dc.contributor.author |
Balachandran, S. C |
|
dc.contributor.author |
Mallik, S. G. V |
|
dc.contributor.author |
Lambert, D. L |
|
dc.date.accessioned |
2011-03-01T12:30:42Z |
|
dc.date.available |
2011-03-01T12:30:42Z |
|
dc.date.issued |
2011-02 |
|
dc.identifier.citation |
Monthly Notices of the Royal Astronomical Society, Vol. 410, No. 4, pp. 2526–2539 |
en |
dc.identifier.uri |
http://hdl.handle.net/2248/5404 |
|
dc.description |
Restricted Access |
en |
dc.description.abstract |
Lithium (Li) abundances are presented and discussed for 70 members of the 50-Myr-old open cluster α Per. More than half of the abundances are from new high-resolution spectra. The Li abundance in the F-type stars is equal to its presumed initial abundance, confirming previous suggestions that pre-main-sequence depletion is ineffective for these stars. Intrinsic star-to-star scatter in Li abundance among these stars is comparable to the measurement uncertainties. There is marginal evidence that the stars of high projected rotational velocity (v sin i) follow a different abundance versus temperature trend from the slow rotators. For stars cooler than about 5500 K, the Li abundance declines steeply with decreasing temperature and there develops a star-to-star scatter in the Li abundance. This scatter is shown to resemble the well-documented scatter seen in the 70-Myr-old Pleiades cluster. The scatter appears to be far less pronounced in the 30-Myr clusters, which have been studied for Li abundance. |
en |
dc.language.iso |
en |
en |
dc.publisher |
Wiley Blackwell |
en |
dc.relation.uri |
http://dx.doi.org/10.1111/j.1365-2966.2010.17630.x |
en |
dc.rights |
© John Wiley & Sons |
en |
dc.subject |
Stars: abundances |
en |
dc.subject |
Open clusters and associations |
en |
dc.subject |
Individual: α Per |
en |
dc.title |
Lithium abundances in the α Per cluster |
en |
dc.type |
Article |
en |