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Surface composition of magnetic neutron stars.The relative abundances of seven constituent nuclei, He4, C12, O16, Ne20, Mg24, Si28, and Fe56, are calculated as a function of time for neutron star atmospheres within which exist magnetic fields of the order of 10 to the 13th G. The opacity, equation of state of the electrons, and cooling rate of the magnetic star are discussed, and it is shown to be a reasonable approximation to assume an atmosphere to be isothermal. The effects of particle diffusion are included in the nuclear reaction network. Computations are performed both for a constant mass atmosphere and for an atmosphere in which mass is being ejected. It is found that the final abundances are model-independent, as long as the initial model contains predominantly He4. The relative abundances are compared to the cosmic ray spectrum. For both the constant-mass and mass-loss atmospheres, nucleosynthesis proceeds virtually completely to Fe56. However the outermost layers of the envelope, in which no mass is being ejected, are composed almost entirely of He4 with trace amounts of Fe56. After the loss of about 10 to the 21st g, only Fe56 is ejected from atmospheres expelling mass.
Document ID
19730027926
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Rosen, L. C.
(Dartmouth College Hanover, N.H., United States)
Cameron, A. G. W.
(Yeshiva University; NASA, Goddard Institute for Space Studies, New York, N.Y., United States)
Date Acquired
August 7, 2013
Publication Date
January 1, 1972
Publication Information
Publication: Astrophysics and Space Science
Volume: 15
Subject Category
Space Sciences
Accession Number
73A12728
Distribution Limits
Public
Copyright
Other

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