Superfluid neutrons in the core of the neutron star in Cassiopeia A

Dany Page; Madappa Prakash; James M. Lattimer; Andrew W. Steiner

Superfluid neutrons in the core of the neutron star in Cassiopeia A

Dany Page
, Madappa Prakash
, James M. Lattimer
, Andrew W. Steiner

Physics and Astronomy

Universidad Nacional Autónoma de México
Ohio University
University of Washington

Research output: Contribution to journal › Conference article › peer-review

Abstract

The supernova remnant Cassiopeia A contains the youngest known neutron star which is also the first one for which real time cooling has ever been observed. In order to explain the rapid cooling of this neutron star, we first present the fundamental properties of neutron stars that control their thermal evolution with emphasis on the neutrino emission processes and neutron/proton superfluidity/superconductivity. Equipped with these results, we present a scenario in which the observed cooling of the neutron star in Cassiopeia A is interpreted as being due to the recent onset of neutron superfluidity in the core of the star. The manner in which the earlier occurrence of proton superconductivity determines the observed rapidity of this neutron star’s cooling is highlighted.

Original language	English
Journal	Proceedings of Science
Volume	142
State	Published - 2011
Event	34th Edition of the Brazilian Workshop on Nuclear Physics, BWNP 2011 - Foz de Iguacu, Brazil Duration: Jun 5 2011 → Jun 10 2011

Cite this

@article{f321094710c840fcb877f31ddb6d2192,

title = "Superfluid neutrons in the core of the neutron star in Cassiopeia A",

abstract = "The supernova remnant Cassiopeia A contains the youngest known neutron star which is also the first one for which real time cooling has ever been observed. In order to explain the rapid cooling of this neutron star, we first present the fundamental properties of neutron stars that control their thermal evolution with emphasis on the neutrino emission processes and neutron/proton superfluidity/superconductivity. Equipped with these results, we present a scenario in which the observed cooling of the neutron star in Cassiopeia A is interpreted as being due to the recent onset of neutron superfluidity in the core of the star. The manner in which the earlier occurrence of proton superconductivity determines the observed rapidity of this neutron star{\textquoteright}s cooling is highlighted.",

author = "Dany Page and Madappa Prakash and Lattimer, \{James M.\} and Steiner, \{Andrew W.\}",

note = "Publisher Copyright: {\textcopyright} Copyright owned by the author(s).; 34th Edition of the Brazilian Workshop on Nuclear Physics, BWNP 2011 ; Conference date: 05-06-2011 Through 10-06-2011",

year = "2011",

language = "English",

volume = "142",

journal = "Proceedings of Science",

issn = "1824-8039",

}

TY - JOUR

T1 - Superfluid neutrons in the core of the neutron star in Cassiopeia A

AU - Page, Dany

AU - Prakash, Madappa

AU - Lattimer, James M.

AU - Steiner, Andrew W.

N1 - Publisher Copyright: © Copyright owned by the author(s).

PY - 2011

Y1 - 2011

N2 - The supernova remnant Cassiopeia A contains the youngest known neutron star which is also the first one for which real time cooling has ever been observed. In order to explain the rapid cooling of this neutron star, we first present the fundamental properties of neutron stars that control their thermal evolution with emphasis on the neutrino emission processes and neutron/proton superfluidity/superconductivity. Equipped with these results, we present a scenario in which the observed cooling of the neutron star in Cassiopeia A is interpreted as being due to the recent onset of neutron superfluidity in the core of the star. The manner in which the earlier occurrence of proton superconductivity determines the observed rapidity of this neutron star’s cooling is highlighted.

AB - The supernova remnant Cassiopeia A contains the youngest known neutron star which is also the first one for which real time cooling has ever been observed. In order to explain the rapid cooling of this neutron star, we first present the fundamental properties of neutron stars that control their thermal evolution with emphasis on the neutrino emission processes and neutron/proton superfluidity/superconductivity. Equipped with these results, we present a scenario in which the observed cooling of the neutron star in Cassiopeia A is interpreted as being due to the recent onset of neutron superfluidity in the core of the star. The manner in which the earlier occurrence of proton superconductivity determines the observed rapidity of this neutron star’s cooling is highlighted.

UR - https://www.scopus.com/pages/publications/85053334705

M3 - Conference article

AN - SCOPUS:85053334705

SN - 1824-8039

VL - 142

JO - Proceedings of Science

JF - Proceedings of Science

T2 - 34th Edition of the Brazilian Workshop on Nuclear Physics, BWNP 2011

Y2 - 5 June 2011 through 10 June 2011

ER -

Superfluid neutrons in the core of the neutron star in Cassiopeia A

Abstract

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