| タイトル | Gamma-ray transfer and energy deposition in supernovae |
| 本文（外部サイト） | http://hdl.handle.net/2060/19960010538 |
| 著者（英） | Harkness, Robert P.; Swartz, Douglas A.; Sutherland, Peter G. |
| 著者所属（英） | NASA Marshall Space Flight Center |
| 発行日 | 1995-06-20 |
| 言語 | eng |
| 内容記述 | Solutions to the energy-independent (gray) radiative transfer equations are compared to results of Monte Carlo simulations of the Ni-56 and Co-56 decay gamma-ray energy deposition in supernovae. The comparison shows that an effective, purely absorptive, gray opacity, kappa(sub gamma) approximately (0. 06 +/- 0.01)Y(sub e) sq cm/g, where Y is the total number of electrons per baryon, accurately describes the interaction of gamma-rays with the cool supernova gas and the local gamma-ray energy deposition within the gas. The nature of the gamma-ray interaction process (dominated by Compton scattering in the relativistic regime) creates a weak dependence of kappa(sub gamma) on the optical thickness of the (spherically symmetric) supernova atmosphere: The maximum value of kappa(sub gamma) applies during optically thick conditions when individual gamma-rays undergo multiple scattering encounters and the lower bound is reached at the phase characterized by a total Thomson optical depth to the center of the atmosphere tau(sub e) approximately less than 1. Gamma-ray deposition for Type Ia supernova models to within 10% for the epoch from maximum light to t = 1200 days. Our results quantitatively confirm that the quick and efficient solution to the gray transfer problem provides an accurate representation of gamma-ray energy deposition for a broad range of supernova conditions. |
| NASA分類 | SPACE RADIATION |
| レポートNO | 96N17704
NASA-TM-111182
NAS 1.15:111182
NIPS-96-07108 |
| 権利 | Copyright, Distribution as joint owner in the copyright |
