Physics
Scientific paper
Jan 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...336..360e&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 336, Jan. 1, 1989, p. 360-366. Research supported by NSF.
Physics
41
Afterglows, Cooling, Neutron Stars, Radiative Heat Transfer, Stellar Physics, Energy Transfer, Gamma Ray Bursts, Measurement
Scientific paper
Thermal afterglow from transient energy releases in neutron stars, such as may result from glitches or gamma-ray bursts, is considered. If observable, thermal afterglow may provide important information on the nature of these events and on neutron star structure. For standard neutron star models, the energy released is either reradiated within a short time of at most hours for energy release near the surface, or most of the energy is stored in the deep interior and then reradiated over thousands of years. Intermediate time scales of order months are possible for afterglow, but only when the prompt afterglow accounts for a very small fraction of the total energy release, and enormous energy releases of about 10 to the 42nd ergs are required to make the afterglow last much longer than a few hours. An observational program to detect afterglow will need to accommodate short time scales.
Cheng Andrew F.
Eichler David
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