Probing the neutron star matter properties with asteroseismology

2016 Fiscal Year Final Research Report

• Project/Area Number: 26800133
• Research Category: Grant-in-Aid for Young Scientists (B)
• Allocation Type: Multi-year Fund
• Research Field: Particle/Nuclear/Cosmic ray/Astro physics
• Research Institution: National Astronomical Observatory of Japan
• Principal Investigator: Sotani Hajime 国立天文台, 理論研究部, 特任助教 (70386720)
• Project Period (FY): 2014-04-01 – 2017-03-31
• Keywords: 中性子星 / 状態方程式 / 星震学

Outline of Final Research Achievements

Neutron stars, which form via supernovae, are in extreme conditions. The density inside the stars becomes significantly over the standard nuclear density. So, via terrestrial nuclear experiments it is very difficult to make an constraint on the interior information of neutron stars. Thus, we focus on the oscillations of neutron stars to extract the interior information. By comparing the quasi-periodic oscillations observed in the giant flares with the crustal torsional oscillations, we set out to get the constraint on the nuclear saturation parameters. In particular, we consider the oscillation in the bubble phase. If our scenario is correct, our results show the evidence of the pasta structure in the neutron star crust observationally.

Free Research Field

宇宙物理