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Record 1 of 4853
Geminga: A cooling superfluid neutron star
External Online Source: doi:10.1086/174236
Author and Affiliation:
Page, Dany(Columbia University, New York, NY, United States)
Abstract: We compare the recent temperature estimate for Geminga with neutron star cooling models. Because of its age (approximately 3.4 x 10(exp 5) yr), Geminga is in the photon cooling era. We show that its surface temperature (approximately 5.2 x 10(exp 5) K) can be understood by both types of neutrino cooling scenarios, i.e., slow neutrino cooling by the modified Urca process or fast neutrino cooling by the direct Urca process or by some exotic matter, and thus does not allow us to discriminate between these two competing schemes. However, for both types of scenarios, agreement with the observed temperature can only be obtained if baryon pairing is present in most, if not all, of the core of the star. Within the slow neutrino cooling scenario, early neutrino cooling is not sufficient to explain the observed low temperature, and extensive pairing in the core is necessary to reduce the specific heat and increase the cooling rate in the present photon cooling era. Within all the fast neutrino cooling scenarios, pairing is necessary throughout the whole core to control the enormous early neutrino emission which, without pairing suppression, would result in a surface temperature at the present time much lower than observed. We also comment on the recent temperature estimates for PSR 0656+14 and PSR 1055-52, which pertain to the same photon cooling era. If one assumes that all neutron stars undergo fast neutrino cooling, then these two objects also provide evidence for extensive baryon pairing in their core; but observational uncertainties also permit a more conservative interpretation, with slow neutrino emission and no pairing at all. We argue though that observational evidence for the slow neutrino cooling model (the 'standard' model) is in fact very dim and that the interpretation of the surface temperature of all neutron stars could be done with a reasonable theoretical a priori within the fast neutrino cooling scenarios only. In this case, Geminga, PSR 0656+14, and PSR 1055-52 all show evidence of baryon pairing down to their very centers.
Publication Date: Jun 10, 1994
Document ID:
19950048301
(Acquired Dec 28, 1995)
Accession Number: 95A79900
Subject Category: ASTROPHYSICS
Document Type: Journal Article
Publication Information: Astrophysical Journal, Part 1 (ISSN 0004-637X); 428; 1; p. 250-260
Publisher Information: United States
Contract/Grant/Task Num: NAGW-3075
Financial Sponsor: NASA; United States
Organization Source: NASA; Washington, DC, United States
Description: 11p; In English
Distribution Limits: Unclassified; Publicly available; Unlimited
Rights: Copyright
NASA Terms: BARYONS; NEUTRINOS; NEUTRON STARS; PLASMA COOLING; STELLAR CORES; SUPERFLUIDITY; SURFACE TEMPERATURE; DENSE PLASMAS; SPECIFIC HEAT; STELLAR MODELS; SUPERNOVA REMNANTS
Imprint And Other Notes: Astrophysical Journal, Part 1 vol. 428, no. 1 p. 250-260 June 10, 1994
Availability Source: Other Sources
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