adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring One-point Statistics in HERA Phase I Data: Effects of Foregrounds and Systematics on Measuring One-point Statistics
Authors: Honggeun Kim, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Kai-Feng Chen, Zhilei Xu, Eleanor Rath, Vincent MacKay, Tyrone Adams, James E. Aguirre, Rushelle Baartman, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, David R. DeBoer, Eloy de Lera Acedo, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Nicolas Fagnoni, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Bryna J. Hazelton, Jack Hickish, Daniel C. Jacobs, Joshua Kerrigan, Piyanat Kittiwisit, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, David H. E. MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Miguel F. Morales, Tshegofalang Mosiane, Steven G. Murray, Hans Nuwegeld, Aaron R. Parsons, Nima Razavi-Ghods, James Robnett, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter van Wyngaarden, Haoxuan Zheng
Figure caption: Normalized likelihood for m2, marginalized over systematics defined in Equation (21). We present the normalized likelihood for each field for Band 1 (top) and Band 2 (bottom), using all observational data points shown in Figure 14. The black solid line is the likelihood considering all data points across all fields. To see the impact of systematics mitigation, we provide the likelihood without the mitigation, based on all fields (gray dashed line). We assume the variance model of m2 ∝ ν0. The cold reionization model has m2 about 0.07 mK2 on average in Band 2, which implies the model is likely to be rejected by the likelihood analysis.
Paper: Exploring One-point Statistics in HERA Phase I Data: Effects of Foregrounds and Systematics on Measuring One-point Statistics
Authors: Honggeun Kim, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Kai-Feng Chen, Zhilei Xu, Eleanor Rath, Vincent MacKay, Tyrone Adams, James E. Aguirre, Rushelle Baartman, Adam P. Beardsley, Gianni Bernardi, Tashalee S. Billings, Judd D. Bowman, Richard F. Bradley, Philip Bull, Jacob Burba, Steven Carey, Chris L. Carilli, David R. DeBoer, Eloy de Lera Acedo, Matt Dexter, Nico Eksteen, John Ely, Aaron Ewall-Wice, Nicolas Fagnoni, Steven R. Furlanetto, Kingsley Gale-Sides, Brian Glendenning, Deepthi Gorthi, Bradley Greig, Jasper Grobbelaar, Ziyaad Halday, Bryna J. Hazelton, Jack Hickish, Daniel C. Jacobs, Joshua Kerrigan, Piyanat Kittiwisit, Matthew Kolopanis, Adam Lanman, Paul La Plante, Adrian Liu, David H. E. MacMahon, Lourence Malan, Cresshim Malgas, Keith Malgas, Bradley Marero, Zachary E. Martinot, Andrei Mesinger, Mathakane Molewa, Miguel F. Morales, Tshegofalang Mosiane, Steven G. Murray, Hans Nuwegeld, Aaron R. Parsons, Nima Razavi-Ghods, James Robnett, Peter Sims, Craig Smith, Hilton Swarts, Nithyanandan Thyagarajan, Pieter van Wyngaarden, Haoxuan Zheng
Figure caption: Predictions of S/N for m2 (top), m3 (middle), and S3 (bottom) measurements assuming 300 night observations, as forecasted with HERA-320 using the fiducial EoR model. We present the S/N considering different foreground removal methods including no foreground (i.e., perfect foreground removal) and wedge removal, represented by blue and red lines, respectively. In addition, we illustrate the case when considering the sample variance only (dashed lines) and the thermal noise and sample variance added in quadrature (solid lines). For the case when accounting for thermal noise and wedge-filtering (red solid line), the total S/N of m3 in Band 1 and Band 2 are around 1.0 and 0.6, respectively.
Paper: Determining the 3D Dynamics of Solar Flare Magnetic Reconnection
Authors: Joel T. Dahlin, Spiro K. Antiochos, Peter F. Wyper, Jiong Qiu, C. Richard DeVore
Figure caption: Initial configuration and driver for the eruptive flare model. (a)–(b) Magnetic topology shown from two orthogonal perspectives: (a) east and (b) above. White (black) shading at the inner boundary corresponds to positive (negative) polarity. Four distinct flux regions are indicated in cyan, green, and red (northern and southern sets of green field lines represent distinct flux regions). (c) Illustration of initial solar surface grid (shown at half resolution for clarity) and coordinate system. Green, red, and blue curves indicate the radial, polar (θ)/latitude and azimuth (ϕ)/longitude coordinates, respectively, with arrows indicating their directions of increase. The polarity inversion lines (PILs) are indicated in yellow, with the oval PIL encircling the active region extending approximately ±34° in longitude and ±22° in latitude. (d) Profile of Bϕ component of the tangential flux injected by the STITCH method (see the text for details) at the inner boundary. Contours of the radial component of the magnetic field are overlaid in grayscale.
