An Ultra Metal-poor Star Near the Hydrogen-burning Limit
  It is unknown whether or not low-mass stars can form at low metallicity.
While theoretical simulations of Population III (Pop III) star formation show
that protostellar disks can fragment, it is impossible for those simulations to
discern if those fragments survive as low-mass stars. We report the discovery
of a low-mass star on a circular orbit with orbital period P = 34.757 +/- 0.010
days in the ultra metal-poor (UMP) single-lined spectroscopic binary system
2MASS J18082002--5104378. The secondary star 2MASS J18082002--5104378 B has a
mass M_2 = 0.14_{-0.01}^{+0.06} M_Sun, placing it near the hydrogen-burning
limit for its composition. The 2MASS J18082002--5104378 system is on a thin
disk orbit as well, making it the most metal-poor thin disk star system by a
considerable margin. The discovery of 2MASS J18082002--5104378 B confirms the
existence of low-mass UMP stars and its short orbital period shows that
fragmentation in metal-poor protostellar disks can lead to the formation and
survival of low-mass stars. We use scaling relations for the typical fragment
mass and migration time along with published models of protostellar disks
around both UMP and primordial composition stars to explore the formation of
low-mass Pop III stars via disk fragmentation. We find evidence that the
survival of low-mass secondaries around solar-mass UMP primaries implies the
survival of solar-mass secondaries around Pop III primaries with masses 10
M_Sun < M_Star < 100 M_Sun. If true, this inference suggests that solar-mass
Pop III stars formed via disk fragmentation could survive to the present day.
