HYDRODYNAMICAL NEUTRON STAR KICKS IN THREE DIMENSIONS

作者：Wongwathanarat Annop^*; Janka Hans Thomas; Mueller Ewald

来源：Astrophysical Journal Letters, 2010, 725(1): L106-L110.

DOI：10.1088/2041-8205/725/1/L106

• pulsars: general
• stars: kinematics and dynamics
• stars: neutron
• supernovae: general

Using three-dimensional (3D) simulations of neutrino-powered supernova explosions, we show that the hydrodynamical kick scenario proposed by Scheck et al. on the basis of two-dimensional (2D) models can yield large neutron star (NS) recoil velocities also in 3D. Although the shock stays relatively spherical, standing accretion-shock and convective instabilities lead to a globally asymmetric mass and energy distribution in the post-shock layer. An anisotropic momentum distribution of the ejecta is built up only after the explosion sets in. Total momentum conservation implies the acceleration of the NS on a timescale of 1-3 s, mediated mainly by long-lasting, asymmetric accretion downdrafts and the anisotropic gravitational pull of large inhomogeneities in the ejecta. In a limited set of 15 M-circle dot models with an explosion energy of about 10(51) erg, this stochastic mechanism is found to produce kicks from <100 km s(-1) to greater than or similar to 500 km s(-1), and kicks greater than or similar to 1000 km s(-1) seem possible. Strong rotational flows around the accreting NS do not develop in our collapsing, non-rotating progenitors. The NS spins therefore remain low with estimated periods of similar to 500-1000 ms and no alignment with the kicks.

• 出版日期2010-12-10