Paper: FEAST: JWST Uncovers the Emerging Timescales of Young Star Clusters in M83
Authors: Alice Knutas, Angela Adamo, Alex Pedrini, Sean T. Linden, Varun Bajaj, Jenna E. Ryon, Benjamin Gregg, Ahmad A. Ali, Eric P. Andersson, Arjan Bik, Giacomo Bortolini, Anne S. M. Buckner, Daniela Calzetti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey Johnson, Thomas S.-Y. Lai, Drew Lapeer, Matteo Messa, Göran Östlin, Elena Sabbi, Linda J. Smith, Monica Tosi
Figure caption: Top left: U−B (F336W–F438W) against the V−I (F547M or F555W−F814W) together with the Yggdrasil SPP model (black solid line). The gray distribution illustrates the entire optical YSC population after visual inspection, while the dots show all the YSCs within the FOV (see Table 1) color coded by the best-fitted ages. The blue square shows the median colors of oYSCs (≤10 Myr) within the NIRCam FOV and photometric error less than 0.2 mag in F150W, F115W, F187N, F200W, F300M, F335M, and F444W. The NIR color–color diagrams in the upper-right, lower-left, and lower-right corners illustrate the eYSCI (red-orange triangles and red distributions), eYSCII (orange-yellow squares and yellow distributions), 3.3 μm PAH peaks (green stars and green distributions), F200W-extracted sources (gray circles), eYSC-BB (purple squares), oYSCs (as defined above, blue circle and blue distributions) together with the Yggdrasil SPP model (black solid lines), MAPPINGS III-H II (light-gray), and MAPPINGS III-PDR+H II models (dark-gray solid lines). Top right: the F150W−F200W against the F200W−F335M. The box displays the color–color selection for embedded clusters from S. T. Linden et al. (2023). Lower left: the F300M−F444W against the F300M−F335M color. Lower right: the F200W−F444W against the F115W−F187N color together with dashed and dotted lines to illustrate the color space of YSOs. The distributions are contours with levels at 16%, 50%, and 84% percentiles. The gray contour in the top-left plot shows the 95% percentile of the total cluster candidates after visual inspection.
Paper: FEAST: JWST Uncovers the Emerging Timescales of Young Star Clusters in M83
Authors: Alice Knutas, Angela Adamo, Alex Pedrini, Sean T. Linden, Varun Bajaj, Jenna E. Ryon, Benjamin Gregg, Ahmad A. Ali, Eric P. Andersson, Arjan Bik, Giacomo Bortolini, Anne S. M. Buckner, Daniela Calzetti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey Johnson, Thomas S.-Y. Lai, Drew Lapeer, Matteo Messa, Göran Östlin, Elena Sabbi, Linda J. Smith, Monica Tosi
Figure caption: The stellar age (left), stellar attenuation (middle), and stellar mass distribution (right) for the different classes, eYSCI (red), eYSCII (orange), and 3.3 μm PAH peaks (green) including the oYSCs (≤10 Myr; cyan) derived with CIGALE. The vertical lines correspond to the median values of eYSCI (red), eYSCII (orange), 3.3 μm PAH peaks (green), and the optical YSCs (≤10 Myr; cyan). The mass distribution (right) also includes a gray dashed line corresponding to the mass cut at 103 M⊙ and the black curve to the 10-logarithm of a cluster mass function (CMF) with a slope of −2. For the stellar age (left panel), the eYSCI median overlaps with the eYSCII.
