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Near-UV nebular absorption lines of η Carinae

Published online by Cambridge University Press:  26 May 2016

Theodore R. Gull ,
Gladys L. Vieira  and
Anthony C. Danks
Theodore R. Gull
Affiliation:
NASA's Goddard Space Flight Center, Code 681, Greenbelt, MD 20771, USA
Gladys L. Vieira
Affiliation:
NASA's Goddard Space Flight Center, Code 681, Greenbelt, MD 20771, USA
Anthony C. Danks
Affiliation:
NASA's Goddard Space Flight Center, Code 681, Greenbelt, MD 20771, USA

Abstract

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The notorious η Carinae was observed with the stis from 2380 Å to 3160 Å with a resolving power of ~ 130000. Over 500 absorption lines have been identified as originating from Fe i, Fe ii, Ti ii, V ii, Cr ii, Ni ii, Co ii, Mn ii, Mg i and Mg ii. Most of the lines have multiple components ranging from −145kms–1, –385kms–1 to –587kms–1. Many interstellar absorption velocity systems, also found in the spectra of other Carina stars, are seen in the spectrum of η Car. While ISM absorption lines originate from the ground energy level, the nebular lines originate from energy levels well above the ground state. We are still evaluating the origin and location of these velocity systems in line of sight.

Type
Part 1. Atmospheres of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 196 - 197
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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