• 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>Nature >The double-degenerate, super- Chandrasekhar nucleus of the planetary nebula Henize 2-428
【24h】

The double-degenerate, super- Chandrasekhar nucleus of the planetary nebula Henize 2-428

机译：行星状星云Henize 2-428的双简简超Chandrasekhar核

获取原文
获取原文并翻译 | 示例
           
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

The planetary nebula stage is the ultimate fate of stars with masses one to eight times that of the Sun (M_⊙). The origin of their complex morphologies is poorly understood, although several mechanisms involving binary interaction have been proposed. In close binary systems, the orbital separation is short enough for the primary star to overfill its Roche lobe as the star expands during the asymptotic giant branch phase. The excess gas eventually forms a common envelope surrounding both stars. Drag forces then result in the envelope being ejected into a bipolar planetary nebula whose equator is coincident with the orbital plane of the system. Systems in which both stars have ejected their envelopes and are evolving towards the white dwarf stage are said to be double degenerate. Here we report that Henize 2-428 has a double-degenerate core with a combined mass of ~～1.76M_⊙, which is above the Chandrasekhar limit (the maximum mass of a stable white dwarf) of 1.4M_⊙.This, together with its short orbital period (4.2 hours), suggests that the system should merge in 700 million years, triggering a type Ⅰa supernova event. This supports the hypothesis of the double-degenerate, super-Chandrasekhar evolutionary pathway for the formation of type Ⅰa supernovae.
机译：行星状星云阶段是恒星的最终命运，其质量是太阳（M_⊙）的1至8倍。尽管已经提出了几种涉及二元相互作用的机制，但人们对其复杂形态的起源知之甚少。在紧密的双星系统中，随着恒星在渐近巨型分支阶段扩张，其轨道间隔足够短，以至于主恒星会超额填充其罗氏瓣。多余的气体最终形成围绕两颗恒星的共同包络。然后，拖曳力导致包络被喷射到双极行星状星云中，该星云的赤道与系统的轨道平面重合。据说两个恒星都弹出了信封并朝着白矮星阶段演化的系统是双重退化的。在此我们报告说，亨利兹岛2-428具有双简并核，其总质量约为〜1.76M_⊙，高于Chandrasekhar极限（稳定的白矮星的最大质量）1.4M_⊙。它的短轨道周期（4.2小时）表明该系统应在7亿年内合并，引发Ⅰa型超新星事件。这支持了关于Ⅰa型超新星形成的双重简并超钱德拉塞卡发展途径的假说。

著录项

  • 来源
    《Nature》 |2015年第7541期|63-65|共3页
  • 作者

    M. Santander-Garcia; P. Rodriguez-Gil; R. L. M. Corradi; D. Jones; B. Miszalski; H. M. J. Boffin; M. M. Rubio-Diez; M. M. Kotze;

  • 作者单位

    Observatorio Astronomico Nacional, Apartado de Correos 112, E-28803, Alcala de Henares, Spain,Instituto de Ciencia de Materiales de Madrid (CSIC), Sor Juana Ines de la Cruz, 3, E-28049 Madrid, Spain;

    Instituto de Astrofisica de Canarias, E-38200 La Laguna, Tenerife, Spain,Departamento de Astrofisica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain;

    Instituto de Astrofisica de Canarias, E-38200 La Laguna, Tenerife, Spain,Departamento de Astrofisica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain;

    Instituto de Astrofisica de Canarias, E-38200 La Laguna, Tenerife, Spain,Departamento de Astrofisica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain;

    South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa,Southern African Large Telescope Foundation, PO Box 9, Observatory 7935, South Africa;

    European Southern Observatory, Alonso de Cordova 3107,19001 Casilla, Santiago, Chile;

    Centro de Astrobiologia, CSIC-INTA, Carretera de Torrejon a Ajalvir, km 4, E-28850 Torrejon de Ardoz, Spain;

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

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);美国《化学文摘》(CA);
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类
  • 关键词

相似文献

  • 外文文献
  • 中文文献
  • 专利
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号