Tests of the nuclear equation of state and superfluid and superconducting gaps using the Cassiopeia A neutron star
Tests of the nuclear equation of state and superfluid and superconducting gaps using the Cassiopeia A neutron star
The observed rapid cooling of the Cassiopeia A neutron star can be interpreted as being caused by neutron and proton transitions from normal to superfluid and superconducting states in the stellar core. Here we present two new Chandra ACIS-S Graded observations of this neutron star and measurements of the neutron star mass M and radius R found from consistent fitting of both the X-ray spectra and cooling behavior. This comparison is only possible for individual nuclear equations of state. We test phenomenological superfluid and superconducting gap models which mimic many of the known theoretical models against the cooling behavior. Our best-fit solution to the Cassiopeia A data is one in which the (M,R) = (1.44 Msun,12.6 km) neutron star is built with the BSk21 equation of state, strong proton superconductor and moderate neutron triplet superfluid gap models, and a pure iron envelope or a thin carbon layer on top of an iron envelope, although there are still large observational and theoretical uncertainties.
015806-1 -015806-11
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Elshamouty, Khaled G.
b9d05acc-ca3c-450e-89ef-6abf0652e21e
Heinke, Craig O.
d7382ed2-cb85-4e15-b2d9-296fc8b6221d
Potekhin, Alexander Y.
b9551650-f6ed-4c4f-b53c-d019cccc49fa
14 January 2015
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Elshamouty, Khaled G.
b9d05acc-ca3c-450e-89ef-6abf0652e21e
Heinke, Craig O.
d7382ed2-cb85-4e15-b2d9-296fc8b6221d
Potekhin, Alexander Y.
b9551650-f6ed-4c4f-b53c-d019cccc49fa
Ho, Wynn C.G., Elshamouty, Khaled G., Heinke, Craig O. and Potekhin, Alexander Y.
(2015)
Tests of the nuclear equation of state and superfluid and superconducting gaps using the Cassiopeia A neutron star.
Physical Review C, 91 (1), , [15806].
(doi:10.1103/PhysRevC.91.015806).
Abstract
The observed rapid cooling of the Cassiopeia A neutron star can be interpreted as being caused by neutron and proton transitions from normal to superfluid and superconducting states in the stellar core. Here we present two new Chandra ACIS-S Graded observations of this neutron star and measurements of the neutron star mass M and radius R found from consistent fitting of both the X-ray spectra and cooling behavior. This comparison is only possible for individual nuclear equations of state. We test phenomenological superfluid and superconducting gap models which mimic many of the known theoretical models against the cooling behavior. Our best-fit solution to the Cassiopeia A data is one in which the (M,R) = (1.44 Msun,12.6 km) neutron star is built with the BSk21 equation of state, strong proton superconductor and moderate neutron triplet superfluid gap models, and a pure iron envelope or a thin carbon layer on top of an iron envelope, although there are still large observational and theoretical uncertainties.
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e-pub ahead of print date: 14 January 2015
Published date: 14 January 2015
Organisations:
Applied Mathematics
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Local EPrints ID: 373013
URI: http://eprints.soton.ac.uk/id/eprint/373013
ISSN: 0556-2813
PURE UUID: 30dfe8c2-ed6c-4307-87cf-e729d052386e
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Date deposited: 06 Jan 2015 10:17
Last modified: 14 Mar 2024 18:46
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Contributors
Author:
Khaled G. Elshamouty
Author:
Craig O. Heinke
Author:
Alexander Y. Potekhin
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