Paper: FEAST: JWST Uncovers the Emerging Timescales of Young Star Clusters in M83
Authors: Alice Knutas, Angela Adamo, Alex Pedrini, Sean T. Linden, Varun Bajaj, Jenna E. Ryon, Benjamin Gregg, Ahmad A. Ali, Eric P. Andersson, Arjan Bik, Giacomo Bortolini, Anne S. M. Buckner, Daniela Calzetti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey Johnson, Thomas S.-Y. Lai, Drew Lapeer, Matteo Messa, Göran Östlin, Elena Sabbi, Linda J. Smith, Monica Tosi
Figure caption: Physical properties of the combined cluster sample younger than 10 Myr. On the left, we show the age–mass distributions. The total visual extinction (AV) is plotted against the stellar mass (middle) and age (right). We can observe the eYSCI (orange triangles), eYSCII (yellow squares), and YSCs (≤ 10 Myr; blue circles). Large symbols show the median AV for the eYSCI, eYSCII, and YSCs (≤ 10 Myr) separately and combined (gray dots). In the middle plot, we use 103−5 × 103 and > 5 × 103 M⊙ mass bins to estimate median AV. The dashed lines correspond to the detection limits for the maximum AV as a function of stellar mass for star clusters with an age of 1 Myr (blue) and 4 Myr (green) estimated using Yggdrasil models. In the right plot, we estimate the median AV in age bins 1−3, 3−6, and 6−10 Myr after the mass cut, to mitigate the effect of stochastic sampling in the age derivation. The gray areas highlight star clusters with mass below 1000 M⊙.
Paper: FEAST: JWST Uncovers the Emerging Timescales of Young Star Clusters in M83
Authors: Alice Knutas, Angela Adamo, Alex Pedrini, Sean T. Linden, Varun Bajaj, Jenna E. Ryon, Benjamin Gregg, Ahmad A. Ali, Eric P. Andersson, Arjan Bik, Giacomo Bortolini, Anne S. M. Buckner, Daniela Calzetti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey Johnson, Thomas S.-Y. Lai, Drew Lapeer, Matteo Messa, Göran Östlin, Elena Sabbi, Linda J. Smith, Monica Tosi
Figure caption: The mass (top) and age (bottom) distributions of the combined eYSCI and eYSCII sample (left) and oYSCs (right) as a function of different galactic environments selected to encompass different dynamical regions of the galaxy: center (yellow); bar (teal); end of the bar (purple); outer regions (gray). The turnover in the mass distributions is due to incompleteness. The vertical lines in the bottom plot show the median ages in each region.
Paper: FEAST: JWST Uncovers the Emerging Timescales of Young Star Clusters in M83
Authors: Alice Knutas, Angela Adamo, Alex Pedrini, Sean T. Linden, Varun Bajaj, Jenna E. Ryon, Benjamin Gregg, Ahmad A. Ali, Eric P. Andersson, Arjan Bik, Giacomo Bortolini, Anne S. M. Buckner, Daniela Calzetti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey Johnson, Thomas S.-Y. Lai, Drew Lapeer, Matteo Messa, Göran Östlin, Elena Sabbi, Linda J. Smith, Monica Tosi
Figure caption: The stellar age (left), stellar attenuation (middle), and stellar mass distribution (right) for the different classes, eYSCI (red), eYSCII (orange), and 3.3 μm PAH peaks (green) including the oYSCs (≤10 Myr; cyan) for the HST FOV. The vertical lines correspond to the median values of eYSCI (red), eYSCII (orange), 3.3 μm PAH peaks (green), and the YSCs (≤10 Myr; cyan). The mass distribution (left) also includes a gray dashed line corresponding to the mass cut at 1 × 103 M⊙ and the black curve to the 10-logarithm of a cluster mass function (CMF) with a slope of −2. For the stellar age (left panel), the eYSCI median overlaps with the eYSCII and YSCs (≤10 Myr).
Paper: FEAST: JWST Uncovers the Emerging Timescales of Young Star Clusters in M83
Authors: Alice Knutas, Angela Adamo, Alex Pedrini, Sean T. Linden, Varun Bajaj, Jenna E. Ryon, Benjamin Gregg, Ahmad A. Ali, Eric P. Andersson, Arjan Bik, Giacomo Bortolini, Anne S. M. Buckner, Daniela Calzetti, Ana Duarte-Cabral, Bruce G. Elmegreen, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Kelsey Johnson, Thomas S.-Y. Lai, Drew Lapeer, Matteo Messa, Göran Östlin, Elena Sabbi, Linda J. Smith, Monica Tosi
Figure caption: The mass (top) and age (bottom) distributions of the combined eYSCI and eYSCII sample (left) and oYSCs (right) in bins containing the same number of eYSCs and oYSCs combined. The central starburst region has been removed. This alternative division is less sensitive to changes in SFR due to different dynamical properties. The turnover in the mass distributions is due to incompleteness. The vertical lines in the bottom plot show the median ages in each region.
