Neutron Star Binaries
Neutron star binaries are believed to result from direct evolution of binary
star systems where one star undergoes a supernova explosion, leaving behind
a neutron star, or from tidal capture of a companion star in a dense globular
cluster. The neutron star can accrete matter from its companion and X-rays
are emitted from the resulting acretion disk or from material falling onto
the surface of the neutron star.
Some of our pictures and recent papers.
ASCA SIS image
of X-ray burster 1728-34.
4U 1915-05
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L. Boirin, D. Barret,
J.F. Olive, J.E. Grindlay, P.F. Bloser 1998, "Low and high frequency
Quasi-Periodic Oscillations in 4U1915-05," Adv. in Space Research, in press
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D. Barret , L. Boirin
, J.F. Olive , J.E. Grindlay, P. F. Bloser , J. Swank, A. P. Smale
1998, "Discovery of High Frequency Quasi-Periodic Oscillations in 4U1915-05,"
Astrophysical Letters and Communications, in press
4U 1820-30
XB 1728-34
KS 1731-260
1E 1724-3045
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D. Barret, J. E. Grindlay,
I. M. Harrus, J. F. Olive 1998, "An ASCA X-ray Observation of
1E1724-3045 in the globular cluster Terzan 2," A&A, in press.
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J.F. Olive, D. Barret,
L. Boirin, J.E. Grindlay 1998, "RXTE Broad Band X-ray Spectrum of the
Burster 1E1724-3045", Proc. of the 32nd COSPAR Meeting
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