Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.6702h&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #67.02; Bulletin of the American Astronomical Society, Vol. 24, p.1227
Astronomy and Astrophysics
Astronomy
Scientific paper
Observations are presented that show that the G5 Ia supergiant AFGL 2343 (HD 179821) is extended at 10.5 and 12.5 microns. The observations were made with the Berkeley/IGPP 10 microns array camera on the UKIRT on Mauna Kea, Hawaii in June 1992. AFGL 2343 has about the coldest IRAS colors of any evolved star with detected CO emission. The energy distribution is double-peaked, with peaks in the optical (8.3 V mag) and far-infrared between 25 and 60 microns. The 10 microns images show that the shell around AFGL 2343 is very cold, appearing at 10.5 and 12.5 microns but not at 8.5 microns. The central star is visible at 8.5 microns and 10.5 microns, but is barely visible at 12.5 microns. The shell appears as a circular ring with 4'' diameter, with bright spots in the North and Eastern sections of the nebula. A color-temperature map made from the 10.5 and 12.5 microns images shows an almost bipolar morphology, with the axis of cold dust lying along the semi-major axis of extended elliptical CO emission seen by Bujarrabal, Alcolea, and Planesas (1992 AA 257, 701.). AFGL 2343 is either a very slowly evolving protoplanetary nebula, or is a mass loss precursor to a supernova. The latter interpretation is supported by the large angular extent, the large mass loss rate of the shell (10(-3) Msun yr(-1) ) and total mass of the remnant (0.5 - 7 Msun at 1.5 - 6 kpc), and the probable high mass of the central star, based on the high 34 km sec(-1) CO expansion velocity of the envelope.
Arens John F.
Graham James
Hawkins G. W.
Jernigan Garret J.
Keto Eric
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