Paper: The Hot Inner AU of V883 Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Ágnes Kóspál
Figure caption: V883 Ori as seen in the Pan-STARRS g − z color image. The green ellipse shows the projected shape of the disk on the sky (scaled ×12 for visibility), assuming an inclination of 38﹩\mathop{.}\limits^{\unicode{x000b0}}﹩3 and a position angle of 32﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4 (L. A. Cieza et al. 2018). The green arrow shows the axis of rotation of the disk (J.-E. Lee et al. 2019). The position angle and inclination of the disk indicate it is the primary illumination source for the bright nebula that extends ∼70″ to the southeast. The nebula is known as IC 430.
Paper: The Hot Inner AU of V883 Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Ágnes Kóspál
Figure caption: The reddest several orders of the 2003 (orange) and 2011 (blue) Keck/HIRES spectra, where the signal-to-noise is suitable, plotted along with the disk model described in Section 3 (black). The model reproduces the weak absorption features well, but misses portions of several H I and Ca II profiles that arise in winds. Strong telluric features are present at the reddest wavelengths shown and are marked by gray vertical lines.
Paper: The Hot Inner AU of V883 Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Ágnes Kóspál
Figure caption: Select orders from the 2023 Keck/NIRSPEC spectrum (magenta) compared with the disk model described in Section 3 (black). The model matches the majority of the absorption features accurately from 1.0 μ to 2.3 μm. Gray vertical bands mark regions of strong telluric absorption.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: The distribution of accretion parameters relative to steady state derived from the posteriors of the MCMC tests, separated based on the dominant atmospheric species. To compare accretion phases, we have recast τd as tSS according to Equation (2). Solutions to the left of the vertical line correspond with the mass-buildup phase, while the right is generally the mass-settling phase for the He-WDs and typically samples the steady state for H-WDs. Most of the individual white dwarfs peak around steady state and have broad distributions. “Weighted” refers to applying a likelihood function that prefers solutions that maximize the mass of pollution in the atmosphere. “Restricted τd” curves place a restricted prior on the disk lifetime of 104–107 yr, while nonrestricted curves allow τd to vary freely between 10−6 and 1010 yr. Applying a weighted likelihood function to prefer solutions that maximize the mass currently in the atmosphere of the white dwarf tends to bring solutions toward the steady state and mass-buildup phases. H-WDs tend to peak at relatively later accretion parameters than He-WDs, but for relevant settling timescales still easily reside in the steady state.
Paper: The Cygnus X-1 Puzzle: Implications of X-Ray Polarization Measurements in the Soft and Hard States on the Properties of the Accretion Flow and the Emission Mechanisms
Authors: Henric Krawczynski, Kun Hu
Figure caption: We propose to explain the soft state emission from Cyg X-1 with a new model in which the geometrically thin, optically thick accretion disk is covered with a layer of mildly relativistically moving pair plasma. This figure shows the result from simple radiation transport simulations showing the spectral energy distribution (SED, top) and Stokes Q energy spectrum (bottom) for models with different bulk flow velocities β in units of speed of light. The purple line is for β = 0, the green line is for constant β = 0.36, and the red line is for the β-profile of Figure 3 in AB98 with β varying from 0.36 to 0.705 along the flow. The SEDs have been normalized to 1 at their peak. Positive Q-values correspond to a PA parallel to the surface of the atmosphere and negative Q-values correspond to a PA parallel to the surface normal.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: The summed water mass fraction distribution for the WDs from the “Original” MCMC test for the H and He WD samples, under the assumption of chondritic parent bodies, compared to the buildup (He WDs) and steady state (H WDs) results. For clarity, we do not show the results from additional MCMC tests; these results are listed in Table 5 and are typically indistinguishable from the “Original” curve. Distributions of water mass fractions of meteorites and solar system moons are shown as the two shaded regions. The distribution of meteorites is largely water-poor, while the distribution of solar system moons is more water-rich (see Section 5.2).
