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Millisecond Pulsars

Published online by Cambridge University Press:  14 August 2015

J.H. Krolik
J.H. Krolik*
Affiliation:
Department of Physics and Astronomy, Johns Hopkins University, Baltimore MD 21218, USA

Abstract

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Millisecond pulsars are intrinsically interesting because they illustrate some of the most extreme physical conditions to be found anywhere in the Universe, and because their evolution exhibits several stages of great drama. It had been widely believed for several years that spin-up of an old neutron star by accretion from a close stellar companion explained their fast rotation, but the absence of companions in several cases cast doubt on that picture. This spring a millisecond pulsar in a close binary was discovered in which the companion appears to be evaporating, thus reconciling the existence of lone millisecond pulsars with the standard picture. Ongoing observations of this new system, and complementary calculations, promise to answer many of the questions remaining about this dramatic phase in stellar evolution.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 8: Highlights of Astronomy. As presented at the XXth General Assembly of the IAU, 1988 , 1989 , pp. 161 - 165
Copyright
Copyright © Kluwer 1989

References

Alpar, M.A., Cheng, A.F., Ruderman, M.A., and Shaham, J., 1982, Nature 300, 728.CrossRefGoogle Scholar
Cheng, A., 1988, submitted to Ap. J.Google Scholar
Djorgovski, S. and Evans, C., 1988, submitted to Ap. J. Lett,Google Scholar
Eichler, D. and Levinson, A., 1988, submitted to Ap. J. Lett.Google Scholar
Fruchter, A.S., 1988, private communicationGoogle Scholar
Ftuchter, A.S., Gunn, J.E., Lauer, T.R., and Dressler, A., 1988, Nature 334, 686.CrossRefGoogle Scholar
Fruchter, A.S., Stinebring, D.R., and Taylor, J.H., 1988, Nature 333, 237.CrossRefGoogle Scholar
Kluźniak, W., Ruderman, M., Shaham, J., and Tavani, M., 1988, Nature 334, 225.CrossRefGoogle Scholar
Kulkarni, S.R., 1988, in Physics of Neutron Stars and Black Holes, ed. Tanaka, Y. (Institute of Space and Astronautical Science: Tokyo)Google Scholar
Kulkarni, S.R., Djorgovski, S., and Fruchter, A.S., 1988, Nature 334, 504.CrossRefGoogle Scholar
Kulkarni, S.R. and Hester, J.J., 1988, submitted to Nature Google Scholar
Michel, F.C., 1988, submitted to Nature Google Scholar
Phinney, E.S., Evans, C.R., Blandford, R.D., and Kulkarni, S.R., 1988, Nature 333, 832.CrossRefGoogle Scholar
Rasio, F.A., Shapiro, S.L., and Teukolsky, S.A., 1988, submitted to Nature Google Scholar
Ruderman, M., Shaham, J., and Tavani, M., 1988, Ap. J. in press.Google Scholar
Ruderman, M., Shaham, J., Tavani, M., and Eichler, D., 1988, Ap. J. in press.Google Scholar
van den Heuvel, E.P.J, and van Paradijs, J., 1988, Nature 334, 227.CrossRefGoogle Scholar
van Paradijs, J., Allington-Smith, J., Callanan, P., Charles, P.A., Hassall, B.J.M., Machin, G., Mason, K.O., Naylor, T., and Smale, A.P., 1988, Nature 334, 684.CrossRefGoogle Scholar