DIVERSITY OF LUMINOUS SUPERNOVAE FROM NON-STEADY MASS LOSS
DIVERSITY OF LUMINOUS SUPERNOVAE FROM NON-STEADY MASS LOSS
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DOI：
10.1088/0004-637x/747/2/118
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发表时间：
2011-10
期刊：
影响因子：
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通讯作者：
T. Moriya;N. Tominaga
中科院分区：
文献类型：
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作者：
T. Moriya;N. Tominaga
我们发现，由于非稳态质量损失的密度梯度的密集风的多样性可以解释光谱多样性的II型发光超新星（LSNe）的一种方式。SN喷出物与周围风的相互作用被认为是照亮LSNe的动力源，因为许多LSNe在其光谱中显示风特征（LSNe中的I型）。然而，也存在没有由风引起的光谱特征的LSNe（类型IIL LSNe）。我们表明，即使LSNe被照亮的相互作用，这是可能的，他们不显示从风的窄谱，如果我们考虑到非稳态质量损失的祖先。当激波爆发发生在密度结构为ρ r-w的稠密风中时，风光学厚区的扩散时标（td）与激波爆发后整个风的激波传播时标（ts）的比值强烈依赖于w。对于w ≠ 1的情况，两个时间尺度是可比的（td/ts ≠ 1），并且td/ts随着w的增大而变小。对于td/ts ≥ 1的情况，激波刚好在光变曲线（LC）峰值之后穿过整个风，在LC峰值之后不能观察到来自风的窄谱线（IIL型LSNe）。如果td/ts小得多，则冲击波在LC峰值之后继续在风中传播，并且保持无冲击风（类型IIn LSNe）。这种差别只有通过对密集风中激波爆发条件的仔细处理才能得到。在LC峰之前，IIL型LSNe中缺乏窄的洛伦兹线轮廓也可以通过密度斜率的差异来解释。此外，我们将我们的模型应用于类型IIn的LSN 2006 gy和类型IIL的LSN 2008 es，发现我们的模型是与观测相一致的。
We show that the diversity in the density slope of the dense wind due to non-steady mass loss can be one way to explain the spectral diversity of Type II luminous supernovae (LSNe). The interaction of SN ejecta and wind surrounding it is considered to be a power source to illuminate LSNe because many LSNe show the wind signature in their spectra (Type IIn LSNe). However, there also exist LSNe without the spectral features caused by the wind (Type IIL LSNe). We show that, even if LSNe are illuminated by the interaction, it is possible that they do not show the narrow spectra from the wind if we take into account the non-steady mass loss of their progenitors. When the shock breakout takes place in a dense wind with the density structure ρ∝r−w, the ratio of the diffusion timescale in the optically thick region of the wind (td) and the shock propagation timescale of the entire wind after the shock breakout (ts) strongly depends on w. For the case w ≲ 1, both timescales are comparable (td/ts ≃ 1) and td/ts gets smaller as w gets larger. For the case td/ts ≃ 1, the shock goes through the entire wind just after the light-curve (LC) peak, and narrow spectral lines from the wind cannot be observed after the LC peak (Type IIL LSNe). If td/ts is much smaller, the shock wave continues to propagate in the wind after the LC peak, and unshocked wind remains (Type IIn LSNe). This difference can be obtained only through careful treatment of the shock breakout condition in a dense wind. The lack of narrow Lorentzian line profiles in Type IIL LSNe before the LC peak can also be explained by the difference in the density slope. Furthermore, we apply our model to Type IIn LSN 2006gy and Type IIL LSN 2008es and find that our model is consistent with the observations.