THE SPECTRA OF TYPE II CEPHEIDS. I. THE Hα LINE IN SHORT-PERIOD STARS

Authors

Edward G. Schmidt, University of Nebraska-LincolnFollow
Kevin M. Lee, University of Nebraska-LincolnFollow
Dale Johnston, University of Nebraska-LincolnFollow
Peter R. Newman, New Mexico State UniversityFollow
Stephanie A. Snedden, New Mexico State UniversityFollow

Date of this Version

8-1-2003

Comments

Published by the University of Chicago Press. The Astronomical Journal. Copyright 2003 American Astronomical Society. AJ 126, 906(2003). Reproduced by permission of the AAS. Permission to use. http://www.journals.uchicago.edu/AJ/.

Abstract

We present 88 Hα profiles for 24 pulsating variable stars with periods between 1 and 3 days in order to explore the behavior of this line in type II as compared with classical Cepheids. Surprisingly, large velocity differences were found between Hα and the metal lines in some type II Cepheids. Strong emission was observed in three stars, VZ Aql, NW Lyr, and V439 Oph, while line filling by incipient emission is present in seven others. All of the stars with emission and most with incipient emission belong to Diethelm's AHB2 class, and the emission is associated with the secondary bump on the rising branch of the light curve. Two stars, BF Ser and MQ Aql, show doubling of the core near maximum light, and asymmetry of the line is noted in some spectra.