Are pre-MS stars older than we thought?

dc.contributor.author	Naylor, T
dc.contributor.author	Mayne, NJ
dc.date.accessioned	2018-01-04T13:59:01Z
dc.date.issued	2010-10-21
dc.description.abstract	We present a consistent age ordering for young clusters and groups determined using the contraction of stars through their pre-main-sequence phase. We compare these with ages derived from the evolution of the upper main-sequence stars, and find the upper MS ages are older by a factor 1.5 to 2. We show that increasing the binary fraction and number of equal-mass binaries amongst the O-stars compared to the rest of the MS cannot remove this discrepancy.	en_GB
dc.identifier.doi	10.1017/S1743921310011476
dc.identifier.uri	http://hdl.handle.net/10871/30826
dc.language.iso	en	en_GB
dc.publisher	Cambridge University Press (CUP) for International Astronomical Union (IAU)	en_GB
dc.rights	© International Astronomical Union 2010	en_GB
dc.subject	methods: statistical	en_GB
dc.subject	stars: formation	en_GB
dc.subject	open clusters and associations: general	en_GB
dc.title	Are pre-MS stars older than we thought?	en_GB
dc.type	Article	en_GB
dc.date.available	2018-01-04T13:59:01Z
dc.description	Special Session 7, IAU XXVII General Assembly	en_GB
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	Vol. 5 issue H15, p. 763	en_GB