Cooling of the Cassiopeia A neutron star and the effect of diffusive nuclear burning
Cooling of the Cassiopeia A neutron star and the effect of diffusive nuclear burning
The study of how neutron stars cool over time can provide invaluable insights into fundamental physics such as the nuclear equation of state and superconductivity and superfluidity. A critical relation in neutron star cooling is the one between observed surface temperature and interior temperature. This relation is determined by the composition of the neutron star envelope and can be influenced by the process of diffusive nuclear burning (DNB). We calculate models of envelopes that include DNB and find that DNB can lead to a rapidly changing envelope composition which can be relevant for understanding the long-term cooling behavior of neutron stars. We also report on analysis of the latest temperature measurements of the young neutron star in the Cassiopeia A supernova remnant. The 13 Chandra observations over 18 years show that the neutron star's temperature is decreasing at a rate of 2-3 percent per decade, and this rapid cooling can be explained by the presence of a proton superconductor and neutron superfluid in the core of the star.
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Ho, Wynn C.G.
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Wijngaarden, M.J.P.
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Chang, Philip
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Heinke, Craig O.
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Page, Dany
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Beznogov, Mikhail
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Patnaude, Daniel J.
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Ho, Wynn C.G.
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Wijngaarden, M.J.P.
e6064827-8f6f-4fc4-b24d-140d11939237
Chang, Philip
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Heinke, Craig O.
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Page, Dany
a48ed41a-7418-4809-a60a-8c44788f99a1
Beznogov, Mikhail
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Patnaude, Daniel J.
435264be-34f2-4810-a581-ad5057b201db
Ho, Wynn C.G., Wijngaarden, M.J.P., Chang, Philip, Heinke, Craig O., Page, Dany, Beznogov, Mikhail and Patnaude, Daniel J.
(2019)
Cooling of the Cassiopeia A neutron star and the effect of diffusive nuclear burning.
AIP Conference Proceedings, 2127, , [020007].
(doi:10.1063/1.5117797).
Abstract
The study of how neutron stars cool over time can provide invaluable insights into fundamental physics such as the nuclear equation of state and superconductivity and superfluidity. A critical relation in neutron star cooling is the one between observed surface temperature and interior temperature. This relation is determined by the composition of the neutron star envelope and can be influenced by the process of diffusive nuclear burning (DNB). We calculate models of envelopes that include DNB and find that DNB can lead to a rapidly changing envelope composition which can be relevant for understanding the long-term cooling behavior of neutron stars. We also report on analysis of the latest temperature measurements of the young neutron star in the Cassiopeia A supernova remnant. The 13 Chandra observations over 18 years show that the neutron star's temperature is decreasing at a rate of 2-3 percent per decade, and this rapid cooling can be explained by the presence of a proton superconductor and neutron superfluid in the core of the star.
Text
1904.07505
- Accepted Manuscript
Text
1.5117797
- Version of Record
More information
Accepted/In Press date: 4 April 2019
e-pub ahead of print date: 17 July 2019
Additional Information:
The following article has been accepted by AIP Conference Proceedings. After it is published, it will be found at https://aip.scitation.org/journal/apc.
Identifiers
Local EPrints ID: 430315
URI: http://eprints.soton.ac.uk/id/eprint/430315
ISSN: 1551-7616
PURE UUID: 3f9607ba-502a-44ef-bc30-ed599f90ccb0
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Date deposited: 25 Apr 2019 16:30
Last modified: 16 Mar 2024 07:47
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Contributors
Author:
M.J.P. Wijngaarden
Author:
Philip Chang
Author:
Craig O. Heinke
Author:
Dany Page
Author:
Mikhail Beznogov
Author:
Daniel J. Patnaude
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