dc.contributor.author | Naylor, T | |
dc.contributor.author | Mayne, NJ | |
dc.contributor.author | Jeffries, RD | |
dc.contributor.author | Littlefair, SP | |
dc.contributor.author | Saunders, ES | |
dc.date.accessioned | 2018-01-04T14:07:23Z | |
dc.date.issued | 2008-10 | |
dc.description.abstract | 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. | en_GB |
dc.identifier.citation | Volume 4, Issue S258, pp. 103-110 | en_GB |
dc.identifier.doi | 10.1017/S1743921309031755 | |
dc.identifier.uri | http://hdl.handle.net/10871/30827 | |
dc.language.iso | en | en_GB |
dc.publisher | Cambridge University Press (CUP) for International Astronomical Union (IAU) | en_GB |
dc.rights | © International Astronomical Union 2009 | en_GB |
dc.subject | methods: statistical | en_GB |
dc.subject | methods: data analysis | en_GB |
dc.subject | stars: pre–main-sequence | en_GB |
dc.title | New methods for determining the ages of PMS stars | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2018-01-04T14:07:23Z | |
dc.description | This is the author accepted manuscript. The final version is available from the publisher via the DOI in this record. | en_GB |
dc.identifier.journal | Proceedings of the International Astronomical Union | en_GB |