Some Thermodynamic Problems of Neutron Stars

中子星的一些热力学问题

• 批准号: 9013290
• 负责人: Sachiko Tsuruta
• 金额: $ 6.98万
• 依托单位: Montana State University
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 1991
• 资助国家: 美国
• 起止时间: 1991-03-01 至 1993-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9013290&HistoricalAwards=false
• 关键词: Some; Thermodynamic; Problems; Neutron; Stars

The idea that highly condensed stars too massive to become white dwarfs could exist as solid "neutron stars" was first advanced by J. Robert Oppenheimer in 1939. Since that time the idea that supernovae nuclei collapse directly into neutron stars (sometimes in a rotating, magnetized form called "pulsars") is now widely accepted. Despite this progress, rather little is understood about their radiation and internal structural properties. Such phenomena as "star quakes" in pulsars suggest that the there are at least two of neutrons consisting of a liquid core and a solid "crust". The Principal Investigator (PI) will study a variety of topics dealing with the interiors of neutron stars, including the transport of radiation from their interior to the surface, and vice versa just after a supernovae explosion, which can be used to make predictions that can be matched with observations, either from the ground or from X-ray detectors on spacecraft. She will include modern "equation of state" microphysics into these calculations and will determine what effects magnetic fields and exotic particles called "WIMPS" have on these models. This work coincides with the expected detection of the nucleus of the supernova in the Magellanic Cloud, SN1987a, which should become visible shortly as emission from the exploding ejecta becomes faint. It is anticipated that the detection (and even non-detection) of this remnant will elucidate which of various competing physical processes are important in neutron stars. The work supported by this award should play a key part in this understanding.

高度凝聚的恒星质量太大而不会变成白色的观点 矮星可以作为固体“中子星”存在， 罗伯特·奥本海默，1939年。 从那时起， 超新星核直接坍缩成中子星（有时 以旋转的、磁化的形式被称为“磁共振”）现在广泛地 接纳的话 尽管取得了这些进展，但人们对 它们的辐射和内部结构特性。 此类现象 因为彗星上的“星星地震”表明至少有两次 由液态核和固态“壳”组成的中子。 的 主要研究者（PI）将研究各种主题， 与中子星内部的联系，包括 从内部到表面的辐射，反之亦然， 在超新星爆炸后，可以用来预测 可以与地面观测相匹配， 来自宇宙飞船上的X射线探测器。 她将包括现代 “状态方程”微观物理学到这些计算，并将 确定什么影响磁场和外来粒子所谓的 “WIMPS”在这些模型上。 这项工作恰逢 这颗超新星的核心是在 麦哲伦星云，SN1987a，应该很快就可以看到， 爆炸喷出物的辐射变得微弱。 是 预计检测（甚至不检测）这一点， 遗迹将阐明各种竞争性的物理 过程在中子星中很重要。 支持的工作 这个奖项应该在这一理解中发挥关键作用。