Superfluid Dynamics as Inferred from the Spin Evolution of Neutron Stars

量子物理学・ナノサイエンス第386回セミナー

概要

Neutron stars are objects that contain the most abundant and highest temperature superfluid in the observable universe. One way to gain information about the superfluid interior structure and dynamics of neutron stars is to study their rotational evolution. Pulsar glitches, sudden spin-ups in the rotation rate of neutron stars, are direct manifestation of their superfluidity nature. Various phases of pulsar glitches, namely formation, magnitude and relaxation, enable us to infer invaluable information and put constraints on the coupling between the superfluid and normal matter, effective masses of protons and neutrons, internal temperature of the sources, internal magnetic field configuration, equation of state, and more…[1]. In this talk, I will attempt to explain how the glitch data can be used to test existing models and to deduce related microphysical parameters by invoking application of the vortex creep model to the observations [2,3,4]. I will also show how the imprints of superfluidity can be identified from the oscillations observed in the deceleration rate of neutron stars [5].

　　　　
• [1]　Gügercinoğlu & Alpar, 2020, MNRAS, 496, 2506
• [2]　Gügercinoğlu, Ge, Yuan, Zhou, 2022, MNRAS, 511, 425
• [3]　Zhou et al., 2023, MNRAS, 519, 74
• [4]　Liu et al., 2023, arXiv:2312.04305
• [5]　Gügercinoğlu, Köksal, Güver, 2023, MNRAS, 518, 5734

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• 量子物理学・ナノサイエンス第386回セミナー

• 東京工業大学理学院量子物理学・ナノサイエンスを拓く量子物理学拠点 共催