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Evolution of Stellar Activity in Early Post-Main-Sequence Phases

Published online by Cambridge University Press:  12 April 2016

A. Maggio ,
S. Sciortino ,
L. Bianchi ,
F.R. Harnden Jr.  and
R. Rosner
A. Maggio
Affiliation:
Istituto e Osservatorio Astronomico, Palermo, Italy
S. Sciortino
Affiliation:
Istituto e Osservatorio Astronomico, Palermo, Italy
L. Bianchi
Affiliation:
Osservatorio Astronomico di Torino, Italy
F.R. Harnden Jr.
Affiliation:
Harvard-Smithsonian Center for Astrophysics, USA
R. Rosner
Affiliation:
Department of Astronomy and Astrophysics andEnrico Fermi Institute, University of Chicago, USA

Extract

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We present preliminary observational evidences on the variation of the activity level in late type stars, during the evolutionary phases on the main sequence and beyond. We have selected a sample of 51 stars (Fig. 1), lying mostly along evolutionary tracks between 1.3 and 1.7 solar masses, which have been observed in soft X-rays with the Einstein Observatory, and in UV with IUE (Maggio et al. 1990; Haisch et al.1990). Two ROSAT targets, and four new IUE observations are also included.

We find that the radiative emission from the outer atmospheres of stars with M > 1.6M⊙ seems to behave differently than for stars with lower mass.

On the main sequence, the X-ray luminosity of most stars with B-V < 0.42 (spectral type F3) is relatively low, at Lx ~ 3 × 1028erg s-1 (Fig. 2). In the early evolutionary phases beyond the main sequence, the X-ray luminosity of the higher mass stars tend to increase sistematically up to ~ 1030erg s-1, while the lower mass stars show an initial moderate increase followed by a drop, at B-V ~ 0.6, below our sensitivity threshold.

Type
VII. Activity, a break of spherical symmetry
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 648 - 650
Copyright
Copyright © Astronomical Society of the Pacific 1993

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