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Pulsation in pre-main sequence stars

Published online by Cambridge University Press:  27 October 2016

Konstanze Zwintz
Konstanze Zwintz*
Affiliation:
Institute for Astro- and Particle Physics, University of Innsbruck Technikerstrasse 25/8, A-6020 Innsbruck, Austria email: [email protected]
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Abstract

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Asteroseismology has been proven to be a successful tool to unravel details of the internal structure for different types of stars in various stages of evolution well after birth. We can now show that it has similar power for pre-main sequence (pre-MS) objects. Pre-MS stars with masses between ~1 and 6 solar masses that have recently been formed and gain their energy mainly from gravitational contraction can become vibrationally unstable during their evolution to the main sequence. Within the past ~15 years, several dozens of pulsating pre-MS stars were discovered using data obtained from ground and from space. Depending on their masses, pre-MS stars can show three different types of pulsations: (i) δ Scuti type p-mode pulsations, (ii) γ Doradus like g-mode oscillations and (iii) g-mode Slowly Pulsating B star pulsations.

Our asteroseismic investigations yielded new insights into the connection between the pulsations and early stellar evolution: We revealed a relation between the stars' oscillatory behavior and their relative evolutionary stages that might lead us to a model-independent determination of the stars' fundamental parameters. With this we will be able to put constraints on theoretical models and help to answer some of the yet open questions in early stellar evolution.

Keywords

asteroseismologystars: early typestars: pre-main sequencestars: variables: δ Scutistars: oscillationsstars: fundamental parameters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 552 - 559
Copyright
Copyright © International Astronomical Union 2016 

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