%0 Journal Article
%T Vela Jr.：超新星喷发团块与超新星遗骸的互动<br>Vela Jr.: Ejecta-Clump Interaction in the Vela Supernova Remnant
%A 王致悦
%J Astronomy and Astrophysics
%P 32-37
%@ 2329-1265
%D 2013
%I Hans Publishing
%R 10.12677/AAS.2013.12005
%X <div style=\"text-align:justify;\">
	<span style=\"line-height:1.5;\">重迭在船帆座超新星遗骸</span><span style=\"line-height:1.5;\">(Vela supernova remnant)</span><span style=\"line-height:1.5;\">视线上的</span><span style=\"line-height:1.5;\">ROSAT</span><span style=\"line-height:1.5;\"> X</span><span style=\"line-height:1.5;\">射线源</span><span style=\"line-height:1.5;\">RX J0852.0-4622</span><span style=\"line-height:1.5;\">，或称</span><span style=\"line-height:1.5;\">Vela Jr.</span><span style=\"line-height:1.5;\">，因其在</span><span style=\"line-height:1.5;\">1.3</span><span style=\"line-height:1.5;\">千电子伏的波段上呈现圆壳外观和检测出</span><span style=\"line-height:1.5;\">44</span><span style=\"line-height:1.5;\">Ti</span><span style=\"line-height:1.5;\">的</span><span style=\"line-height:1.5;\">γ</span><span style=\"line-height:1.5;\">射线衰变线</span><span style=\"line-height:1.5;\">，</span><span style=\"line-height:1.5;\">所以被认为是新发现的年轻超新星遗骸。然而，观测证据指出</span><span style=\"line-height:1.5;\">Vela Jr.</span><span style=\"line-height:1.5;\">应属于船帆座超新星遗骸的一部份而非独立的物体。二维气体动力学模拟显示，超新星快速的高密度喷发气体物</span><span style=\"line-height:1.5;\">(</span><span style=\"line-height:1.5;\">子弹</span><span style=\"line-height:1.5;\">)</span><span style=\"line-height:1.5;\">可以影响遗骸的外围，产生类似于</span><span style=\"line-height:1.5;\">Vela Jr.</span><span style=\"line-height:1.5;\">的圆环结构。估计</span><span style=\"line-height:1.5;\">Vela Jr.</span><span style=\"line-height:1.5;\">的能量为</span><span style=\"line-height:1.5;\">&lt;0.3 × 10</span><span style=\"line-height:1.5;\">49</span><span style=\"line-height:1.5;\"> erg</span><span style=\"line-height:1.5;\">，相当于</span><span style=\"line-height:1.5;\">1700 km</span><span style=\"line-height:1.5;\">/s</span><span style=\"line-height:1.5;\">、</span><span style=\"line-height:1.5;\">&lt;</span><span style=\"line-height:1.5;\">~</span><span style=\"line-height:1.5;\">0.1M</span><span style=\"line-height:1.5;\">⊙</span><span style=\"line-height:1.5;\">的超新星喷发物所注入的动能。我们认为子弹生成最有可能的机制是镍泡效应</span><span style=\"line-height:1.5;\">(nickel bubble effect)</span><span style=\"line-height:1.5;\">。我们预测子弹应该产生辐射，而船帆座超新星遗骸在低</span><span style=\"line-height:1.5;\">X</span><span style=\"line-height:1.5;\">射线亮度的波段上也应存在其它类似的结构。&lt;br/&gt;</span><span style=\"line-height:1.5;\">The </span><span style=\"line-height:1.5;\">ROSAT</span><span style=\"line-height:1.5;\"> source RX J0852.0-4622, or Vela Jr., superposed on the Vela supernova remnant, has been identified as a separate young supernova remnant based on its shell-like appearance in X-ray &gt; 1.3 keV and on its detection as a source of the
%K 星际介质(RX J0852-4622
%K Vela Jr.)；超新星遗骸(Vela Jr.
%K Vela SNR
%K SN1572)；流体力学；不稳定性；冲击波<br>ISM (RX J0852.0-4622
%K Vela Jr.)
%K Supernova Remnants (Vela Jr.
%K Vela SNR
%K SN1572)
%K Hydrodynamics
%K Instabilities
%K Shock Waves
%U http://www.hanspub.org/journal/PaperInformation.aspx?PaperID=9800