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Title: Fast pulsars, strange stars

Conference ·
OSTI ID:6903945

The initial motivation for this work was the reported discovery in January 1989 of a 1/2 millisecond pulsar in the remnant of the spectacular supernova, 1987A. The status of this discovery has come into grave doubt as of data taken by the same group in February, 1990. At this time we must consider that the millisecond signal does not belong to the pulsar. The existence of a neutron star in remnant of the supernova is suspected because of recent observations on the light curve of the remnant, and of course by the neutrino burst that announced the supernova. However its frequency is unknown. I can make a strong case that a pulsar rotation period of about 1 ms divides those that can be understood quite comfortably as neutron stars, and those that cannot. What we will soon learn is whether there is an invisible boundary below which pulsar periods do not fall, in which case, all are presumable neutron stars, or whether there exist sub- millisecond pulsars, which almost certainly cannot be neutron stars. Their most plausible structure is that of a self-bound star, a strange-quark-matter star. The existence of such stars would imply that the ground state of the strong interaction is not, as we usually assume, hadronic matter, but rather strange quark matter. Let us look respectively at stars that are bound only by gravity, and hypothetical stars that are self-bound, for which gravity is so to speak, icing on the cake.

Research Organization:
Lawrence Berkeley Lab., CA (USA)
Sponsoring Organization:
DOE/ER
DOE Contract Number:
AC03-76SF00098
OSTI ID:
6903945
Report Number(s):
LBL-28680; CONF-900295-5; ON: DE90011631; TRN: 90-016582
Resource Relation:
Conference: 6. workshop on nuclear dynamics, Jackson Hole, WY (USA), 17-24 Feb 1990
Country of Publication:
United States
Language:
English