2008/03/31 by J. D. Hartman, B. S. Gaudi, M. H. Pinsonneault +6 · 1 citation
Physics and Astronomy · Social Sciences · #Angular momentum #Astronomy and Astrophysical Research #Cluster (spacecraft) #Educational Leadership and Practices #Open cluster #Planet #Pleiades #Rotation (mathematics) #Star cluster #Stars #Stellar rotation #Stellar, planetary, and galactic studies #Transit (satellite) #astro-ph
paper · pdf · doi:10.1088/0004-637x/691/1/342
published as Astrophys.J.691:342-364,2009 · Replaced with version accepted to ApJ. 104 pages, 7 tables, 26 figures
arxiv created 2008/09/22 · openalex publication_date 2009/01/14 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
In the course of conducting a deep (14.5 ≲ r ≲ 23), 20 night survey for transiting planets in the rich ∼550 Myr old open cluster M37, we have measured the rotation periods of 575 stars, which lie near the cluster main sequence, with masses 0.2 M ☉ ≲ M ≲ 1.3 M ☉ . This is the largest sample of rotation periods for a cluster older than 500 Myr. Using this rich sample we investigate a number of relations between rotation period, color, and the amplitude of photometric variability. Stars with M ≳ 0.8 M ☉ show a tight correlation between period and mass with heavier stars rotating more rapidly. There is a group of four stars with P > 15 days that fall well above this relation, which, if real, would present a significant challenge to theories of stellar angular momentum evolution. Below 0.8 M ☉ , the stars continue to follow the period–mass correlation but with a broad tail of rapid rotators that expands to shorter periods with decreasing mass. We combine these results with observations of other open clusters to test the standard theory of lower main-sequence stellar angular momentum evolution. We find that the model reproduces the observations for solar-mass stars, but discrepancies are apparent for stars with 0.6 ≲ M ≲ 1.0 M ☉ . We also find that for late K through early M dwarf stars in this cluster, rapid rotators tend to be bluer than slow rotators in B − V but redder than slow rotators in V − I C . This result supports the hypothesis that the significant discrepancy between the observed and predicted temperatures and radii of low-mass main-sequence stars is due to stellar activity.