Investigating Photocenter Contamination in Interacting Binaries Using the Multi-wavelength Capabilities of SIM-Lite

Details Investigating Photocenter Contamination in Interacting Binaries Using the Multi-wavelength Capabilities of SIM-Lite Investigating Photocenter Contamination in Interacting Binaries Using the Multi-wavelength Capabilities of SIM-Lite

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541916g&link_type=abstract

American Astronomical Society, AAS Meeting #215, #419.16; Bulletin of the American Astronomical Society, Vol. 42, p.278

Astronomy and Astrophysics

Astronomy

Scientific paper

Interacting binaries consist of a compact object accreting from a non-degenerate companion. This accretion can dominate the luminosity of an interacting binary system. Because SIM-Lite only measures the photocenter of an astrometric target, determining the true astrometric orbits of such systems will be difficult. We have modified the Eclipsing Light Curve code (Orosz & Hauschildt 1999) to allow us to model the reflex motions of interacting binaries. This code gives us sufficient flexibility to investigate nearly every configuration of interacting binary. We find that SIM will be able to determine astrometric orbits for all sufficiently bright interacting binaries where the primary or secondary star dominates the luminosity. For systems where there are multiple components that comprise the spectrum in the optical bandpass accessible to SIM-Lite, multi-wavelength photometry, and data on system parameters, will be required to extract the true astrometric orbit. There are a large number of systems where the accretion disk dominates the luminosity. In these cases, only the orbital inclination will be constrained by SIM-Lite observations. In all of these cases, however, SIM-Lite will provide valuable information that will allow us to begin to understand the complex evolution of mass-transferring binaries. It remains critical that SIM-Lite maintains a multi-wavelength capability to allow for the proper deconvolution of the astrometric orbits in multi-component systems.

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