Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud
Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud
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DOI：
10.3847/1538-4365/aa653c
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发表时间：
2017-03
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通讯作者：
L. Bozzetto;M. Filipovi'c;B. Vukoti'c;M. Pavlović;D. Urošević;D. Urošević;P. Kavanagh;B. Arbutina;P. Maggi;M. Sasaki;F. Haberl;E. Crawford;Q. Roper;K. Grieve;S. Points
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作者：
L. Bozzetto;M. Filipovi'c;B. Vukoti'c;M. Pavlović;D. Urošević;D. Urošević;P. Kavanagh;B. Arbutina;P. Maggi;M. Sasaki;F. Haberl;E. Crawford;Q. Roper;K. Grieve;S. Points
我们构建了任何星系中最完整的超新星遗迹 (SNR) 样本——大麦哲伦星云 (LMC) SNR 样本。我们研究它们的各种特性，例如光谱指数 (α)、尺寸和表面亮度。我们提出 LMC SNR 的空间分布和环境密度之间的关联，以及它们位于超巨星壳周围的趋势。我们发现证据表明，与核心塌陷 (CC) 类型相比，16 个已知的 Ia 型 LMC SNR 在密度较低的环境中正在扩展。我们整个星系群 (74) 的平均直径为 41 pc，与附近的星系相当。我们没有发现 SN 爆炸类型、椭圆度或年龄之间存在任何相关性。与斜率 a = 0.96 的关系意味着随机直径很容易模仿这样的指数。据估计，LMC 中超新星的发生率约为每 200 年 1 次。整个 LMC SNR 总体的平均 α 为 -0.52，这是大多数 SNR 的典型值。然而，我们的估计表明，随着残余物的老化，同步加速器α明显变平。正如预测的那样，我们样本中的 CC SNR 是比 Ia 型残余物更亮的无线电发射器。我们还估计 LMC 的关系斜率约为 3.8，与其他附近的星系相当。我们还发现了电子在星系中的驻留时间（4.0-14.3 Myr），这意味着 SNR 应该是 CR 产生和加速的主要机制。
We construct the most complete sample of supernova remnants (SNRs) in any galaxy—the Large Magellanic Cloud (LMC) SNR sample. We study their various properties such as spectral index (α), size, and surface brightness. We suggest an association between the spatial distribution and environment density of LMC SNRs, and their tendency to be located around supergiant shells. We find evidence that the 16 known type Ia LMC SNRs are expanding in a lower density environment compared to the Core-Collapse (CC) type. The mean diameter of our entire population (74) is 41 pc, which is comparable to nearby galaxies. We did not find any correlation between the type of SN explosion, ovality, or age. The relationship with slope a = 0.96 implies that the randomized diameters are readily mimicking such an exponent. The rate of SNe occurring in the LMC is estimated to be ∼1 per 200 yr. The mean α of the entire LMC SNR population is −0.52, which is typical of most SNRs. However, our estimates show a clear flattening of the synchrotron α as the remnants age. As predicted, the CC SNRs in our sample are significantly brighter radio emitters than type Ia remnants. We also estimate the relation for the LMC to have a slope ∼3.8, which is comparable with other nearby galaxies. We also find the residency time of electrons in the galaxy (4.0–14.3 Myr), implying that SNRs should be the dominant mechanism for the production and acceleration of CRs.