The Orbital Period of the Atoll--Source X0614+09

Details The Orbital Period of the Atoll--Source X0614+09 The Orbital Period of the Atoll--Source X0614+09

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999noao.prop..164w&link_type=abstract

NOAO Proposal ID #1999B-0164

Computer Science

Scientific paper

The most luminous stellar X-ray sources are interacting binaries that contain either a neutron star (NS) or a black hole. These ``X-ray binaries'' are important, since they allow the determination of NS masses which in turn can be used to constrain the equation of state of nuclear matter. The most luminous LMXBs fall into two classes characterized by their X-ray time and spectral variability. They are termed Z-sources and Atoll-sources according to the pattern they trace in the X-ray color-color diagram. The Z-sources are believed to have both higher accretion rates and stronger NS magnetic fields than the Atoll-sources. It has been suggested that this difference might be an evolutionary effect leading to evolved companions/long periods for Z- and dwarf companions/short periods for Atoll-sources. This prediction holds true so far for the Z-sources, but recent observations indicate that the picture for Atoll-sources is more complex. We propose to photometrically monitor the Atoll-source X0614+091 in order to determine the orbital period of the system and explore the validity of the evolutionary model for Z- and Atoll-sources.

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