PROPERTIES OF NEWLY FORMED DUST GRAINS IN THE LUMINOUS TYPE IIn SUPERNOVA 2010jl-猫眼课题宝

DOI：

10.1088/0004-637x/776/1/5

发表时间：

2013-08

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

K. Maeda;T. Nozawa;D. Sahu;Y. Minowa;K. Motohara;I. Ueno;G. Folatelli;T. Pyo;Yutaro Kitagawa;K. Kawabata;G. Anupama;T. Kozasa;T. Moriya;T. Moriya;M. Yamanaka;M. Yamanaka;K. Nomoto;M. Bersten;R. Quimby;M. Iye

超新星(SNE)被认为是宇宙中尘埃颗粒的主要产生场所。然而，我们对它们对尘埃产生的重要性的了解受到了对单个近地天体产生的尘埃粒子的性质和数量的观测上的不佳限制。在这篇文章中，我们给出了在爆炸一年半后，发光的IIn型超新星2010jl的近红外(NIR)光的光谱。这个独特的数据集揭示了新形成的尘埃粒子的多个特征。光谱的近红外部分提供了一个罕见的例子，可以清楚地检测到新形成的热尘埃颗粒的热发射。在∼1350K-1450K的温度范围内，我们确定了尘埃物种的主要种群是碳颗粒。尘埃粒子的质量为∼(7.58.5)×10−4M☉。氢发射线表现出与波长有关的吸收，这提供了对新形成的尘埃颗粒(≲0.1μm，最有可能是≲0.01μm)的典型尺寸的很好估计。我们认为，这些尘埃颗粒是在一个致密的冷却壳层中形成的，这是SN-星周介质(CSM)强烈相互作用的结果。尘埃颗粒占发射体积的10%，表明尘埃颗粒是一种不均匀的块状结构。平均CSM密度必须为≳3×107 cm−3，对应的质量损失率为≳0.02M☉yr−1(质量损失风速为∼100公里S−1)。这有力地支持了这样一种假设，即SN 2010jl和其他发光的SNE IIn是由非常密集的CSM内的强烈相互作用提供动力的，可能是在爆炸前的上个世纪内由类似发光蓝色变量的喷发造成的。

Supernovae (SNe) have been proposed to be the main production sites of dust grains in the universe. However, our knowledge of their importance to dust production is limited by observationally poor constraints on the nature and amount of dust particles produced by individual SNe. In this paper, we present a spectrum covering optical through near-Infrared (NIR) light of the luminous Type IIn supernova 2010jl around one and a half years after the explosion. This unique data set reveals multiple signatures of newly formed dust particles. The NIR portion of the spectrum provides a rare example where thermal emission from newly formed hot dust grains is clearly detected. We determine the main population of the dust species to be carbon grains at a temperature of ∼1350–1450 K at this epoch. The mass of the dust grains is derived to be ∼(7.5–8.5) × 10−4 M☉. Hydrogen emission lines show wavelength-dependent absorption, which provides a good estimate of the typical size of the newly formed dust grains (≲ 0.1 μm, and most likely ≲ 0.01 μm). We believe the dust grains were formed in a dense cooling shell as a result of a strong SN–circumstellar media (CSM) interaction. The dust grains occupy ∼10% of the emitting volume, suggesting an inhomogeneous, clumpy structure. The average CSM density must be ≳ 3 × 107 cm−3, corresponding to a mass loss rate of ≳ 0.02 M☉ yr−1 (for a mass loss wind velocity of ∼100 km s−1). This strongly supports a scenario in which SN 2010jl and probably other luminous SNe IIn are powered by strong interactions within very dense CSM, perhaps created by Luminous-Blue-Variable-like eruptions within the last century before the explosion.

PROPERTIES OF NEWLY FORMED DUST GRAINS IN THE LUMINOUS TYPE IIn SUPERNOVA 2010jl

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