Spectral Mapping of Accretion Disks in Cataclysmic Binaries: Bridging the CV Period Gap

Details Spectral Mapping of Accretion Disks in Cataclysmic Binaries: Bridging the CV Period Gap Spectral Mapping of Accretion Disks in Cataclysmic Binaries: Bridging the CV Period Gap

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6796b&link_type=abstract

HST Proposal ID #6796

Physics

Hst Proposal Id #6796 Binaries And Star Formation

Scientific paper

Maximum-entropy eclipse mapping techniques have advanced to the stage of delivering spatially-resolved spectra of accretion disks. By fitting disk model atmospheres to these spectra we are now able to determine the radial run of the temperature, surface density {which controls the local effective gravity of the disk}, Mach number {which controls the strength of Balmer lines vs Balmer continuum}, and the vertical temperature gradient in the disk {which controls whether the lines are in emission or absorption}. Accretion disks in Cataclysmic Variables {CVs} cover a range of accretion rates and viscosity states. CVs show a bi-modal distribution of orbital periods, with systems clustering at periods of 1.5-2 hr or 3-5 hr, and a remarkable dearth of systems with periods between 2-3 hr. Our previous HST mapping experiments have framed accretion disks on both sides of this period gap, corresponding to the low and high accretion regimes. We now propose to look inside the gap by mapping the disk of V348 Pup {P_orb= 2.44 hr}. There are evidences that its disk has different properties from those previously mapped by HST at shorter and longer periods. Observations of this type can drive fundamental new insights into the physics of accretion disks.

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