Formation of globular clusters induced by external ultraviolet radiation
  We present a novel scenario for globular cluster (GC) formation, where the
ultraviolet (UV) background radiation effectively works so as to produce
compact star clusters. Here, we explore the formation of GCs in UV radiation
fields. For this purpose, we calculate baryon and dark matter (DM) dynamics in
spherical symmetry, incorporating the self-shielding effects by solving the
radiative transfer of UV radiation. In addition, we prescribe the star
formation in cooled gas components and pursue the dynamics of formed stars. As
a result, we find that the evolution of subgalactic objects in UV background
radiation are separated into three types, that is, (1) prompt star formation,
where less massive clouds ~10^{5-8} M_sun are promptly self-shielded and
undergo star formation, (2) delayed star formation, where photoionized massive
clouds >10^8 M_sun collapse despite high thermal pressure and are eventually
self-shielded to form stars in a delayed fashion, and (3) supersonic infall,
where photoionized less massive clouds ~10^{5-8} M_sun contract with supersonic
infall velocity and are self-shielded when a compact core forms. In particular,
the type (3) is a novel type found in the present simulations, and eventually
produces a very compact star cluster. The resultant mass-to-light ratios,
half-mass radii, and velocity dispersions for the three types are compared to
the observations of GCs, dwarf spheroidals (dSphs), and ultra-compact dwarfs
(UCDs). It turns out that the properties of star clusters resulting from
supersonic infall match well with those of observed GCs, whereas the other two
types are distinct from GCs. Hence, we conclude that supersonic infall in a UV
background is a promising mechanism to form GCs.