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: The distribution of inferred observation times relative to steady state (tSS, calculated from τd and the median settling time through Equation (2)) for two example WDs, derived from the posteriors of the MCMC test that uses a standard likelihood function and no strong prior on the disk lifetime (the “Original” likelihood function). Solutions to the left of the vertical line correspond with the mass-buildup phase (light shaded region) while the right (darker shaded region) is generally the mass-settling phase for the He-WDs and typically samples the steady state for H-WDs. The median of each WD’s distribution is shown as the vertical dashed line. Most WDs have a broad distribution with a peak around the steady state.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: The distributions of water mass fractions derived for two example WDs, based on the observed abundances and the accretion parameter posteriors of the MCMC test for the “Original” likelihood function. For visualization, water abundances of zero are plotted at 10−2.5. The median ﹩{{\rm{f}}}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ is shown as the vertical line.
Paper: The Cygnus X-1 Puzzle: Implications of X-Ray Polarization Measurements in the Soft and Hard States on the Properties of the Accretion Flow and the Emission Mechanisms
Authors: Henric Krawczynski, Kun Hu
Figure caption: Efficiency ηgrav(r1 = r, r2 = ∞) between the conversion of gravitational energy to free energy when mass moves on Keplerian orbits from r → ∞ to r.
Paper: Do White Dwarfs Sample Water-rich Planetary Material?
Authors: Isabella L. Trierweiler, Carl Melis, Érika Le Bourdais, Patrick Dufour, Alycia J. Weinberger, Boris T. Gänsicke, Nicola Gentile-Fusillo, Siyi Xu, 偲艺 许, Jay Farihi, Andrew Swan, Malena Rice, Edward D. Young
Figure caption: Water mass fractions derived from observed pollution abundances vs. the temperature of the WD; H-WDs are corrected assuming steady state, while He-WDs are corrected assuming the mass-buildup accretion phase. High-temperature WDs, including most of the H-WDs, tend to have lower water mass fractions.
Paper: The Cygnus X-1 Puzzle: Implications of X-Ray Polarization Measurements in the Soft and Hard States on the Properties of the Accretion Flow and the Emission Mechanisms
Authors: Henric Krawczynski, Kun Hu
Figure caption: The observed X-ray fluxes set a lower limit on the energy density Urad of X-rays in the corona. The energy has to be supplied by magnetized plasma with the energy density UB, by soft radiation with energy density Usoft, or bulk motion of plasma with energy density Umatter streaming into the corona, each with its characteristic velocity.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Density at r = 40rs for four azimuthal bins as a function of polar angle. The profiles shown are time averaged over the last 2 days of the simulation.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Terms in the angular momentum conservation Equation (23) for MHD-T in code units. The terms are averaged over the last 2 days of the simulation in azimuth and 10° from the midplane.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Azimuthally averaged radiation (Prad), magnetic (Pmag), and gas (Pgas) pressures as a function of polar angle at r = 40rs, averaged over the last 2 days of the simulations. The profiles for MHD-T, MHD-P, and HD are shown as solid, dashed, and dotted lines, respectively.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Lab-frame radiation energy density slices of MHD-T during the initial self-intersection shock, around the middle of the simulation, and the final snapshot. The top row shows midplane slices, while the bottom row shows vertical slices at the collision angle (shown as a dashed line in the top row panels).
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Luminosity measured at r = 400rs in units of the Eddington luminosity as a function of time since the first self-intersection collision.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Mollweide projection of the radial mass flux for MHD-T measured at r = 100rs and t = 7 days. The cyan × marks the injection angle at r = 400rs, and the black × marks the first stream–stream collision angle. The projection is centered at φ = 0 and is shown in terms of the spherical polar coordinates θ and φ.
Paper: Radiation-magnetohydrodynamic Simulations of Accretion Flow Formation After a Tidal Disruption Event
Authors: Maria Renee Meza, Xiaoshan Huang, 小珊 黄, Shane W. Davis, Yan-Fei Jiang, 燕飞 姜
Figure caption: Disk thickness computed for four azimuthal bins as a function of cylindrical radius. The profiles shown are time averaged over the last 2 days of the simulation.