Double Degenerate Binary Stars: Constraining the Masses of Compact Objects

Details Double Degenerate Binary Stars: Constraining the Masses of Compact Objects Double Degenerate Binary Stars: Constraining the Masses of Compact Objects

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999noao.prop..211h&link_type=abstract

NOAO Proposal ID #1999B-0211

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Scientific paper

Double degenerates are binary stars containing two compact objects (white dwarfs, neutron stars, or WD+NS). Like other binary stars, double degenerates offer an opportunity to accurately determine the masses of the binary components. The upper limit NS mass, for example, has important implications for our understanding of the equation of state of matter at high (nuclear) density. Double degenerates are also important as probes of gravitational radiation and general relativity. The emission of gravitational radiation may cause some double degenerates to merge on timescales less than a Hubble time. Such merging systems may be progenitors of type Ia supernovae. We propose two observing runs on the CTIO 1.5m telescope (+ CCD imager) to investigate double degenerates. The first run (1 night) will be used to search for eclipses in the P_orb=1.4 h WD+WD binary WD 0957-666. Detection of eclipses could be used in conjunction with existing spectroscopic data to determine the sizes of the WDs and provide checks of the theoretical WD mass-radius relation. The second run (2 nights) will be used to search for optical counterparts to three radio pulsars believed to be NS+WD binaries. If the WD components in these systems can be identified optically, then future investigations can provide constraints on the elusive NS mass.

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