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Interacting supernovae from photoionization-confined shells around red supergiant stars

机译：围绕红色超巨星周围的电离受限壳相互作用的超新星

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摘要

Betelgeuse, a nearby red supergiant, is a fast-moving star with a powerful stellar wind that drives a bow shock into its surroundings. This picture has been challenged by the discovery of a dense and almost static shell that is three times closer to the star than the bow shock and has been decelerated by some external force. The two physically distinct structures cannot both be formed by the hydrodynamic interaction of the wind with the interstellar medium. Here we report that a model in which Betelgeuse's wind is photoionized by radiation from external sources can explain the static shell without requiring a new understanding of the bow shock. Pressure from the photoionized wind generates a standing shock in the neutral part of the wind6 and forms an almost static, photoionization-confined shell. Other red supergiants should have much more massive shells than Betelgeuse, because the photoionization-confined shell traps up to 35 per cent of all mass lost during the red supergiant phase, confining this gas close to the star until it explodes. After the supernova explosion, massive shells dramatically affect the supernova light curve, providing a natural explanation for the many supernovae that have signatures of circumstellar interaction.
机译：邻近的红色超级巨星Betelgeuse是一颗快速移动的恒星，具有强烈的恒星风，可向周围环境造成弓形冲击。这张照片的挑战是，发现了一个密集且几乎静止的壳，该壳比弓形冲击波更靠近恒星，并且由于某种外力而减速了三倍。风与星际介质的水动力相互作用不能同时形成两个物理上不同的结构。在这里，我们报告一个模型，其中Betelgeuse的风被外部源的辐射光电离，可以解释静态壳体，而无需重新了解船首冲击。光电离风产生的压力会在风的中性部分6产生站立冲击，并形成几乎静态的，受光电离限制的壳体。其他红色超巨星应该有比Betelgeuse更大的壳，因为受光电离作用限制的壳最多可以捕获红色超巨星阶段损失的所有质量的35％，从而将这种气体限制在恒星附近直至爆炸。在超新星爆炸之后，大质量的壳层极大地影响了超新星的光曲线，为许多具有星际相互作用特征的超新星提供了自然的解释。

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  • 来源
    《Nature》 |2014年第7514期|282-285|共4页
  • 作者

    Jonathan Mackey; Shazrene Mohamed; Vasilii V. Gvaramadze; Rubina Kotak; Norbert Langer; Dominique M.-A. Meyer; Takashi J. Moriya; Hilding R. Neilson;

  • 作者单位

    Argelander-Institut fuer Astronomie, Auf dem Huegel 71, 53121 Bonn, Germany;

    South African Astronomical Observatory, PO Box 9, 7935 Observatory, South Africa;

    Sternberg Astronomical Institute, Lomonosov Moscow State University, Universitetskij Prospect 13, Moscow 119992, Russia,Isaac Newton Institute of Chile, Moscow Branch, Universitetskij Prospect 13, Moscow 119992, Russia,Space Research Institute, Russian Academy of Sciences, Profsoyuznaya 84/32, Moscow 117997, Russia;

    Astro physics Research Centre, School of Mathematics and Physics, Queen's University Belfast, Belfast BT7 1NN, UK;

    Argelander-Institut fuer Astronomie, Auf dem Huegel 71, 53121 Bonn, Germany;

    Argelander-Institut fuer Astronomie, Auf dem Huegel 71, 53121 Bonn, Germany;

    Argelander-Institut fuer Astronomie, Auf dem Huegel 71, 53121 Bonn, Germany;

    Department of Physics and Astronomy, East Tennessee State University, Box 70652, Johnson City, Tennessee 37614, USA;

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