Library of Emergent Spectra and Fluxes of Type Ia Explosions
Description: The files on this page are part of the paper Expectations for the Hard X-ray Continuum and Gamma-ray Line Fluxes from the Type Ia supernova SN 2014J in M82 by The and Burrows (2014), submitted to the Astrophysical Journal. Recently, a Type Ia supernova, now designated SN 2014J, exploded in the galaxy Messier 82 at a distance of ~3.5 megaparsecs. There already exist in the literature many predictions for the hard photon signatures of many disparate Type Ia models. We surmise, however, that a focussed set of new calculations in aid of the ongoing SN 2014J campaign to detect its hard continuum and line emissions might be of use. In this spirit, we have calculated detailed spectra for fifteen models in the literature of Type Ia explosions at various times since the onset of explosion. The models are described in the associated paper, and references therein.
To derive the emergent spectrum at a given post-explosion time we employ the variance reduction Monte Carlo code developed in Burrows & The (1990) and The, Burrows, & Bussard (1990), augmented to include the bremsstrahlung X-ray production of the Compton electrons and the iron fluorescence line at ~6.4 keV (Clayton & The 1991; The, Bridgman, & Clayton 1994). The six most prominent lines of Ni-56 decay (including the 158, 750, and 812 keV lines) and the forty-five most prominent lines of Co-56 decay (the most important of which are at 847, 1238, 1772, and 2598 keV) are followed from emission, through Compton scatterings, to either photoelectric absorption in the homologously-expanding debris or escape. We also include the ten lines of Co-57 decay, for which the 14.4, 122, and 136 keV lines are the most important. The production of positrons is included, but they are assumed to form positronium instantaneously and to annihilate in situ (Bussard, Ramaty, & Drachman 1979). Both two-photon (25%) and three-photon (75%) decays are allowed, and those photons are then followed in the Monte Carlo. The electron-positron pair-prodcution cross section is taken from Ambwani & Sutherland (1988), the full angle-dependent Klein-Nishina formula for Compton scattering is used, and the photoelectric cross sections for the thirty-one most abundant elements thought to reside in Type Ia debris are taken from Veigele et al.(1973) and Henke et al. (1982). Feel free to contact Adam Burrows if you have questions or requests.
Format:
1) The files with the names *model*spec_3p5Mpc.dat each contain the model's spectrum in photons cm-2s-1keV-1 at a distance of 3.5 Mpc. The first column is the low-energy edge of the bin and the other columns are the spectra at the times indicated at the top of each column.
2) The files with the names fxtot_vs_t_*model*_3p5Mpc.dat each contain the band fluxes in units of photons cm-2s-1 at 3.5 Mpc at various times (in days) after explosion (in bins of width 10 keV, between 10 and 100 keV). The first column on the left is time in days since explosion. The other columns are the associated band fluxes at the day and photon energy interval given.
3) The files with the names gamma_line_flux_*model*_3p5Mpc.dat each contain a column (at the far left) giving the day since explosion, followed by columns of the associated line fluxes (in photons cm-2s-1 at 3.5 Mpc) for the line energies given in the column headings (top row). Those line energies are 158, 750, 812, 847, 1238, 511, 14.4, 122, and 6.4 keV.
Individual model hard X-ray band fluxes below 100 keV in 10 keV bins:
Individual model gamma line fluxes as a function of time: