Rotation, Planets, and the "Second Parameter" of the Horizontal Branch

Abstract

We analyze the angular momentum evolution from the red giant branch (RGB) to the horizontal branch (HB) and along the HB. Using rotation velocities for stars in the globular cluster M13, we find that the required angular momentum for the fast rotators is up to 1-3 orders of magnitude (depending on some assumptions) larger than that of the sun. Planets of masses up to five times Jupiter's mass and up to an initial orbital separation of about 2 AU are sufficient to spin-up the RGB progenitors of most of these fast rotators. Other stars have been spun-up by brown dwarfs or low-mass main sequence stars. Our results show that the fast rotating HB stars must have been spun-up by companions while they evolved on the RGB. The angular momentum considerations presented in this paper further supports the "planet second parameter" model. In this model the "second parameter" process is interaction with low-mass companions, in most cases gas giant planets, and in a minority of cases with brown dwarfs or low-mass main sequence stars.

15 pages + 1 figure (postscript), Submitted to MNRAS

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