The Nature of the AM Canum Venaticorum Variables, the Cataclysmic-Db White Dwarf Connection?

Details The Nature of the AM Canum Venaticorum Variables, the Cataclysmic-Db White Dwarf Connection? The Nature of the AM Canum Venaticorum Variables, the Cataclysmic-Db White Dwarf Connection?

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6085s&link_type=abstract

HST Proposal ID #6085

Computer Science

Hst Proposal Id #6085 Hot Stars

Scientific paper

The fundamental nature of the AM Canum Venaticorum (AM CVn) objects remains a mystery. Unlike their helium purity in the optical, far UV spectra of AM CVn objects reveal a broad mix of metal absorption features and He II (1640). We propose two GHRS observations of AM CVn to gain fundamental insight: (1) a single GHRS G140L exposure in RAPID mode with a spectrum every 20 seconds (over 2.5 cycles of the 1120s period= 46 minutes) delivering the first rapid time-resolved monitoring of the far UV line profiles and continuum levels over the range of the putative rotational/orbital periods (175s~1100s) reported for the systems and; (2) a single deep exposure with GHRS G160M in ACCUM mode to secure and model the first fully-resolved line profile for the complex He II (1640) region and detect circumbinary/circumstellar features. Are they really helium- transferring binary white dwarfs or single (merged?) rotating degenerates? Do they manifest wind outflow in the far UV? Are they related to the helium-rich DO/DB degenerates? Are they surrounded by circumstellar/circumbinary shells? What is the rotation rate of the underlying hot degenerate? A single very noisy, 15 hour IUE HIRES image of AM CVn (Solheim and Sion 1994, A&A (Letters), in press) revealed evidence for a hot circumbinary/circumstellar shell and a strong, complex asymmetric He II (1640) profile with broad emission reversal, remarkably similar to the He II (1640) profile structure of the "cool" DO star HZ21.

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