Sakurai's Novalike Object: Real-Time Monitoring of a Stellar Thermal Pulse

Details Sakurai's Novalike Object: Real-Time Monitoring of a Stellar Thermal Pulse Sakurai's Novalike Object: Real-Time Monitoring of a Stellar Thermal Pulse

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8593b&link_type=abstract

HST Proposal ID #8593

Physics

Hst Proposal Id #8593 Hot Stars

Scientific paper

This is a continuation of a Cycle 7-8 Long-Term program. Sakurai's novalike variable {V4334 Sgr} presents a ``once-in-a-lifetime'' opportunity for real-time observations of a star undergoing a final helium thermal pulse. The star rose from obscurity to become an 11th-magnitude, hydrogen-deficient red giant in 1995-96, and currently it is undergoing episodes of atmospheric dust formation which make it drop to quite faint magnitudes at random intervals. If it follows the pattern of the similar object V605 Aql, it will soon begin evolving back to high temperature. During the subsequent few years, it would then begin to {re}-ionize its large, faint planetary nebula, and we should be able to witness the re-establishment of a fast stellar wind as the effective temperature increases. The spectroscopic portion of this program is a Target-of-Oppurtunity. When the star does start to become hot again, we will start using STIS to monitor the spectroscopic development of the star in the UV at regular intervals, continuing over the next 3 Cycles. We will also use WFPC2 once a year to monitor expansion of the ejecta. In combination with ground-based monitoring {optical, IR, and mm}, we will thus produce the first detailed case study of a thermal pulse, as the star re-traces its evolution across the HR diagram from the AGB to the planetary-nebula phase.

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