THE EFFECT OF A COSMIC RAY PRECURSOR IN SN 1006?
THE EFFECT OF A COSMIC RAY PRECURSOR IN SN 1006?
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DOI：
10.1088/2041-8205/735/1/l21
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发表时间：
2011-04
期刊：
影响因子：
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通讯作者：
C. Rakowski;J. Laming;U. Hwang;K. Eriksen;P. Ghavamian;J. Hughes
中科院分区：
文献类型：
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作者：
C. Rakowski;J. Laming;U. Hwang;K. Eriksen;P. Ghavamian;J. Hughes
像许多年轻的超新星遗迹一样，SN 1006显示出接近或突出于主爆炸波之外的喷射物团块。在这封信中，我们检查三个这样的凸出沿东部边缘。它们与激波前后面的喷射指半对齐，并显示出O vii和O viii的发射线。我们首先在上游介质的背景下解释了饱和非共振贝尔不稳定性，这种不稳定性在平流后增强了瑞利-泰勒不稳定性的增长。如果间隔由残余物的性质决定或由宇宙射线前体的首选尺寸尺度决定，我们将讨论它们的表观周期性。我们还简要讨论了另一种可能，即这些结构起源于爆炸本身的喷出物结构。在这种情况下，SN 1006的年轻演化年龄意味着爆炸最外层的密度结构，这对热核超新星爆炸模型中的爆燃和爆炸具有潜在的重要意义。
Like many young supernova remnants, SN 1006 exhibits what appear to be clumps of ejecta close to or protruding beyond the main blast wave. In this Letter, we examine three such protrusions along the east rim. They are semi-aligned with ejecta fingers behind the shock-front and exhibit emission lines from O vii and O viii. We first interpret them in the context of an upstream medium modified by the saturated non-resonant Bell instability which enhances the growth of Rayleigh–Taylor instabilities when advected post-shock. We discuss their apparent periodicity if the spacing is determined by properties of the remnant or by a preferred size scale in the cosmic ray precursor. We also briefly discuss the alternative that these structures have an origin in the ejecta structure of the explosion itself. In this case, the young evolutionary age of SN 1006 would imply density structure within the outermost layers of the explosion with potentially important implications for deflagration and detonation in thermonuclear supernova explosion models.