发表机构
Max Planck Institute for Gravitational Physics (Albert Einstein Institute); Leibniz Universität Hannover（马克斯·普朗克引力物理研究所（爱因斯坦研究所）; 汉诺威莱布尼茨大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文基于双组分模型分析脉冲星自转噪声，区分扩散与守恒角动量，用高斯过程方法证明全状态观测可检验平稳性，为引力波与射电计时联合观测铺路。
AI 中文摘要
我们基于物理动机的双组分自转游走模型，对脉冲星自转噪声进行了分析。我们聚焦于两种模型，它们以总角动量动力学为区分特征：一种是奇异且非平稳的模型，其总角动量具有扩散性；另一种是极简且平稳的模型，其总角动量守恒。我们开发了可扩展的高斯过程方法，并利用模拟数据表明，在具备全状态观测（即同时获得壳层和超流旋转状态的独立数据）的情况下，这两种模型完全可检验且可区分。这为检验脉冲星自转噪声的平稳性开辟了道路，可能通过联合连续引力波观测和脉冲星射电计时来实现。然而，当仅有一个分量可观测时，稳健的推断和预测更难实现，且依赖于先验和数据质量。
英文摘要
We present an analysis of pulsar spin noise based on physically-motivated two-component models of spin wandering. We focus on two models, distinguished by their total angular momentum dynamics: a singular, nonstationary model with a diffusive total angular momentum, and a minimal, stationary model anchored on a conserved total angular momentum. We develop scalable Gaussian process methods and, using mock data, show that the two models are fully testable and distinguishable with full-state observations, i.e., simultaneous independent data on the crust and the superfluid rotational states. This paves a path to testing stationarity in pulsar spin noise, potentially achievable with joint continuous gravitational wave observations and radio timing of pulsars. However, robust inferences and predictions are harder to achieve, and depend on the priors and data quality, when only one component is observationally accessible.
Comments21 pages + refs, 12 figures, comments welcome
