X-ray Bursts, Superbursts, and Outbursts from Accreting Neutron Stars: What heats the Interior?

中子星是宇宙中最密集的天体，自从它们被首次发现以来，就一直吸引着理论家和观测者。 尽管在过去的四十年里对电磁频谱进行了大量的观测，但在其内部深处发生的许多事情仍然是不可理解的。 由于X射线望远镜，如钱德拉，实验室核实验，也许在不久的将来引力波探测器，如激光干涉引力波天文台（LIGO），中子星星物理学的知识正在迅速增长。 事实上，美国国家科学院的报告《连接夸克与宇宙：新世纪的11个科学问题》（Connecting Quarks with the Cosmos：Eleven Science Questions for the New世纪）将超高密度和温度下物质的性质确定为21世纪的11个关键科学问题之一。 此外，最近的2010年十年巡天“新世界，新视野”确定了恒星和恒星演化的前沿问题之一，“是什么控制了致密恒星残余物的质量，半径和自旋？“该项目开发的模型将使现有和未来的观测能够进一步加深我们对致密物质和恒星演化物理学的了解。该项目包括招募下一代科学家和向公众提供信息的活动，并提供为期三年的研究生支持。 该项目支持本科生协助运行项目中使用的代码，并协助使用开源梅萨恒星演化代码测试，维护和发布教育资源。 PI在本科生的帮助下将使用梅萨开发问题集，情节和动画。 密歇根州立大学是一所拥有多元化学生群体的大型公立大学，将成为开发这些资源的试验田。 特别是，PI将开发问题“模板”，使学生可以更容易地使用梅萨探索恒星物理。 这些工具将张贴在梅萨网络论坛http://mesastar.org/上。 张贴这些工具将使其他教师更容易采用梅萨进行课堂教学，并有望激励其他人张贴他们的结果。 为了向公众宣传，PI将把在该奖项任期内取得的发现纳入密歇根州立大学艾布拉姆斯天文馆的公开演讲中。从技术上讲，对于低质量X射线双星中的中子星，其中中子星吸积氢或氦丰富的物质，存在大量跨越广泛时间尺度的时间依赖现象。星星。 在吸积过程中，被吸积物质的失控热核燃烧可以观察到I型X射线爆发。 观测到的数千次X射线爆发、更罕见、能量更高的超级爆发以及冷却瞬变都编码了有关致密物质的物理信息，特别是中子星星的亚核密度“地壳”。 十多年来，中子星星外壳的模型一直认为这三层是相互影响的：短暂的爆发产生了超级爆发的燃料，超级爆发的灰烬形成了外壳，外壳中的核反应加热了外壳。 然而，在过去的几年里，越来越多的证据表明，这张照片充其量是不完整的，还有额外的，强大的，浅的-而且还没有被确认的-热源存在。 该项目将利用最新的核反应物理学，包括新发现的中微子冷却机制，生成中子星星地壳的全球模型，并利用现有和未来对冷却瞬变、超级爆发和X射线爆发的观测，限制地壳中额外加热的深度和强度。 此外，他们还将预测地壳成分作为密度函数的独特性，这对于确定中子星星的热和磁演化以及维持质量四极的能力非常重要。

Neutron stars are the densest objects in the Universe and have fascinated theorists and observers since they were first conjectured. Despite a wealth of observations across the electromagnetic spectrum over the last four decades, much of what happens in their deep interior remains inscrutable. Owing to X-ray telescopes such as Chandra, laboratory nuclear experiments, and perhaps in the near future gravitational wave detectors such as the Laser Interferometer Gravitational Wave Observatory (LIGO), knowledge of neutron star physics is growing rapidly. Indeed, the National Academy report, "Connecting Quarks with the Cosmos: Eleven Science Questions for the New Century" identified the nature of matter at exceedingly high density and temperature as one of the eleven critical science questions for the twenty-first century. Moreover, the recent 2010 Decadal Survey "New Worlds, New Horizons" identifies as one of its Frontier questions for Stars and Stellar Evolution, "What controls the mass, radius, and spin of compact stellar remnants?" The models developed in this project will enable existing and future observations to further our knowledge of the physics of dense matter and stellar evolution.This project includes activities to recruit the next generation of scientists and to inform the public and provides support of a graduate student for three years. The project supports an undergraduate to assist with running the codes used in the project, and to assist with testing, maintaining, and posting educational resources using the open-source MESA stellar evolution code. The PI with assistance from the undergraduate will develop problem sets, plots, and animations using MESA. Michigan State is a large public institution with a diverse student population and will serve as a testbed for development of these resources. In particular, the PI will develop problem "templates" so that students can more readily use MESA to explore stellar physics. These tools will be posted on the MESA web forum http://mesastar.org/. Posting these tools will make it easier for other instructors to adopt MESA for classroom instruction and is expected to motivate others to post their results as well. For public outreach, the PI will incorporate discoveries made during the tenure of this award into public talks at Michigan State's Abrams Planetarium.More technically, for neutron stars in low-mass X-ray binaries, in which the neutron star accretes hydrogen- or helium-rich material, there is a wealth of time-dependent phenomena spanning a wide range of timescales. During accretion, runaway thermonuclear burning of the accreted matter is observable as a Type I X-ray burst. The thousands of observed X-ray bursts, the rarer and more energetic superbursts, and the cooling transients all encode information about the physics of dense matter, in particular the sub-nuclear-density "crust" of the neutron star. For over a decade the model of the neutron star's crust has been that the three layers influence each other: the short bursts produce the fuel for superbursts, superburst ashes form the outer crust, and nuclear reactions in the crust heat the envelope. In the last several years, however, evidence has steadily mounted that this picture is at best incomplete, and that additional, strong, shallow---and as yet unidentified---heat sources are present. This project will generate global models of the neutron star crust with the latest nuclear reaction physics, including a newly discovered neutrino cooling mechanism, and use existing and future observations of cooling transients, superbursts, and X-ray bursts to constrain the depth and strength of additional heating in the crust. In addition, they will make predictions for the uniqueness of the crust composition as a function of density, which is important for determining the neutron star's thermal and magnetic evolution as well as its ability to sustain a mass quadrupole.