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dc.contributor.authorNaylor, T
dc.contributor.authorMayne, NJ
dc.contributor.authorJeffries, RD
dc.contributor.authorLittlefair, SP
dc.contributor.authorSaunders, ES
dc.date.accessioned2018-01-04T14:07:23Z
dc.date.issued2008-10
dc.description.abstractWe 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.citationVolume 4, Issue S258, pp. 103-110en_GB
dc.identifier.doi10.1017/S1743921309031755
dc.identifier.urihttp://hdl.handle.net/10871/30827
dc.language.isoenen_GB
dc.publisherCambridge University Press (CUP) for International Astronomical Union (IAU)en_GB
dc.rights© International Astronomical Union 2009en_GB
dc.subjectmethods: statisticalen_GB
dc.subjectmethods: data analysisen_GB
dc.subjectstars: pre–main-sequenceen_GB
dc.titleNew methods for determining the ages of PMS starsen_GB
dc.typeArticleen_GB
dc.date.available2018-01-04T14:07:23Z
dc.descriptionThis is the author accepted manuscript. The final version is available from the publisher via the DOI in this record.en_GB
dc.identifier.journalProceedings of the International Astronomical Unionen_GB


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