The neutrino gravitational memory from a core collapse supernova: phenomenology and physics potential
The neutrino gravitational memory from a core collapse supernova: phenomenology and physics potential
复制标题
DOI：
10.1088/1475-7516/2021/07/055
复制
发表时间：
2021-05
影响因子：
6.4
通讯作者：
Mainak Mukhopadhyay;Carlos A. Cardona;C. Lunardini
中科院分区：
文献类型：
--
作者：
Mainak Mukhopadhyay;Carlos A. Cardona;C. Lunardini
广义相对论预言，来自非对称发射源的物质或辐射的通过应该引起局部时空度量的永久变化。这种现象被称为引力记忆效应，从未被观察到，然而超新星中微子长期以来一直被认为是未来探测的一个有希望的途径。随着分赫兹引力波干涉仪的出现，观测超新星中微子记忆将成为可能，这对多信使天文学和引力测试具有重要意义。在这项工作中，我们开发了一个唯象（解析）玩具模型的超新星中微子记忆效应，这是总体上与数值模拟的结果相一致。这种描述，然后推广到几个感兴趣的案例研究。我们发现，对于一个银河系超新星，无量纲应变，h（t），是一个订单<$10 -22 - 10-21，并在一个典型的时间尺度，变化范围为<$0.1 - 10秒，取决于中微子发射的各向异性的时间演化。特征应变hc（f）在频率f max = 10-1Hz时具有最大值。𝒪记忆应变的时间和频率结构的详细特征将告诉我们坍缩核心附近的物质动力学，并允许区分不同的恒星坍缩场景。像DECIGO和BBO这样的下一代引力波探测器将对典型星系距离及更远距离的超新星的中微子记忆效应敏感; Ultimate DECIGO的可探测距离超过10 Mpc。
General Relativity predicts that the passage of matter or radiation from an asymmetrically-emitting source should cause a permanent change in the local space-time metric. This phenomenon, called the gravitational memory effect, has never been observed, however supernova neutrinos have long been considered a promising avenue for its detection in the future. With the advent of deci-Hertz gravitational wave interferometers, observing the supernova neutrino memory will be possible, with important implications for multimessenger astronomy and for tests of gravity. In this work, we develop a phenomenological (analytical) toy model for the supernova neutrino memory effect, which is overall consistent with the results of numerical simulations. This description is then generalized to several case studies of interest. We find that, for a galactic supernova, the dimensionless strain, h(t), is of order ∼ 10-22 - 10-21, and develops over a typical time scale that varies between ∼ 0.1 - 10 s, depending on the time-evolution of the anisotropy of the neutrino emission. The characteristic strain, h c(f), has a maximum at a frequency f max ∼ 𝒪(10-1) - 𝒪(1) Hz. The detailed features of the time- and frequency-structure of the memory strain will inform us of the matter dynamics near the collapsed core, and allow to distinguish between different stellar collapse scenarios. Next generation gravitational wave detectors like DECIGO and BBO will be sensitive to the neutrino memory effect for supernovae at typical galactic distances and beyond; with Ultimate DECIGO exceeding a detectability distance of 10 Mpc.