scholarly journals Spin evolution of accreting neutron stars: Nonlinear development of ther-mode instability

2007 ◽  
Vol 76 (6) ◽  
Author(s):  
Ruxandra Bondarescu ◽  
Saul A. Teukolsky ◽  
Ira Wasserman
Keyword(s):  
Neutron Stars ◽  
Mode Instability ◽  
Nonlinear Development ◽  
Spin Evolution

scholarly journals THE R-MODE INSTABILITY IN ROTATING NEUTRON STARS

2001 ◽  
Vol 10 (04) ◽  
pp. 381-441 ◽  
Author(s):  
NILS ANDERSSON ◽  
KOSTAS D. KOKKOTAS
Keyword(s):  
Neutron Stars ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Binary Systems ◽  
Current Understanding ◽  
Mode Instability ◽  
Spin Evolution ◽  
Astrophysical Significance

In this review we summarize the current understanding of the gravitational-wave driven instability associated with the so-called r-modes in rotating neutron stars. We discuss the nature of the r-modes, the detailed mechanics of the instability and its potential astrophysical significance. In particular we discuss results regarding the spin-evolution of nascent neutron stars, the detectability of r-mode gravitational waves and mechanisms limiting the spin-rate of accreting neutron stars in binary systems.

scholarly journals Nonlinear Development of the Secular Bar‐Mode Instability in Rotating Neutron Stars

2004 ◽  
Vol 617 (1) ◽  
pp. 490-499 ◽  
Author(s):  
Shangli Ou ◽  
Joel E. Tohline ◽  
Lee Lindblom
Keyword(s):  
Neutron Stars ◽  
Mode Instability ◽  
Nonlinear Development

scholarly journals Spinning down newborn neutron stars: Nonlinear development of ther-mode instability

2009 ◽  
Vol 79 (10) ◽  
Author(s):  
Ruxandra Bondarescu ◽  
Saul A. Teukolsky ◽  
Ira Wasserman
Keyword(s):  
Neutron Stars ◽  
Mode Instability ◽  
Nonlinear Development

R-mode oscillations of rapidly rotating Newtonian stars: A new numerical scheme and its application to the spin evolution of neutron stars

2000 ◽  
Vol 62 (8) ◽  
Author(s):  
Shigeyuki Karino ◽  
Shin’ichirou Yoshida ◽  
Shijun Yoshida ◽  
Yoshiharu Eriguchi
Keyword(s):  
Neutron Stars ◽  
Numerical Scheme ◽  
Spin Evolution

scholarly journals Pulsars & Magnetars

2008 ◽  
Vol 4 (S259) ◽  
pp. 485-492 ◽  
Author(s):  
Michael Kramer
Keyword(s):  
Magnetic Field ◽  
Neutron Stars ◽  
Evolutionary Sequence ◽  
Radio Pulsars ◽  
Observable Universe ◽  
Spin Evolution ◽  
Field Strengths

AbstractThe largest magnetic field encountered in the observable Universe can be found in neutron stars, in particular in radio pulsars and magnetars. While recent discoveries have slowly started to blur the distinction between these two classes of highly magnetized neutron stars, it is possible that both types of sources are linked via an evolutionary sequence. Indications for this to be the case are obtained from observations of the spin-evolution of pulsars. It is found that most young pulsars are heading across the top of the main distribution of radio pulsars in the P–Ṗ-diagram, suggesting that at least a sub-class of young pulsars may evolve into objects with magnetar-like magnetic field strengths. Part of this evolutionary sequence could be represented by RRATs which appear to share at least in parts properties with both pulsars and magnetars.

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