Midterm II:† Suggested
Study Problems, in no particular order
explicitly that an isothermal, monatomic ideal gas will not be
the Luminosity-Core Temperature homology relations for UMS and LMS stars.
that the 1 solar mass core of a 10 solar mass star collapses to produce a
Type II supernova.† Assume further
that all of the energy released by the collapsing core is converted to
neutrinos and that 1% of the neutrinos are
absorbed by the overlying envelope to power the ejection of the supernova
remnant.† Estimate the final radius
of the stellar remnant if sufficient energy is to be liberated to just
barely eject the remaining 9 solar masses to infinity.
the gravitational binding energy of a neutron star with a mass of 1.4
solar masses and a radius of 10 km.†
Compare your answer with the amount of energy released in neutrinos
the exact expression for electron degeneracy pressure (for the nonrelativistic case) to derive the degeneracy
condition discussed in lecture.†
Discuss the evolution of the Sun in the log(r)-log(T) plane.
the Sun were to collapse into a neutron star.† Find the resultant rotation period and
magnetic field strength.† Compare
the rotation (before and after) to the breakup rotation period for the
is the transmitted intensity of light through a cloud in the optically
thin and optically thick limits?†
How do these change if the cloud emits
light as well as absorbs light?
some or all of Keplerís laws to estimate the free-fall time for a cloud
external magnetic field contributes a pressure term to the Virial Equation
that can help induce the collapse of a cloud that would, in the absence of
the external pressure and magnetic field, be in hydrostatic balance.† If the external magnetic pressure is
given by B2/8p, retrace
the arguments for a maximum external gas pressure before cloud collapse
(as in HW 4).† How might this change
if there is a uniform internal
magnetic field that supports the cloud against collapse instead?
an expression for the centrifugal radius of a slowly rotating cloud that
collapses to form a protoplanetary disk.†
Given some typical parameter ranges, how big is the resulting
protoplanetary disk for the protosun?