Almog Yalinewich
Norm's group meeting 24.10.19
Eddington lifetime
Hydrostatic equilibrium
Instability when
Massive stars are radiative
At high masses, GR effects become important
Helium burning temperature
Eddington luminosity
Stars cannot support themselves if
In the range
Synthetic population
Stellar structure
Semi empirical relations
BSE
Neutron stars can explain all ULX
No need for intermediate mass black holes
A sizeable fraction of the companions are He stars