Using time-of-flight delays of the three neutrino mass eigenstates across sharp supernova features, a galactic supernova at 10 kpc could individually constrain or measure neutrino masses at JUNO, with precision that depends strongly on the assumed mass scale.
What is $\Delta m^2_{ee}$ ?
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abstract
The current short baseline reactor experiments, Daya Bay and RENO (Double Chooz) have measured (or are capable of measuring) an effective $\Delta m^2$ associated with the atmospheric oscillation scale of 0.5 km/MeV in electron anti-neutrino disappearance. In this paper, I compare and contrast the different definitions of such an effective $\Delta m^2$ and argue that the simple, L/E independent, definition given by $\Delta m^2_{ee} \equiv \cos^2 \theta_{12} \Delta m^2_{31}+ \sin^2 \theta_{12} \Delta m^2_{32}$, i.e. "the $\nu_e$ weighted average of $\Delta m^2_{31}$ and $\Delta m^2_{32}$," is superior to all other definitions and is useful for both short baseline experiments mentioned above and for the future medium baseline experiments JUNO and RENO 50.
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Individual Neutrino Masses From a Supernova
Using time-of-flight delays of the three neutrino mass eigenstates across sharp supernova features, a galactic supernova at 10 kpc could individually constrain or measure neutrino masses at JUNO, with precision that depends strongly on the assumed mass scale.