论文标题
来自热核超新星的银河系正气
Galactic Positrons from Thermonuclear Supernovae
论文作者
论文摘要
IA型超新星（SNE IA）可能源自多种爆炸场景和祖细胞通道。它们在亮度上显示出约10个差异，因此质量为56ni-> 56co-> 56 fe。我们介绍了SNE IA内正面子的命运的研究，以评估其逃生部分和能量光谱。我们针对正电子和伽马射线的详细蒙特卡洛运输模拟包括56 CO的β +衰减和配对生产。我们模拟了各种各样的爆炸场景，包括靠近Chandrasekhar Mass，M（CH）的白色矮人（WD）的爆炸，HE触发了Sub-M CH WDS的爆炸以及两个WDS的动态合并。对于每个模型，我们研究了1至1E13 G之间祖细胞磁场的大小和形态的影响。基于观察到的亮度分布的人口合成，用于估计由于从SN IA中逃脱而导致银河系正子的总体贡献。我们发现这是由正常的sne ia主导的，其中发射正电子的分布的变化很小。我们估计了SNE IA对<2％的银河系正值的总贡献，并且取决于磁场的形态，分别为M（CH）和Sub-M（CH）的6 ... 20％。
Type Ia Supernovae (SNe Ia) may originate from a wide variety of explosion scenarios and progenitor channels. They exhibit a factor of about 10 difference in brightness and, thus, a differentiation in the mass of 56Ni->56Co->56 Fe. We present a study on the fate of positrons within SNe Ia in order to evaluate their escape fractions and energy spectra. Our detailed Monte Carlo transport simulations for positrons and gamma-rays include both beta + decay of 56 Co and pair production. We simulate a wide variety of explosion scenarios, including the explosion of white dwarfs (WD) close to the Chandrasekhar mass, M(Ch), He-triggered explosions of sub-M Ch WDs, and dynamical mergers of two WDs. For each model, we study the influence of the size and morphology of the progenitor magnetic field between 1 and 1E13 G. Population synthesis based on the observed brightness distribution of SNe Ia was used to estimate the overall contributions to Galactic positrons due to escape from SN Ia. We find that this is dominated by normal-bright SNe Ia, where variations in the distribution of emitted positrons are small. We estimate a total SNe Ia contribution to the Galactic positrons of < 2% and, depending on the magnetic field morphology, less than 6...20% for M(Ch) and sub-M(Ch), respectively.
