Modeling Multi-Wavelength Stellar Astrometry. I. SIM Lite Observations of Interacting Binaries - Astrophysics > Solar and Stellar AstrophysicsReport as inadecuate




Modeling Multi-Wavelength Stellar Astrometry. I. SIM Lite Observations of Interacting Binaries - Astrophysics > Solar and Stellar Astrophysics - Download this document for free, or read online. Document in PDF available to download.

Abstract: Interacting binaries consist of a secondary star which fills or is very closeto filling its Roche lobe, resulting in accretion onto the primary star, whichis often, but not always, a compact object. In many cases, the primary star,secondary star, and the accretion disk can all be significant sources ofluminosity. SIM Lite will only measure the photocenter of an astrometrictarget, and thus determining the true astrometric orbits of such systems willbe difficult. We have modified the Eclipsing Light Curve code Orosz andHauschildt 2000 to allow us to model the flux-weighted reflex motions ofinteracting binaries, in a code we call REFLUX. This code gives us sufficientflexibility to investigate nearly every configuration of interacting binary. Wefind that SIM Lite will be able to determine astrometric orbits for allsufficiently bright interacting binaries where the primary or secondary stardominates the luminosity. For systems where there are multiple components thatcomprise the spectrum in the optical bandpass accessible to SIM Lite, we findit is possible to obtain absolute masses for both components, althoughmulti-wavelength photometry will be required to disentangle the multiplecomponents. In all cases, SIM Lite will at least yield accurate inclinations,and provide valuable information that will allow us to begin to understand thecomplex evolution of mass-transferring binaries. It is critical that SIM Litemaintains a multi-wavelength capability to allow for the proper deconvolutionof the astrometric orbits in multi-component systems.



Author: Jeffrey L. Coughlin, Dawn M. Gelino, Thomas E. Harrison, D. W. Hoard, David R. Ciardi, G. Fritz Benedict, Steve B. Howell, Barbar

Source: https://arxiv.org/



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