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Pre-main-sequence variable stars
2007In section 2.19, we outlined what was presently known about star formation, and the early evolution of stars. There are several types of variability which are specifically or predominantly found among young stars. Most or all of these would be found in a given star, such as the sun, at various times in its pre-main-sequence (PMS) lifetime.
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Pre-Main-Sequence Stages of Stars
Publications of the Astronomical Society of Japan, 1965Abstract Evolutionary model sequences of gravitationally contracting stars were calculated for masses, 0.4, 0.6, 1.0, 1.5, 2.0 and 3.0 M⊙, by using the surface condition based on the conventional mixing length theory of convection and assuming the contraction to be homologous. The mixing length was assumed to be equal to 1-pressure scale
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Asteroseismology of pre-main sequence stars
2008More than 30 years ago the first pulsating pre-main sequence (PMS) stars have been discov- ered. Since then, pulsations in 18 Herbig Ae stars and 18 members of young open clusters were detected and detailed asteroseismic investigations were conducted for some of them. We describe our latest results in this field.
Zwintz, Konstanze +2 more
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PHOTOMETRIC VARIABILITY OF PRE-MAIN SEQUENCE STARS
BOOK OF ABSTRACTS: XIV Serbian-Bulgarian Astronomical ConferenceFor several decades we have been performing photometric monitoring of some of the star formation regions. A significant part of our program is focused on young variable stars, such as FU Orionis, EX Lupi and UX Orionis objects. These three types of young variable stars show changes in brightness with large amplitudes and attract the attention of star ...
Evgeni Semkov +3 more
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Disk accretion in pre-main sequence stars
AIP Conference Proceedings, 1998This paper provides an overview of the observations which support the presence of accretion in disks around pre-main sequence stars and of the characteristics of accretion inferred from their interpretation. The main properties of outbursting, high mass accretion disks, the FU Orionis objects, are summarized. Accretion in the Classical T Tauri stars is
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The Evolution of Pre-Main-Sequence Stars
1999The location of optically visible Pre-Main-Sequence (PMS) stars in the H-R diagram combined with the use of theoretical evolutionary tracks have played a central role in stellar evolution studies since the initial work of Hayashi, Cameron and Iben in the early ′60s.
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The Nearest Pre-Main Sequence Multiple Stars
2007Protoplanetary disks are where planets form, and where the pre-biotic materials which produce life-bearing worlds are assembled or produced. We need to understand them, how they interact with their central stars, and their evolution both to reconstruct the Solar System’s history, and to account for the observed diversity of exo-planetary systems.
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Proper Motions of Pre-Main Sequence Stars
2014The kinematic study of young stars is an important tool to discuss the early stages of star formation. In this context, proper motions allow us to detect moving group structures of young stars to which they belong. Individual distances to moving group members can be inferred from proper motion and radial velocity data using the convergent point ...
Ferreira, A. C. S., +5 more
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