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V605 Aql: 80 Years after the Final Helium Shell Flash

Published online by Cambridge University Press:  15 December 2006

Geoffrey C. Clayton ,
J. M. Fedrow ,
P. A. Crowther ,
F. Kerber ,
N. Pirzkal  and
O. De Marco
Geoffrey C. Clayton
Affiliation:
Department of Physics & Astronomy, Louisiana State University, Baton Rouge, LA 70803 email:gclayton@fenway.phys.lsu.edu Maria Mitchell Observatory, Maria Mitchell Association, 3 Vestal Street, Nantucket MA 02554
J. M. Fedrow
Affiliation:
Maria Mitchell Observatory, Maria Mitchell Association, 3 Vestal Street, Nantucket MA 02554 The Evergreen State College, 2700 Evergreen Parkway NW, Olympia, Washington 98505 email:v605aql@yahoo.com
P. A. Crowther
Affiliation:
Department of Physics & Astronomy, University of Sheffield, Hicks Building, Hounsfield Rd, Sheffield, S3 7RH, UK email:paul.crowther@sheffield.ac.uk
F. Kerber
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Strae 2, D-85748 Garching, Germany email:fkerber@eso.org
N. Pirzkal
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Strae 2, D-85748 Garching, Germany email:fkerber@eso.org STScI, 3700 San Martin Dr., Baltimore, MD 21218; email:npirzkal@eso.org
O. De Marco
Affiliation:
Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024 email:orsola@amnh.org
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Abstract

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We have obtained new optical spectra with the ESO/VLT of the final helium flash star, V605 Aql. These spectra indicate that V605 Aql has evolved significantly in only 80 years. It now has a T$_{\rm eff}\sim$95,000 K and has abundances similar to those seen in [WC] central stars but not to those of a typical RCB star.

Keywords

stars: evolutionabundancesAGB and post-AGB
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 379 - 380
Copyright
© 2006 International Astronomical Union