Proc. Neutrino Astrophysics - MPP Theory Group

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Figure 4: SN 1987A bounds on FCNC neutrino interactions.
Figure 5: Supernovae and FCNC neutrino interactions. R-process.
tory. In Fig. 4 we display the SN 1987A constraints on explicit R-parity-violating FCNCs in
the presence of non-zero neutrino masses in the hot dark matter eV range. In Fig. 5 we display
the sensitivity of the r-process argument to the presence of FCNC neutrino interactions.
Taken altogether, Fig. 4 and Fig. 5 disfavour a leptoquark interpretation of the recent HERA
anomaly.
As a final example of how astrophysics can constrain neutrino properties we consider
the case of resonant νe → νs and ¯νe → ¯νs conversions in supernovae, where νs is a sterile
neutrino [25], which we assume to be in the hot dark matter mass range. The implications
of such a scenario for the supernova shock re-heating, the detected ¯νe signal from SN 1987A
and for the r-process nucleosynthesis hypothesis have been recently analysed [25]. In Fig. 6,