Modelling chromospheric line profiles in NGC 2808: evidence of mass loss from RGB stars

¹ Instituto de Astronomía y Física del Espacio, Buenos Aires, Argentina e-mail: pablo@iafe.uba.ar
² INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: carla.cacciari@bo.astro.it
³ European Southern Observatory, Karl-Schwarzschild-Str. 2, 85749 Garching b. München, Germany e-mail: lpasquin@eso.org

Received: 30 December 2005
Accepted: 21 March 2006

Abstract

In this study we test the possibility that the asymmetry in the profiles of the Hα and Ca ii K lines in red giant stars is due to the presence of an active chromosphere rather than to mass loss. To this end, we compare line profiles computed using relevant model chromospheres to profiles of the Hα and Ca ii K lines observed in five red giant stars of the globular cluster NGC 2808. The spectra were taken with FLAMES during the science verification, using the UVES mode at high resolution ( 000) for the Hα line, and GIRAFFE in MEDUSA mode () for the Ca ii K line. We find that the observed profiles are better described if a negative (outward) velocity field is included in the model chromospheres. This leads to mass loss rates of a few 10^-9  yr^-1, so very close to the requirements of the stellar evolution theory.