Using an adapted version of the SGRID code, we construct for the first time consistent quasi-equilibrium configurations for a binary system consisting of two neutron stars in which each is admixed with dark matter. The stars are modelled as a system of two non-interacting fluids minimally coupled to gravity. For the fluid representing baryonic matter the SLy equation of state is used, whereas the second fluid, which corresponds to dark matter, is described using the equation of state of a degenerate Fermi gas. We consider two different scenarios for the distribution of the dark matter. In the first scenario the dark matter is confined to the core of the star, whereas in the second scenario the dark matter extends beyond the surface of the baryonic matter, forming a halo around the baryonic star. The presence of dark matter alters the star's reaction to the companion's tidal forces, which we investigate in terms of the coordinate deformation and mass shedding parameters. The constructed quasi-equilibrium configurations mark the first step towards consistent numerical-relativity simulations of dark matter admixed neutron star binaries.
$g$-mode oscillations of dark matter admixed neutron stars
Inter-University Centre for Astronomy and Astrophysics（大学间天文与天体物理中心）；Department of Physics and Astronomy, California State University Long Beach（加州州立大学长滩分校物理与天文学系）
Scalar and vector dark matter admixed neutron stars with linear and quadratic couplings
Università di Salerno（萨莱诺大学）；INFN, Gruppo collegato di Salerno（意大利国家核物理研究所萨莱诺协作组）；Institute for Particle Physics Phenomenology (IPPP), Department of Physics, Durham University（达勒姆大学粒子物理现象学研究所）
Observational bounds on Dark Matter Admixed Neutron Stars from Gravitational Wave Data
Instituto Nacional de Pesquisas Espaciais（巴西国家空间研究所）；Universidade Federal do Rio Grande do Sul（南里奥格兰德联邦大学）；Universidade Federal do Espírito Santo（圣埃斯皮里图联邦大学）
Two-fluid $f$-mode oscillations of dark-matter-admixed neutron stars
Institute of Astrophysics, Central China Normal University（华中师范大学天文物理研究所）；School of Optoelectronic Information Engineering, Institute of Astronomy and High Energy Physics, Hubei University of Education（湖北教育学院光电信息工程学院、天体与高能物理研究所）；School of Mathematics and Physics, China University of Geosciences（中国地质大学数学与物理学院）；School of Physics, Huazhong University of Science and Technology（华中科技大学物理学院）；INFN Sezione di Catania, Dipartimento di Fisica, Universitá di Catania（意大利国家核物理研究院卡塔尼亚分部、卡塔尼亚大学物理系）
Equilibrium Structure and Radial Oscillations of Dark Matter Admixed Neutron Stars
在[Leung等人，Phys. Rev. D 84，107301（2011）]，我们提出了我们的结果，使用广义相对论双流体形式主义来研究简并暗物质和正常核物质的混合物的流体静力平衡构型。在这项工作中，我们提出了更多的分析，以补充我们以前的研究结果。我们详细研究了这些致密星的径向振荡模式。我们发现，这些恒星一般有两类振荡模式。对于给定的恒星总质量，第一类模式对暗物质粒子质量不敏感。当暗物质的质量分数趋于零时，它们也适当地还原为具有相同总质量的相应普通中子星的振荡模式。另一方面，第二类模式主要是由于暗物质流体。在小的暗物质质量分数限制，这些模式的特点是纯粹的暗物质的振荡，而正常的物质基本上是在休息。在两种流体的质量分数相当的中间状态下，正常物质与暗物质由于它们通过重力的耦合而振荡。与第一类模式相反，这些暗物质主导模式的频率敏感地依赖于暗物质粒子的质量。
Bose-Einstein Condensate Dark Matter in the Core of Neutron Stars: Implications for Gravitational-wave Observations
International Centre for Theoretical Sciences, Tata Institute of Fundamental Research（国际理论科学中心，塔塔基础研究所）；Inter-University Centre for Astronomy and Astrophysics (IUCAA)（大学间天文学与天体物理中心）；OzGrav-ANU, Centre for Gravitational Astrophysics, College of Science, The Australian National University（澳引力-澳大利亚国立大学，引力天体物理学中心，理学院，澳大利亚国立大学）
Fudan University（复旦大学）；INFN Sezione di Catania, Dipartimento di Fisica, Universitá di Catania（意大利国家核物理研究所卡塔尼亚分部、物理学系、卡塔尼亚大学）；University of Geosciences, Wuhan（武汉地球科学学院）；Shanghai Research Center for Theoretical Nuclear Physics, NSFC, Fudan University（国家自然科学基金委上海理论核物理研究中心，复旦大学）
Universality of dual mass-scaled fundamental modes in two-fluid neutron stars with mirror dark matter
Kochi University（高知大学）；RIKEN Center for Interdisciplinary Theoretical and Mathematical Sciences (iTHEMS), RIKEN（理化学研究所交叉理论数学科学中心（iTHEMS））；Kochi University of Technology（高知工科大学）；University of Tübingen（蒂宾根大学）；Indian Institute of Science（印度科学学院）；Institute of Physics of the Czech Academy of Sciences (FZU)（捷克科学院物理研究所）
Implications of Fermionic Dark Matter Interactions on Anisotropic Neutron Stars
Birla Institute of Technology and Science - Pilani（比拉理工学院-皮拉尼分校）；Inter-University Centre for Astronomy and Astrophysics（大学天文学与天体物理中心）；Tezpur University（特普尔大学）
