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New methods for determining the ages of PMS stars

Published online by Cambridge University Press:  01 October 2008

Tim Naylor ,
N. J. Mayne ,
R. D. Jeffries ,
S. P. Littlefair  and
Eric S. Saunders
Tim Naylor
Affiliation:
School of Physics, University of Exeter Stocker Road, Exeter, EX4 4QL, UK.
N. J. Mayne
Affiliation:
School of Physics, University of Exeter Stocker Road, Exeter, EX4 4QL, UK.
R. D. Jeffries
Affiliation:
Astrophysics Group, School of Physical and Geographical Sciences, Keele University, Keele, Staffordshire ST5 5BGUK.
S. P. Littlefair
Affiliation:
Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH, UK.
Eric S. Saunders
Affiliation:
Las Cumbres Observatory Global Telescope network, 6740 CortonaDrive, Suite 102, Goleta, CA93117, USA
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Abstract

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We present three new methods for determining the age of groups of pre-main-sequence stars. The first, creating empirical isochrones allows us to create a robust age ordering, but not to derive actual ages. The second, using the width of the gap in colour-magnitude space between the pre-main-sequence and main-sequence (the radiative convective gap) has promise as a distance and extinction independent measure of age, but is as yet uncalibrated. Finally we discuss τ2 fitting of the main sequence as the stars approach the terminus of the main sequence. This method suggests that there is a factor two difference between these “nuclear” ages, and more conventional pre-main-sequence contraction ages.

Keywords

methods: statisticalmethods: data analysisstars: pre–main-sequence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S258: The Ages of Stars , October 2008 , pp. 103 - 110
Copyright
Copyright © International Astronomical Union 2009

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