Abstract
We estimate the rate of collisions between stars and free-floating planets (FFPs) in globular clusters, in particular, the collision of FFPs with red giant branch (RGB) stars. Recent dynamical simulations imply that the density of such objects could exceed ∼106 pc -3 near the cores of rich globular clusters. We show that in these clusters ∼5%-10% of all RGB stars near the core would suffer a collision with an FFP and that such a collision can spin up the RGB star's envelope by an order of magnitude. In turn, the higher rotation rates may lead to enhanced mass-loss rates on the RGB, which could result in bluer horizontal branch (HB) stars. Hence, it is plausible that the presence of a large population of FFPs in a globular cluster can influence the distribution of stars on the HB of that cluster to a detectable degree.
Original language | English |
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Pages (from-to) | L87-L90 |
Journal | Astrophysical Journal |
Volume | 563 |
Issue number | 1 PART 2 |
DOIs | |
State | Published - 10 Dec 2001 |
Keywords
- Globular clusters: General
- Planetary systems
- Stars: General
- Stars: Horizontal-branch
- Stars: Mass loss
- Stars: Rotation