Sinking of a magnetically confined mountain on an accreting neutron star

被引：29

作者：

Wette, K. ^{[1
]}

Vigelius, M. ^{[2
]}

Melatos, A. ^{[2
]}

机构：

[1] Australian Natl Univ, Ctr Gravitat Phys, Canberra, ACT 0200, Australia

[2] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2010年 / 402卷 / 02期

关键词：

accretion; accretion discs; stars: magnetic fields; stars: neutron; pulsars: general; RADIATION MAGNETOHYDRODYNAMICS CODE; 2 SPACE DIMENSIONS; FIELD EVOLUTION; GRAVITATIONAL-RADIATION; ASTROPHYSICAL FLOWS; MILLISECOND PULSARS; RADIO PULSARS; MASS; DECAY; CRUST;

D O I：

10.1111/j.1365-2966.2009.15937.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We perform ideal-magnetohydrodynamic axisymmetric simulations of magnetically confined mountains on an accreting neutron star, with masses less than or similar to 0.12 M-circle dot. We consider two scenarios, in which the mountain sits atop a hard surface or sinks into a soft, fluid base. We find that the ellipticity of the star, due to a mountain grown on a hard surface, approaches similar to 2 x 10(-4) for accreted masses greater than or similar to 1.2 x 10(-3) M-circle dot, and that sinking reduces the ellipticity by between 25 and 60 per cent. The consequences for gravitational radiation from low-mass X-ray binaries are discussed.

引用

页码：1099 / 1110

页数：12

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