New methods for determining the ages of PMS stars
Proceedings of the International Astronomical Union
Cambridge University Press (CUP) for International Astronomical Union (IAU)
© International Astronomical Union 2009
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 tau-squared 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.
This is the author accepted manuscript. The final version is available from the publisher via the DOI in this record.
Volume 4, Issue S258, pp. 103-110