Abstract / Description of output
We show that hard encounters in the central regions of globular clusters
embedded in dark matter (DM) haloes necessarily lead to the formation of
gravitationally-bound stellar envelopes that extend far beyond the
nominal tidal radius of the system. Using statistical arguments and
numerical techniques we derive the equilibrium distribution function of
stars ejected from the centre of a non-divergent spherical potential.
Independently of the velocity distribution with which stars are ejected,
GC envelopes have density profiles that approach asymptotically
$\rho\sim r^{-4}$ at large distances and become isothermal towards the
centre. Adding a DM halo component leaves two clear-cut observational
signatures: (i) a flattening, or slightly increase of the projected
velocity dispersion profile at large distances, and (ii) an outer
surface density profile that is systematically shallower than in models
with no dark matter.
Original language | English |
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Pages (from-to) | L31-L35 |
Journal | Monthly Notices of the Royal Astronomical Society: Letters |
Volume | 471 |
Issue number | 1 |
DOIs | |
Publication status | Published - 15 Jun 2017 |
Keywords / Materials (for Non-textual outputs)
- Astrophysics - Astrophysics of Galaxies