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Title: Supernova Light Curves and Spectra from Several Code Pipelines

 [1];  [1];  [1]
  1. Los Alamos National Laboratory
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Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
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DOE Contract Number:
Resource Type:
Technical Report
Country of Publication:
United States

Citation Formats

Wollaeger, Ryan Thomas, Frey, Lucille Helen, and Even, Wesley Paul. Supernova Light Curves and Spectra from Several Code Pipelines. United States: N. p., 2018. Web. doi:10.2172/1422937.
Wollaeger, Ryan Thomas, Frey, Lucille Helen, & Even, Wesley Paul. Supernova Light Curves and Spectra from Several Code Pipelines. United States. doi:10.2172/1422937.
Wollaeger, Ryan Thomas, Frey, Lucille Helen, and Even, Wesley Paul. 2018. "Supernova Light Curves and Spectra from Several Code Pipelines". United States. doi:10.2172/1422937.
title = {Supernova Light Curves and Spectra from Several Code Pipelines},
author = {Wollaeger, Ryan Thomas and Frey, Lucille Helen and Even, Wesley Paul},
abstractNote = {},
doi = {10.2172/1422937},
journal = {},
number = ,
volume = ,
place = {United States},
year = 2018,
month = 2

Technical Report:

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  • This report discusses supernova light simulations. A brief review of supernovae, basics of supernova light curves, simulation tools used at LANL, and supernova results are included. Further, it happens that many of the same methods used to generate simulated supernova light curves can also be used to model the emission from fireballs generated by explosions in the earth’s atmosphere.
  • We present a new series of supernova neutrino light curves and spectra calculated by numerical simulations for a variety of progenitor stellar masses (13-50 M {sub Sun }) and metallicities (Z = 0.02 and 0.004), which would be useful for a broad range of supernova neutrino studies, e.g., simulations of future neutrino burst detection by underground detectors or theoretical predictions for the relic supernova neutrino background. To follow the evolution from the onset of collapse to 20 s after the core bounce, we combine the results of neutrino-radiation hydrodynamic simulations for the early phase and quasi-static evolutionary calculations of neutrinomore » diffusion for the late phase, with different values of shock revival time as a parameter that should depend on the still unknown explosion mechanism. We describe the calculation methods and basic results, including the dependence on progenitor models and the shock revival time. The neutrino data are publicly available electronically.« less
  • To assess the effectiveness of optical emission as a probe of spatial asymmetry in core-collapse supernovae (CCSNe), we apply in this paper the radiative transfer software SuperNu to a unimodal CCSN model. The SNSPH radiation hydrodynamics software was used to simulate an asymmetric explosion of a 16more » $${M}_{\odot }$$ zero-age main-sequence binary star. The ejecta has 3.36 $${M}_{\odot }$$ with 0.024 $${M}_{\odot }$$ of radioactive 56Ni, with unipolar asymmetry along the z-axis. For 96 discrete angular views, we find a ratio between maximum and minimum peak total luminosities of ~1.36. The brightest light curves emerge from views orthogonal to the z-axis. Multigroup spectra from UV to IR are obtained. We find a shift in wavelength with viewing angle in a near-IR Ca ii emission feature, consistent with Ca being mostly in the unimode. We compare emission from the gray gamma-ray transfer in SuperNu and from the detailed gamma-ray transfer code Maverick. Relative to the optical light curves, the brightness of the gamma-ray emission is more monotonic with respect to viewing angle. UBVRI broadband light curves are also calculated. Parallel with the unimode, the U and B bands have excess luminosity at $$\gtrsim 10$$ days post-explosion, due to 56Ni on the unimode. Finally, we compare our CCSN model with SN 2002ap, which is thought to have a similar ejecta morphology.« less
  • Neutron spectra were calculated as a function of angle between 0 and 110$sup 0$ for $sup 12$C on $sup 56$Fe at 192, 500, 700, and 900 MeV. Proton spectra were calculated for the same angular range but for only 192-MeV $sup 12$C on $sup 56$Fe. The most significant property of these spectra is that there is an appreciable number of neutrons emitted with energies greater than the incident energy per nucleon at all angles investigated. 9 figures. (auth)