Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003csss...12..834d&link_type=abstract
The Future of Cool-Star Astrophysics: 12th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (2001 July 30 - August
Astronomy and Astrophysics
Astrophysics
M 67, Rotation, Angular Momentum
Scientific paper
On the basis of accurate projected rotational velocity v sin i for 28 main sequence, turnoff and giant stars, we study the evolution of the angular momentum in old open cluster M 67. >From these data, we show that early main sequence G stars have rotational velocity two times larger the Sun, with a possible trend with (bv) color, in that redder colors correspond to lower v sin i. The stars at the turnoff are the fastest rotators, with v sin i between 6.3 and 7.6
km s-1, while stars just above the turnoff are already significantly slower. Along the Red Giant Branch rotation decreases smoothly and for stars redder than (bv)⪆ 1, only upper limits can be found, including 4 clump stars. Analyzing the angular momentum history of 1.2 Msun stars with the help of theoretical evolutionary tracks, we see that these stars probably obey different angular momentum evolution laws on the main sequence and along the Red Giant Branch: while on the main sequence some extra braking is required, in addition to angular momentum conservation, along the Red Giant Branch the data are well represented by the IΩ=C law. Finally, comparing the rotational velocity of the M 67 turnoff stars with their main sequence progenitors in younger open clusters, we find that younger clusters show substantially higher rotation rates, indicating that 1.2 Msun stars do experience main sequence braking.
de Medeiros Jose Renan
Melo H. F. C.
Pasquini Luca
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