Flavor Transformations: snewpy.flavor_transformation¶
This module implements flavor transformations that describe how neutrinos of different flavors change into each other between production inside the supernova and detection on Earth.
Base Class for Flavor Transformations¶
- class snewpy.flavor_transformation.FlavorTransformation[source]¶
Generic interface to compute neutrino and antineutrino survival probability.
- abstract prob_ee(t, E)[source]¶
Electron neutrino survival probability.
- Parameters:
t (float or ndarray) – List of times.
E (float or ndarray) – List of energies.
- Returns:
float or ndarray – Transition probability.
- abstract prob_eebar(t, E)[source]¶
Electron antineutrino survival probability.
- Parameters:
t (float or ndarray) – List of times.
E (float or ndarray) – List of energies.
- Returns:
float or ndarray – Transition probability.
- abstract prob_ex(t, E)[source]¶
X -> e neutrino transition probability.
- Parameters:
t (float or ndarray) – List of times.
E (float or ndarray) – List of energies.
- Returns:
float or ndarray – Transition probability.
- abstract prob_exbar(t, E)[source]¶
X -> e antineutrino transition probability.
- Parameters:
t (float or ndarray) – List of times.
E (float or ndarray) – List of energies.
- Returns:
float or ndarray – Transition probability.
- abstract prob_xe(t, E)[source]¶
e -> X neutrino transition probability.
- Parameters:
t (float or ndarray) – List of times.
E (float or ndarray) – List of energies.
- Returns:
float or ndarray – Transition probability.
- abstract prob_xebar(t, E)[source]¶
e -> X antineutrino transition probability.
- Parameters:
t (float or ndarray) – List of times.
E (float or ndarray) – List of energies.
- Returns:
float or ndarray – Transition probability.
Available Transformations¶
Supernova oscillation physics for flavors e, X, e-bar, X-bar.
For measured mixing angles and latest global analysis results, visit http://www.nu-fit.org/.
- class snewpy.flavor_transformation.NoTransformation[source]¶
Survival probabilities for no oscillation case.
- class snewpy.flavor_transformation.CompleteExchange[source]¶
Survival probabilities for the case when the electron flavors are completely exchanged with the x flavor.
- class snewpy.flavor_transformation.AdiabaticMSW(mix_angles=None, mh=MassHierarchy.NORMAL)[source]¶
Adiabatic MSW effect.
Initialize transformation matrix.
- Parameters:
mix_angles (tuple or None) – If not None, override default mixing angles using tuple (theta12, theta13, theta23).
mh (MassHierarchy) – MassHierarchy.NORMAL or MassHierarchy.INVERTED.
- class snewpy.flavor_transformation.NonAdiabaticMSWH(mix_angles=None, mh=MassHierarchy.NORMAL)[source]¶
Nonadiabatic MSW effect.
Initialize transformation matrix.
- Parameters:
mix_angles (tuple or None) – If not None, override default mixing angles using tuple (theta12, theta13, theta23).
mh (MassHierarchy) – MassHierarchy.NORMAL or MassHierarchy.INVERTED.
- class snewpy.flavor_transformation.TwoFlavorDecoherence(mix_angles=None, mh=MassHierarchy.NORMAL)[source]¶
Star-earth transit survival probability: two flavor case.
Initialize transformation matrix.
- Parameters:
mix_angles (tuple or None) – If not None, override default mixing angles using tuple (theta12, theta13, theta23).
mh (MassHierarchy) – MassHierarchy.NORMAL or MassHierarchy.INVERTED.
- class snewpy.flavor_transformation.ThreeFlavorDecoherence[source]¶
Star-earth transit survival probability: three flavor case.
- class snewpy.flavor_transformation.NeutrinoDecay(mix_angles=None, mass=<Quantity 1.11265006e-17 eV s2 / m2>, tau=<Quantity 1. d>, dist=<Quantity 10. kpc>, mh=MassHierarchy.NORMAL)[source]¶
Decay effect, where the heaviest neutrino decays to the lightest neutrino. For a description and typical parameters, see A. de Gouvêa et al., PRD 101:043013, 2020, arXiv:1910.01127.
Initialize transformation matrix.
- Parameters:
mix_angles (tuple or None) – If not None, override default mixing angles using tuple (theta12, theta13, theta23).
mass (astropy.units.quantity.Quantity) – Mass of the heaviest neutrino; expect in eV/c^2.
tau (astropy.units.quantity.Quantity) – Lifetime of the heaviest neutrino.
dist (astropy.units.quantity.Quantity) – Distance to the supernova.
mh (MassHierarchy) – MassHierarchy.NORMAL or MassHierarchy.INVERTED.
- class snewpy.flavor_transformation.AdiabaticMSWes(mix_angles, mh=MassHierarchy.NORMAL)[source]¶
A four-neutrino mixing prescription. The assumptions used are that:
the fourth neutrino mass is the heaviest but not so large that the electron-sterile resonances are inside the neutrinosphere;
the “outer” or H’ electron-sterile MSW resonance is adiabatic;
the “inner” or H’’ electron-sterile MSW resonance (where the electron fraction = 1/3) is non-adiabatic.
For further insight see, for example, Esmaili, Peres, and Serpico, Phys. Rev. D 90, 033013 (2014).
Initialize transformation matrix.
- Parameters:
mix_angles (tuple) – Values for mixing angles (theta12, theta13, theta23, theta14).
mh (MassHierarchy) – MassHierarchy.NORMAL or MassHierarchy.INVERTED.
- class snewpy.flavor_transformation.NonAdiabaticMSWes(mix_angles, mh=MassHierarchy.NORMAL)[source]¶
A four-neutrino mixing prescription. The assumptions used are that:
the fourth neutrino mass is the heaviest but not so large that the electron-sterile resonances are inside the neutrinosphere;
the “outer” or H’ electron-sterile MSW resonance is non-adiabatic;
the “inner” or H’’ electron-sterile MSW resonance (where the electron fraction = 1/3) is non-adiabatic.
For further insight see, for example, Esmaili, Peres, and Serpico, Phys. Rev. D 90, 033013 (2014).
Initialize transformation matrix.
- Parameters:
mix_angles (tuple) – Values for mixing angles (theta12, theta13, theta23, theta14).
mh (MassHierarchy) – MassHierarchy.NORMAL or MassHierarchy.INVERTED.