Magnetic fields generated by r-modes in accreting quark stars

被引：7

作者：

Bonanno, L. ^{[1
,4
]}

Cuofano, C. ^{[2
,3
]}

Drago, A. ^{[2
,3
]}

Pagliara, G. ^{[1
]}

Schaffner-Bielich, J. ^{[1
]}

机构：

[1] Heidelberg Univ, Inst Theoret Phys, D-69120 Heidelberg, Germany

[2] Univ Ferrara, Dipartmento Fis, I-44100 Ferrara, Italy

[3] INFN Sez Ferrara, I-44100 Ferrara, Italy

[4] Goethe Univ Frankfurt, Inst Theoret Phys, D-60438 Frankfurt, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2011年 / 532卷

关键词：

X-rays: binaries; gravitational waves; magnetic fields; instabilities; pulsars: general; DIRECT URCA PROCESSES; NPE-MU MATTER; BULK VISCOSITY; NEUTRON-STARS; DIFFERENTIAL ROTATION; STRANGE STARS; GRAVITATIONAL-RADIATION; STELLAR INTERIORS; HYBRID STARS; INSTABILITY;

D O I：

10.1051/0004-6361/201116661

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We show that the r-mode instability can generate strong toroidal fields in the core of accreting millisecond quark stars by inducing differential rotation. We follow the spin frequency evolution on a long time-scale, taking into account the magnetic damping rate in the evolution equations of r-modes. The maximum spin frequency of the star is only marginally lower than without the magnetic field. The late-time evolution of the stars that enter the r-mode instability region is instead quite different if the generated magnetic fields are taken into account: they leave the millisecond pulsar region and become radio pulsars.

引用

页数：7

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