Binary Interaction in the Mira AB Accreting System

Details Binary Interaction in the Mira AB Accreting System Binary Interaction in the Mira AB Accreting System

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8298k&link_type=abstract

HST Proposal ID #8298

Computer Science

Hst Proposal Id #8298 Binary Stars

Scientific paper

The Mira AB system belongs to a class of detached binaries in which a compact object accretes mass from the wind of a cool giant or supergiant. This system provides a unique laboratory for detailed study of wind accretion processes because it is the only wind-accreting binary that has been resolved with the HST and whose components can be studied individually. In 1995, we resolved this binary using the HST FOC camera images and objective prism observations. We detected significant asymmetries in the giant's atmosphere and found evidence for possible interaction with its companion. A study of the asymmetric outflow from Mira can be pivotal for understanding the early formation of asymmetries in the atmospheres and the circumstellar envelopes of planetary nebulae progenitors, because Mira-type stars are a critical link in the evolutionary path toward planetary nebulae. We propose to carry out follow up HST observations using STIS to obtain high spatial/spectral resolution ob se rvations of each component of the system. Our main scientific objectives are: 1. To further study the signatures of the interaction between Mira A and Mira B; 2. To determine if the asymmetries in Mira A are related to a bipolar outflow or structures in the extended atmosphere; 3. To carry out detailed study and modeling of the accretion processes in the system.

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