Stars as Laboratories for Fundamental Physics - MPP Theory Group

Supernova Neutrinos 425
Given these parameters one infers that the number of expected
Kamiokande events is 16.9 plus 5.6 background, 4.0 events at IMB,
and 1.8 plus 1.0 background at Baksan. The inferred best-fit neutrinosphere
radius is 40.2 km, and the inferred total emitted ν e energy is
0.84×10 53 erg which corresponds to a total binding energy of the neutron
star of 5.02×10 53 erg if exact equipartition of the energy among
the neutrino flavors is assumed.
The inferred average neutrino energy, the luminosity-decay time
scale, radius of the source, and total energy emitted all agree reasonably
well with what one expects from a core collapse SN, even though ⟨E νe ⟩
is somewhat low, the radius and inferred binding energy somewhat
large. Of course, all of the inferred quantities carry large uncertainties
because of the sparse data.
Loredo and Lamb (1995) have also considered two-component cooling
schemes where the neutrino signal is modelled to consist of Kelvin-
Helmholtz cooling, plus a low-energy component which mimics the neutrinos
emitted by the accreting matter during the stalled-shock phase
in the delayed-explosion scenario. With more parameters they naturally
find a better fit to the data. More interestingly, the inferred
Fig. 11.16. Two-dimensional marginal distribution for the parameters τ and
⟨E νe ⟩ = 2.13 T 0 of the Kelvin-Helmholtz component of the Loredo and Lamb
(1995) best-fit two-component cooling model. The parameters τ and T 0 are
those of a displaced power law as described in the text. (Curves courtesy of
Tom Loredo, taken from Loredo and Lamb 1995.)