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Comments from Amol, June 29 2010

Amol’s suggestion for models to look at:

1. Livermore (energies have a smooth time variation) 2. Garching early time (accretion phase) 3. Garching late time (cooling phase) 4. Basel (smooth monotonic time variation for energies and fluxes)

Flux File Format

Compatible with GLoBES

Seven columns and 501 lines with equidistant energies

Energy / Phi_nue / Phi_numu / Phi_nutau / Phi_nuebar / Phi_numubar / Phi_nutaubar


Energy should be in GeV

Flux units: per second per cm^2 (per energy bin).  The flux should be for a supernova at 10 kpc.

I suggest 0 to 0.1 GeV as the standard energy range for the flux file (the binning in 500 bins will be finer than any experiment energy resolution).

Files are differential energy spectra only: there should be one file per time slice, plus one file with the spectrum integrated over time.

One-line comments beginning with # and ending with "\n" can be included for notes.

Proposed filename format: fluxname-time-timebinsize.dat

Other info to be indicated in fluxname-notes.dat


Livermore model

"Future detection of supernova neutrino burst and explosion mechanism."

T. Totani, K. Sato, H.E. Dalhed, J.R. Wilson,

Astrophys. J. 496 216 (1998) eprint

Garching models

"Supernova neutrinos: Flavor-dependent fluxes and spectra."

Georg G. Raffelt, Mathias Th. Keil, Robert Buras, Hans-Thomas Janka, Markus Rampp,

To appear in the proceedings of 4th Workshop on Neutrino Oscillations and their Origin (NOON2003), Kanazawa, Japan, 10-14 Feb 2003. 
Published in *Kanazawa 2003, Neutrino oscillations and their origin* eprint

"Explosions of O-Ne-Mg cores, the crab supernova, and subluminous Type IIp supernovae."

F.S. Kitaura, Hans-Thomas Janka, W. Hillebrandt,

Submitted to Astron.Astrophys. 

"Neutrino Signal of Electron-Capture Supernovae from Core Collapse to Cooling"

Hüdepohl, L., Müller, B., Janka, H.-T., Marek, A., Raffelt, G. G.

Physical Review Letters 104 251101 (2010) eprint

Basel model

"Protoneutron star evolution and the neutrino driven wind in general relativistic neutrino radiation hydrodynamics simulations."

T. Fischer, S.C. Whitehouse, A. Mezzacappa, F.-K. Thielemann, M. Liebendorfer, . eprint


Luminosities and Mean Energies

Here are files of the luminosities and mean energies. Other than the Garching case the functional form of the spectra is unknown.


Figures from Totani et al.

Fig1 Fig4

Digitized data File:Totani.tar


Figures from Hüdepohl et al.

Fig1a Fig1b Fig2

Original data File:Garching.tar


Figures from Fischer et al.

Fig2a Fig2b Fig2d
Fig2a Fig2b Fig2d

Digitized data File:Fischer.tar


In the absence of profiles from the simulations here are some density profiles used in Kneller, McLaughlin and Brockman. Three 1D models are provided ranging from a weak explosion (model 6e35) through something canonical (model 8e35) and then up a strong explosion case (model 2e36). For compactness the data is in 'carpet' format: i.e.

t1 t2 t3 ....
r1 rho11 rho12 rho13 ....
r2 rho21 rho22 rho23 ....
r3 rho31 rho32 rho33 ....
. . . .
. . . .
. . . .

i.e. each column gives rho(r) at some fixed time. There are 750 rows, 78 columns in each file. The units are: [r] is in cm, [t] is in seconds. [rho] is in g/cm^3. Y_e can be set to 1/2. There are two issues with the profiles you should be aware of: the profiles have deficiencies in the inner regions because neutrino cooling was not included in the simulations, the shocks are 'soft'. To compensate for these problems the profiles between the proto-neutron star and a radius of r ~ few hundred km should be replaced by a parametric form such as a double power-law

rho = C1 r^n1 + C2 r^n2

The parameters C1, C2, n1, n2 are determined by the requirement that the parametric form be continuous and have continuous derivative at the boundaries with the rest of the data. The soft shocks can either be steepened by hand or you should use a value of theta_13 no larger than 1°.

Lastly, this data is provided solely for the purpose of this study.