Seismic study of stellar convective regions: the base of the convective envelope in low-mass stars

• Type: Article in International Scientific Journal
• Date: 2000

Authors

Monteiro, MJPFG (Author) FCUP; Christensen Dalsgaard, J (Author) Other; Thompson, MJ (Author) Other

Journal

Title: Monthly Notices of the Royal Astronomical Society

Vol. 316

Pages: 165-172

ISSN: 0035-8711

Publisher: Oxford University Press

Indexing

ISI Web of Knowledge - 87 Citations

Scopus - 85 Citations

Scientific classification

FOS: Natural sciences > Physical sciences

Other information

Authenticus ID: P-000-ZG7

DOI: 10.1046/j.1365-8711.2000.03471.x

Abstract (EN): The possibility of observing solar-type oscillations on other stars is of great relevance to investigating the uncertain aspects of the internal structure of stars. One of these aspects is the convective overshoot that takes place at the borders of the envelopes of stars of mass similar to, or lower than, the Sun. It affects the temperature stratification, mixing, rotation and magnetic-field generation. Asteroseismology can provide an observational test for the studies of the structure of such overshoot regions. The seismic study of the transition in the Sun, located at the base of the convection zone, has been successful in determining the characteristics of this layer in the Sun. In this work we consider the extension of the analysis to other solar-type stars (of mass between 0.85 and 1.2 M.) in order to establish a method for determining the characteristics of their convective envelopes. In particular, we hope to be able to establish seismologically that a star does indeed possess a convective envelope, to measure the size of the convective region and also to constrain the properties of an overshoot layer at the bottom of the envelope. The limitations in terms of observational uncertainties and stellar characteristics, and the detectability of an overshoot layer, are discussed.

Language: English

Type (Professor's evaluation): Scientific

No. of pages: 8