A Long-lived Disk around the Red Rectangle?

Details A Long-lived Disk around the Red Rectangle? A Long-lived Disk around the Red Rectangle?

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...453..721j&link_type=abstract

Astrophysical Journal v.453, p.721

Astronomy and Astrophysics

Astronomy

76

Stars: Circumstellar Matter, Ism: Individual Name: Red Rectangle, Radio Lines: Ism

Scientific paper

We report high signal-to-noise ratio radio CO emission from the circumstellar envelope around the Red Rectangle. The CO (2-1) line displays a narrow central spike with an FWHM ˜ 2 km s-1, which is much narrower than the circumstellar CO lines typically found around most mass-losing red giants. In addition, instead of the sharp edges expected for a spherical envelope, the lines show extended blueshifted and redshifted wings, with a full width at zero intensity of 12 km s-1, consistent with a bipolar distribution. The circumstellar CO traces the center of mass of the system rather than the binary motion of HD 44179, the optically visible star in the Red Rectangle. There appears to have been significant de-acceleration of the gas ejected from the mass-losing star; the observed CO emission may result from a bipolar outflow from a disk that is viewed edge-on. We suggest that much of the material around the Red Rectangle resides in a long-lived configuration, such as a gravitationally bound disk.
Because the material may dwell for a long time near the binary system, the resulting substantial processing and evolution may explain why the circumstellar matter is so different around the Red Rectangle compared to that around AFGL 2688, another post-main-sequence bipolar nebula. We speculate that large carbon particles similar to the grains up to 20 microns in diameter found in the solar system might grow around the Red Rectangle.

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