Formation of neutron star / black hole binaries and their merger rate in the local Universe

中子星/黑洞双星的形成及其在当地宇宙中的合并率

• 批准号: 231548287
• 负责人: Professor Dr. Thomas Tauris
• 金额: --
• 依托单位: Institut for Fysik og Astronomi
• 依托单位国家: 德国
• 项目类别: Research Grants
• 财政年份: 2013
• 资助国家: 德国
• 起止时间: 2012-12-31 至 2019-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/231548287?language=en
• 关键词: Formation; neutron; star; black; hole

The expected detection of gravitational waves will open a new window to the Universe and compliment our knowledge of astrophysical sources obtained from photons and neutrinos. The advanced LIGO (Laser Interferometer Gravitational-Wave Observatory) detector, together with its European sister VIRGO and the German detector GEO 600, will be operational in 2014 and reach full sensitivity in 2015. The most promising candidate sources for transient burst detections of high-frequency gravitational waves (10 Hz - 10 kHz) are merging neutron stars (NS) and black holes (BH). These compact objects are formed in tight binaries and undergo spiral-in due to continuous emission of gravitational waves until they finally merge in a violent transient event - possibly leading to a short gamma-ray burst. The main aim of this project is to calculate theoretically the rate of such merging NS/BH in the local Universe using our best up-to-date knowledge of stellar and binary evolution. These results will be compared to the upcoming LIGO detection rates which will enable us to better constrain the input physics behind key binary stellar interactions such as mass and angular momentum loss, common envelopes, evolution of naked helium stars, the role of rapid stellar rotation in massive binaries and, finally, the momentum kick imparted to newborn NS and BH. A second aim of this project is to better understand - and to quantify - the formation, the location, the properties and the lifetimes of Galactic recycled radio pulsars orbiting NS or BH. Whereas we know of 9 radio pulsars orbiting another NS we still have no detections of a radio pulsar orbiting a BH. With this project we hope to gain theoretical knowledge about such systems which will enhance the chance of success in future radio surveys. A recycled pulsar is formed when an old NS is spun up to a high spin frequency via accretion of mass and angular momentum from a companion star in a close binary system. Many aspects of this mass-transfer process and the accretion physics involved are not well understood but play a crucial role for recycling radio pulsars to high spin rates and low B-fields, which make them detectable for billions of years to follow. A third outcome of this study is therefore a better knowledge of the evolution of high-mass X-ray binaries which again can be confronted with observations. To model the population of compact binaries the evolution of a large sample of binary star systems is needed - from the zero age main sequence, via mass transfer and supernova explosions - in order to predict the number of both observable radio pulsars orbiting NS and BH as well as the advanced LIGO detection rate of mergers. To achieve these goals we make use of advanced population synthesis techniques with Monte Carlo simulations and explore new aspects of massive binary stellar evolution for the first time.

重力波的预期检​​测将为宇宙打开一个新窗口，并补充我们对从光子和中微子获得的天体物理来源的了解。先进的LIGO（激光干涉仪重力 - 波段）探测器及其欧洲姊妹处女座和德国探测器Geo 600将于2014年运作，并在2015年达到完全敏感性。瞬态爆发检测最有前途的候选候选象征，用于高频引力浪潮（10 Hz-10 Hz-10 Hz-10 kHz）（10 Hz-10 kHz）（BHS）（BHS）（BH）（BH）（BH）（BH）（BH）（BH）。这些紧凑的物体以紧密的二进制形式形成，并且由于引力波的连续发射，直到最终在剧烈的短暂事件中合并为止 - 可能导致短伽马射线爆发。该项目的主要目的是从理论上计算当地宇宙中这种合并NS/BH的速率，使用我们对恒星和二进制进化的最佳了解。这些结果将与即将到来的LIGO检测率进行比较，这将使我们能够更好地限制关键二元恒星相互作用的输入物理，例如质量和角动量损失，常见信封，裸氦星的演变，巨大的二进制中快速恒星旋转的作用，最终，动力踢踢了瞬间的启发，即势力踢出的newborn nes and Newborn ns and bhh。该项目的第二个目的是更好地理解 - 并量化 - 银河回收的无线电脉冲星的地层，位置，特性和寿命。尽管我们知道有9个旋转另一个NS的无线电脉冲星，但我们仍然无法检测到旋转BH的无线电脉冲星。有了这个项目，我们希望获得有关此类系统的理论知识，这将增强未来无线电调查中成功的机会。当旧的NS通过从近距离二元系统中的伴侣恒星中积聚到质量和角动量时，就会形成回收的脉冲星。这种质量转移过程和所涉及的积物物理学的许多方面尚不清楚，但对于将无线电脉冲星回收至高自旋速率和低B场的关键作用，这使得它们在随后的数十亿年内可检测到。因此，这项研究的第三个结果是对高质量X射线二进制的进化有了更好的了解，这可以再次与观察结果面对面。为了模拟紧凑型二进制文件的种群，需要大量二进制星系的演变 - 从零年龄的主要序列（通过传质和超新星爆炸），以预测可观察到的无线电脉冲脉冲NS和BH的可观察到的无线电脉冲脉冲的数量，以及Advanced的合并合并率。为了实现这些目标，我们利用蒙特卡洛模拟的先进人群合成技术，并首次探索了大规模二元恒星进化的新方面。