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Title: Constraining superfluidity in dense matter from the cooling of isolated neutron stars

Authors:
; ; ;
Publication Date:
Sponsoring Org.:
USDOE
OSTI Identifier:
1418070
Resource Type:
Journal Article: Publisher's Accepted Manuscript
Journal Name:
Physical Review C
Additional Journal Information:
Journal Volume: 97; Journal Issue: 1; Related Information: CHORUS Timestamp: 2018-01-25 08:15:15; Journal ID: ISSN 2469-9985
Publisher:
American Physical Society
Country of Publication:
United States
Language:
English

Citation Formats

Beloin, Spencer, Han, Sophia, Steiner, Andrew W., and Page, Dany. Constraining superfluidity in dense matter from the cooling of isolated neutron stars. United States: N. p., 2018. Web. doi:10.1103/PhysRevC.97.015804.
Beloin, Spencer, Han, Sophia, Steiner, Andrew W., & Page, Dany. Constraining superfluidity in dense matter from the cooling of isolated neutron stars. United States. doi:10.1103/PhysRevC.97.015804.
Beloin, Spencer, Han, Sophia, Steiner, Andrew W., and Page, Dany. 2018. "Constraining superfluidity in dense matter from the cooling of isolated neutron stars". United States. doi:10.1103/PhysRevC.97.015804.
@article{osti_1418070,
title = {Constraining superfluidity in dense matter from the cooling of isolated neutron stars},
author = {Beloin, Spencer and Han, Sophia and Steiner, Andrew W. and Page, Dany},
abstractNote = {},
doi = {10.1103/PhysRevC.97.015804},
journal = {Physical Review C},
number = 1,
volume = 97,
place = {United States},
year = 2018,
month = 1
}

Journal Article:
Free Publicly Available Full Text
This content will become publicly available on January 25, 2019
Publisher's Accepted Manuscript

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  • Cited by 178
  • We propose that the observed cooling of the neutron star in Cassiopeia A is due to enhanced neutrino emission from the recent onset of the breaking and formation of neutron Cooper pairs in the {sup 3}P{sub 2} channel. We find that the critical temperature for this superfluid transition is {approx_equal}0.5x10{sup 9} K. The observed rapidity of the cooling implies that protons were already in a superconducting state with a larger critical temperature. This is the first direct evidence that superfluidity and superconductivity occur at supranuclear densities within neutron stars. Our prediction that this cooling will continue for several decades atmore » the present rate can be tested by continuous monitoring of this neutron star.« less
  • Baryon and quark superfluidity in the cooling of neutron stars are investigated. Future observations will allow us to constrain combinations of the neutron or {lambda} -hyperon pairing gaps and the star's mass. However, in a hybrid star with a mixed phase of hadrons and quarks, quark gaps larger than a few tenths of an MeV render quark matter virtually invisible for cooling. If the quark gap is smaller, quark superfluidity could be important, but its effects will be nearly impossible to distinguish from those of other baryonic constituents. (c) 2000 The American Physical Society.
  • We investigate the effect of microscopic three-body forces on the {sup 3}P F{sub 2} neutron superfluidity in neutron matter, {beta}-stable neutron star matter, and neutron stars by using the BCS theory and the Brueckner-Hartree-Fock approach. We adopt the Argonne V18 potential supplemented with a microscopic three-body force as the realistic nucleon-nucleon interaction. We have concentrated on studying the three-body force effect on the {sup 3}P F{sub 2} neutron pairing gap. It is found that the three-body force effect considerably enhances the {sup 3}P F{sub 2} neutron superfluidity in neutron star matter and neutron stars.
  • The nearby isolated neutron stars (INSs) are a group of seven relatively slowly rotating neutron stars that show thermal X-ray spectra, most with broad absorption features. They are interesting both because they may allow one to determine fundamental neutron-star properties by modeling their spectra, and because they appear to be a large fraction of the overall neutron-star population. Here, we describe a series of XMM -Newton observations of the nearby INS RX J0806.4-4123, taken as part of larger program of timing studies. From these, we limit the spin-down rate to nu-dot=(-4.3+-2.3)x10{sub -16}Hz s{sup -1}. This constrains the dipole magnetic fieldmore » to be <3.7 x 10{sup 13} G at 2sigma, significantly less than the field of approx10{sup 14} G implied by simple models for the X-ray absorption found at 0.45 keV. We confirm that the spectrum is thermal and stable (to within a few percent), but find that the 0.45 keV absorption feature is broader and more complex than previously thought. Considering the population of INSs, we find that magnetic field decay from an initial field of approx<3 x 10{sup 14} G accounts most naturally for their timing and spectral properties, both qualitatively and in the context of the models for field decay of Pons and collaborators.« less