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2011MNRAS.416..447S - Mon. Not. R. Astron. Soc., 416, 447-456 (2011/September-1)
Modelling the rotational evolution of solar-like stars: the rotational coupling time-scale.
SPADA F., LANZAFAME A.C., LANZA A.F., MESSINA S. and COLLIER CAMERON A.
Abstract (from CDS):
A power-law dependence of τc on the inner differential rotation leads to a more satisfactory agreement with observations than a two-valued prescription for τc, which would imply a dichotomy between the initially slow (Prot ≳ 3 d) and fast (Prot ≲ 3 d) rotators. However, we find it impossible to reconcile the high fraction of fast rotators in α Per with the rotation period distributions in stellar systems at earlier and later evolutionary stages. This could be explained by local environmental effects (e.g. early removal of circumstellar discs due to ultraviolet radiation and winds from nearby high-mass stars) or by observational biases.
The low KS probability that the synthetic and observed distributions are not incompatible, found in some cases, may be due to oversimplified assumptions of the double-zone model, but the large relative uncertainties in the age determination of very young clusters and associations are expected to play a relevant role. Other possible limitations and uncertainties are discussed.
Abstract Copyright: 2011 The Authors Monthly Notices of the Royal Astronomical Society2011 RAS
Journal keyword(s): methods: numerical - stars: interiors - stars: late-type - stars: pre-main-sequence - stars: rotation
Simbad objects: 18
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