O’Connor 2015 Models

Data from O’Connor 2015, black hole forming simulations of a 40 solar mass progenitor from Woosley and Heger 2007 and the LS220 EOS.

Reference: O’Connor ApJS 219 24 2015

• doi:10.1088/0067-0049/219/2/24

• arXiv:1411.7058

import matplotlib as mpl
import matplotlib.pyplot as plt
import numpy as np

from astropy import units as u

from snewpy.neutrino import Flavor, MassHierarchy
from snewpy.models.ccsn import OConnor_2015
from snewpy.flavor_transformation import NoTransformation, AdiabaticMSW, ThreeFlavorDecoherence

mpl.rc('font', size=16)
%matplotlib inline

Initialize Models

To start, let’s see what progenitors are available for the OConnor_2015 model. We can use the param property to view all physics parameters and their possible values:

OConnor_2015.param

{'progenitor_mass': [<Quantity 40. solMass>], 'eos': ['LS220']}

We’ll initialise this progenitor. If this is the first time you’re using a progenitor, snewpy will automatically download the required data files for you.

model = OConnor_2015(progenitor_mass=40*u.solMass)

model

OConnor_2015 Model: M1_neutrinos.dat

Parameter	Value
Progenitor mass	\(40\) \(\mathrm{M_{\odot}}\)
EOS	LS220

Finally, let’s plot the luminosity of different neutrino flavors for this model. (Note that the OConnor_2015 simulation didn’t distinguish between \(\nu_x\) and \(\bar{\nu}_x\), so both have the same luminosity.)

fig, ax = plt.subplots(1, figsize=(8, 6), tight_layout=False)

for flavor in Flavor:
    ax.plot(model.time, model.luminosity[flavor]/1e51,  # Report luminosity in units foe/s
            label=flavor.to_tex(),
            color='C0' if flavor.is_electron else 'C1',
            ls='-' if flavor.is_neutrino else ':',
            lw=2)
ax.set(xlim=(0, 0.55),
        xlabel=r'$t-t_{\rm bounce}$ [s]',
        title=r'{}: {} $M_\odot$'.format(model.metadata['EOS'], model.metadata['Progenitor mass'].value))
ax.grid()
ax.legend(loc='upper right', ncol=2, fontsize=18)
ax.set(ylabel=r'luminosity [foe s$^{-1}$]');

Initial and Oscillated Spectra

Plot the neutrino spectra at the source and after the requested flavor transformation has been applied.

Adiabatic MSW Flavor Transformation: Normal mass ordering

# Adiabatic MSW effect. NMO is used by default.
xform_nmo = AdiabaticMSW()

# Energy array and time to compute spectra.
# Note that any convenient units can be used and the calculation will remain internally consistent.
E = np.linspace(0,100,201) * u.MeV
t = 400*u.ms

ispec = model.get_initial_spectra(t, E)
ospec_nmo = model.get_transformed_spectra(t, E, xform_nmo)

fig, axes = plt.subplots(1,2, figsize=(12,5), sharex=True, sharey=True, tight_layout=True)

for i, spec in enumerate([ispec, ospec_nmo]):
    ax = axes[i]
    for flavor in Flavor:
        ax.plot(E, spec[flavor],
                label=flavor.to_tex(),
                color='C0' if flavor.is_electron else 'C1',
                ls='-' if flavor.is_neutrino else ':', lw=2,
                alpha=0.7)

    ax.set(xlabel=r'$E$ [{}]'.format(E.unit),
           title='Initial Spectra: $t = ${:.1f}'.format(t) if i==0 else 'Oscillated Spectra: $t = ${:.1f}'.format(t))
    ax.grid()
    ax.legend(loc='upper right', ncol=2, fontsize=16)

ax = axes[0]
ax.set(ylabel=r'flux [erg$^{-1}$ s$^{-1}$]')

fig.tight_layout();