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Your search keyword '"Raymond, John C [0000-0002-7868-1622]"' showing total 2 results
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2 results on '"Raymond, John C [0000-0002-7868-1622]"'

1. The Spin of a Newborn Black Hole: Swift J1728.9-3613

Author

Draghis, Paul A, Balakrishnan, Mayura, Miller, Jon M, Cackett, Edward, Fabian, Andrew C, Miller-Jones, James, Ng, Mason, Raymond, John C, Reynolds, Mark, Zoghbi, Abderahmen, Draghis, PA [0000-0002-2218-2306], Balakrishnan, M [0000-0001-9641-6550], Miller, JM [0000-0003-2869-7682], Cackett, E [0000-0002-8294-9281], Fabian, AC [0000-0002-9378-4072], Miller-Jones, J [0000-0003-3124-2814], Ng, M [0000-0002-0940-6563], Raymond, JC [0000-0002-7868-1622], Reynolds, M [0000-0003-1621-9392], Zoghbi, A [0000-0002-0572-9613], Apollo - University of Cambridge Repository, Draghis, Paul A [0000-0002-2218-2306], Balakrishnan, Mayura [0000-0001-9641-6550], Miller, Jon M [0000-0003-2869-7682], Cackett, Edward [0000-0002-8294-9281], Fabian, Andrew C [0000-0002-9378-4072], Miller-Jones, James [0000-0003-3124-2814], Ng, Mason [0000-0002-0940-6563], Raymond, John C [0000-0002-7868-1622], Reynolds, Mark [0000-0003-1621-9392], and Zoghbi, Abderahmen [0000-0002-0572-9613]

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), 5101 Astronomical Sciences, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 51 Physical Sciences
Abstract

The origin and distribution of stellar-mass black hole spins are a rare window into the progenitor stars and supernova events that create them. Swift J1728.9-3613 is an X-ray binary, likely associated with the supernova remnant G351.9-0.9 (Balakrishnan et al. 2023). A NuSTAR X-ray spectrum of this source during its 2019 outburst reveals reflection from an accretion disk extending to the innermost stable circular orbit. Modeling of the relativistic Doppler shifts and gravitational redshifts imprinted on the spectrum measures a dimensionless spin parameter of $a=0.86\pm0.02$ ($1\sigma$ confidence), a small inclination angle of the inner accretion disk $\theta0.82$, concluding that the black hole must have formed with a high spin. This demonstrates that black hole formation channels that leave a supernova remnant, and those that do not (e.g. Cyg X-1), can both lead to high natal spin with no requirement for subsequent accretion within the binary system. Emerging disparities between the population of high-spin black holes in X-ray binaries and the low-spin black holes that merge in gravitational wave events may therefore be explained in terms of different stellar conditions prior to collapse, rather than different environmental factors after formation., Comment: 11 pages, 3 appendices, 10 figures. Accepted for publication in ApJ

Published
2023
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2. Defining the Middle Corona

Author

West, Matthew J, Seaton, Daniel B, Wexler, David B, Raymond, John C, Del Zanna, Giulio, Rivera, Yeimy J, Kobelski, Adam R, Chen, Bin, DeForest, Craig, Golub, Leon, Caspi, Amir, Gilly, Chris R, Kooi, Jason E, Meyer, Karen A, Alterman, Benjamin L, Alzate, Nathalia, Andretta, Vincenzo, Auchère, Frédéric, Banerjee, Dipankar, Berghmans, David, Chamberlin, Phillip, Chitta, Lakshmi Pradeep, Downs, Cooper, Giordano, Silvio, Harra, Louise, Higginson, Aleida, Howard, Russell A, Kumar, Pankaj, Mason, Emily, Mason, James P, Morton, Richard J, Nykyri, Katariina, Patel, Ritesh, Rachmeler, Laurel, Reardon, Kevin P, Reeves, Katharine K, Savage, Sabrina, Thompson, Barbara J, Van Kooten, Samuel J, Viall, Nicholeen M, Vourlidas, Angelos, Zhukov, Andrei N, West, Matthew J [0000-0002-0631-2393], Seaton, Daniel B [0000-0002-0494-2025], Wexler, David B [0000-0002-5763-6267], Raymond, John C [0000-0002-7868-1622], Del Zanna, Giulio [0000-0002-4125-0204], Rivera, Yeimy J [0000-0002-8748-2123], Kobelski, Adam R [0000-0002-4691-1729], Chen, Bin [0000-0002-0660-3350], DeForest, Craig [0000-0002-7164-2786], Golub, Leon [0000-0001-9638-3082], Caspi, Amir [0000-0001-8702-8273], Gilly, Chris R [0000-0003-0021-9056], Kooi, Jason E [0000-0002-5595-2522], Meyer, Karen A [0000-0001-6046-2811], Alterman, Benjamin L [0000-0001-6673-3432], Alzate, Nathalia [0000-0001-5207-9628], Andretta, Vincenzo [0000-0003-1962-9741], Auchère, Frédéric [0000-0003-0972-7022], Banerjee, Dipankar [0000-0003-4653-6823], Berghmans, David [0000-0003-4052-9462], Chamberlin, Phillip [0000-0003-4372-7405], Chitta, Lakshmi Pradeep [0000-0002-9270-6785], Downs, Cooper [0000-0003-1759-4354], Giordano, Silvio [0000-0002-3468-8566], Harra, Louise [0000-0001-9457-6200], Higginson, Aleida [0000-0003-1380-8722], Howard, Russell A [0000-0001-9027-8249], Kumar, Pankaj [0000-0001-6289-7341], Mason, Emily [0000-0002-8767-7182], Mason, James P [0000-0002-3783-5509], Morton, Richard J [0000-0001-5678-9002], Nykyri, Katariina [0000-0002-6905-9487], Patel, Ritesh [0000-0001-8504-2725], Rachmeler, Laurel [0000-0002-3770-009X], Reardon, Kevin P [0000-0001-8016-0001], Reeves, Katharine K [0000-0002-6903-6832], Savage, Sabrina [0000-0002-6172-0517], Thompson, Barbara J [0000-0001-6952-7343], Van Kooten, Samuel J [0000-0002-4472-8517], Viall, Nicholeen M [0000-0003-1692-1704], Vourlidas, Angelos [0000-0002-8164-5948], Zhukov, Andrei N [0000-0002-2542-9810], and Apollo - University of Cambridge Repository

Subjects
Corona
Abstract

The middle corona, the region roughly spanning heliocentric distances from 1.5 to 6 solar radii, encompasses almost all of the influential physical transitions and processes that govern the behavior of coronal outflow into the heliosphere. The solar wind, eruptions, and flows pass through the region, and they are shaped by it. Importantly, the region also modulates inflow from above that can drive dynamic changes at lower heights in the inner corona. Consequently, the middle corona is essential for comprehensively connecting the corona to the heliosphere and for developing corresponding global models. Nonetheless, because it is challenging to observe, the region has been poorly studied by both major solar remote-sensing and in-situ missions and instruments, extending back to the Solar and Heliospheric Observatory (SOHO) era. Thanks to recent advances in instrumentation, observational processing techniques, and a realization of the importance of the region, interest in the middle corona has increased. Although the region cannot be intrinsically separated from other regions of the solar atmosphere, there has emerged a need to define the region in terms of its location and extension in the solar atmosphere, its composition, the physical transitions that it covers, and the underlying physics believed to shape the region. This article aims to define the middle corona, its physical characteristics, and give an overview of the processes that occur there.

Published
2023

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