Modelling Neutron-Star Ocean Dynamics

被引:0
|
作者
Gittins, Fabian [1 ]
Celora, Thomas [1 ]
Beri, Aru [2 ]
Andersson, Nils [1 ]
机构
[1] Univ Southampton, Math Sci & STAG Res Ctr, Southampton SO17 1BJ, England
[2] IISER Mohali, Dept Phys Sci, Manauli 140306, Punjab, India
关键词
asteroseismology; neutron stars; oscillations; rotation; X-ray bursts; X-RAY-BURSTS; R-MODES; RELATIVISTIC STARS; PLANETARY-WAVES; ROTATING STARS; OSCILLATIONS; FREQUENCY; BINARY; DISCOVERY; EQUATIONS;
D O I
10.3390/universe9050226
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We revisit the calculation of mode oscillations in the ocean of a rotating neutron star, which may be excited during thermonuclear X-ray bursts. Our present theoretical understanding of ocean modes relies heavily on the traditional approximation commonly employed in geophysics. The approximation elegantly decouples the radial and angular sectors of the perturbation problem by neglecting the vertical contribution from the Coriolis force. However, as the implicit assumptions underlying it are not as well understood as they ought to be, we examine the traditional approximation and discuss the associated mode solutions. The results demonstrate that, while the approximation may be appropriate in certain contexts, it may not be accurate for rapidly rotating neutron stars. In addition, using the shallow-water approximation, we show analytically how the solutions that resemble r-modes change their nature in neutron-star oceans to behave like gravity waves. We also outline a simple prescription for lifting Newtonian results in a shallow ocean to general relativity, making the result more realistic.
引用
收藏
页数:19
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