Published 1982 | Version v1
Report Restricted

Neutron star cooling: effects of envelope physics

Creators

Description

Neutron star cooling calculations are reported which employ improved physics in the calculation of the temperature drop through the atmosphere. The atmosphere microphysics is discussed briefly. The predicted neutron star surface temperatures, in the interesting interval 200 less than or equal to t (yr) less than or equal to 105, do not differ appreciably from the earlier results of Van Riper and Lamb (1981) for a non-magnetic star; for a magnetic star, the surface temperature is lower than in the previous work. Comparison with observational limits show that an exotic cooling mechanism, such as neutrino emission from a pion condensate or in the presence of percolating quarks, is not required unless the existence of a neutron star in the Tycho or SN1006 SNRs is established

Availability note (English)

MF available from INIS under the Report Number; Available from NTIS, PC A02/MF A01 as DE83001941.

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Additional details

Publishing Information

Imprint Pagination
5 p.
Report number
LA-UR--82-2844

Conference

Title
International Astronomical Union symposium on supernova remnants and their X-ray emission.
Dates
29 Aug - 2 Sep 1982.
Place
Venice (Italy).

INIS

Country of Publication
United States
Country of Input or Organization
United States
INIS RN
14739664
Subject category
S79: ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;
Resource subtype / Literary indicator
Conference
Descriptors DEI
COOLING; ENERGY TRANSFER; NEUTRINOS; NEUTRON STARS; STAR MODELS; STELLAR ATMOSPHERES
Descriptors DEC
ATMOSPHERES; ELEMENTARY PARTICLES; FERMIONS; LEPTONS; MASSLESS PARTICLES; MATHEMATICAL MODELS; STARS

Optional Information

Secondary number(s)
CONF-820884--2.