at R ∼ +104 kpc) is thus opposite to the rotational direction of G1's disk.
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Comparison between observed and simulated correlations between SN stretch (x 1), and host galaxy properties (stellar mass on the left, and u − r rest-frame color on the right). We present results for SNe in DES-SN Shallow (upper panels) and Deep (lower panels) separately. Data (gray 2D histogram) are compared to our baseline simulation (modeling SN–host correlations using host galaxy stellar mass, P21 (M ⋆), solid contour lines). In general, we find excellent agreement between the observed and simulated distributions of the stretch as a function of different environmental variables and, when slicing the sample into bins in stellar mass or galaxy color, we find excellent agreement between the mean, standard deviation, and skewness of the simulated and observed x 1 distributions of the bin.
Paper: Lyman Limit System with O VI in the Circumgalactic Environment of a Pair of Galaxies
Authors: Dheerajkumar Khonde, Purvi Udhwani, Anand Narayanan, Sowgat Muzahid, Vikram Khaire, Martin Wendt
Figure caption: The left panel shows a flux map of galaxy G1 from the O II narrowband data cube of spatial dimensions ﹩{6}^{{\prime} ^{\prime} }\times {6}^{{\prime} ^{\prime} }﹩. The right panel shows the velocity map of this galaxy obtained from the GalPaK3D analysis. The disk-type structure of the galaxy is clear from this map. The white arrow points toward the location of the quasar sight line at a distance of 104 kpc from the center of the galaxy.
Paper: Lyman Limit System with O VI in the Circumgalactic Environment of a Pair of Galaxies
Authors: Dheerajkumar Khonde, Purvi Udhwani, Anand Narayanan, Sowgat Muzahid, Vikram Khaire, Martin Wendt
Figure caption: The horizontal axis is the velocity in the rest frame of the absorber, where v = 0 km s−1 corresponds to z = 0.39047. This system plot shows the spectra of the quasar obtained from HST/COS and Keck/HIRES, at the expected locations of a few undetected lines. The profile seen at the expected location of the line Si III 1206 is the result of contamination from O IV 787 absorption associated with the quasar and H I 918 from an absorber at z ∼0.83 (N. Tejos et al. 2014).
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Comparison between observed and simulated SN and host galaxy properties. We present the comparison both for our baseline simulation (where dust and SN–host correlations are modeled as a function of the host galaxy stellar mass, P21 (M ⋆)) and for an alternative simulation where dust and SN–host correlations are modeled as a function of the host galaxy rest-frame u − r color (P21 (u − r); see Section 4). We present results for SNe in DES-SN Shallow fields (upper panels) and Deep fields (lower panels) separately.
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Redshift distribution of the DES-SN sample compared to the Pantheon+ compilation. DES-SN is the largest and deepest sample of SN Ia to date. The dashed lines represent the different surveys’ redshift distributions contributing to the total Pantheon+ compilation. The Pantheon+ and the DES-SN samples presented in this paper have a small overlap of 146 SNe (previously published by Brout et al. 2019a).
Paper: The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties
Authors: M. Vincenzi, D. Brout, P. Armstrong, B. Popovic, G. Taylor, M. Acevedo, R. Camilleri, R. Chen, T. M. Davis, J. Lee, C. Lidman, S. R. Hinton, L. Kelsey, R. Kessler, A. Möller, H. Qu, M. Sako, B. Sanchez, D. Scolnic, M. Smith, M. Sullivan, P. Wiseman, J. Asorey, B. A. Bassett, D. Carollo, A. Carr, R. J. Foley, C. Frohmaier, L. Galbany, K. Glazebrook, O. Graur, E. Kovacs, K. Kuehn, U. Malik, R. C. Nichol, B. Rose, B. E. Tucker, M. Toy, D. L. Tucker, F. Yuan, T. M. C. Abbott, M. Aguena, O. Alves, S. S. Allam, F. Andrade-Oliveira, J. Annis, D. Bacon, K. Bechtol, G. M. Bernstein, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. E. S. Pereira, S. Desai, H. T. Diehl, P. Doel, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, M. Gatti, G. Giannini, D. Gruen, R. A. Gruendl, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, N. Kuropatkin, O. Lahav, S. Lee, H. Lin, J. L. Marshall, J. Mena-Fernández, F. Menanteau, R. Miquel, A. Palmese, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, A. Roodman, E. Sanchez, D. Sanchez Cid, M. Schubnell, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, C. To, A. R. Walker, N. Weaverdyck, M. Yamamoto
Figure caption: Overview of the paper.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: The interchange slingshot, from the 20–parallel simulation. Starting at t 0 = 23,860 r g/c, several outward spirals of magnetically dominated material from the star’s closed magnetosphere are produced over the next ∼8 spin periods. The spirals are visible in density ρ, plasma β, and magnetization σ, but are clearest in the passive scalar ﹩{ \mathcal F }﹩ that directly traces material from the force-free magnetosphere. Equatorial slices are shown, with the light cylinder and corotation radius marked in gray.
Paper: Accreting Neutron Stars in 3D General-relativistic Magnetohydrodynamic Simulations: Jets, Magnetic Polarity, and the Interchange Slingshot
Authors: Kyle Parfrey, Alexander Tchekhovskoy
Figure caption: EM and hydrodynamic contributions to the torque on the star in the μ = 5 and 10 simulations, in units of the isolated-pulsar torque N 0. The “accretion-interacting” torque is applied by all field lines that couple to the accretion flow, both inside and outside the columns. The total torque is the sum of the three components. Positive (negative) values indicate spin-up (spin-down) of the star. The μ = 5 simulations spin up consistently, while the μ = 10 runs display brief, intermittent torque reversals.
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: Left: the blue curve shows the histogram for χ N samples drawn from representative distributions consistent with the inferred results for the default spin model in R. Abbott et al. (2021b, 2023b). The black dashed lines mark the 90% credible region for the probability density of χ N distribution inferred with the ONE_COM model. Right: the credible regions for the two components inferred with the TWO_COM model. Note that the credible region for Component II is rescaled for better illustration.
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: The evolution of branching ratio (﹩{{ \mathcal F }}_{0}﹩) in the local Universe (z = 0) across total mass for the large χ N component. The gray area is the 90% region for the prior used in the inference, and the blue dashed lines show the 68% posterior credible region.
Paper: The Heavier the Faster: A Subpopulation of Heavy, Rapidly Spinning and Quickly Evolving Binary Black Holes
Authors: Wei-Hua Guo, Yin-Jie Li, Yuan-Zhu Wang, Yong Shao, Shi-Chao Wu, Tao Zhu, Yi-Zhong Fan
Figure caption: Posterior distribution of hyperparameters for the TWO_COM model as defined in Section 4. The dashed lines mark the 90% credible intervals for the marginal distributions.