Understanding the Red Rectangle and its central binary HD 44179

Details Understanding the Red Rectangle and its central binary HD 44179 Understanding the Red Rectangle and its central binary HD 44179

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7297v&link_type=abstract

HST Proposal ID #7297

Mathematics

Logic

Hst Proposal Id #7297 Stellar Ejecta

Scientific paper

The ``Red Rectangle'' is one of the nearest and best known of the proto-planetary nebulae. The central star {HD 44179} has recently left the AGB {within the past several hundred years} by ejecting a dense, dusty disk and surrounding optical and molecular envelope, and is now passing through spectral type A on its rapid evolution to higher temperatures. Moreover, the central star is a spectroscopic binary with a period of 319 days. We propose to exploit the high spatial resolution and coronographic capabilities of the WFPC2 and STIS instruments to investigate the molecule and dust formation processes in the Red Rectangle nebula and the influence of the changing nebular conditions on these processes from the inner dust disk to the outer regions. Our objective is to limit the potential identifications of the carriers of the many unique, and still unidentified, emission features in the optical spectrum of the nebula, through detailed morphological and spectroscopic studies of their spatial and spectral characteristics.

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