Universality of the Turbulent Magnetic Field in Hypermassive Neutron Stars Produced by Binary Mergers

被引：32

作者：

Aguilera-Miret, Ricard ^{[1
,2
,3
]}

Vigano, Daniele ^{[2
,3
,4
]}

Palenzuela, Carlos ^{[1
,2
,3
]}

机构：

[1] Univ Illes Balears, Dept Fis, E-07122 Baleares, Spain

[2] Univ Illes Balears, Inst Appl Community & Community Code IAC3, E-07122 Palma De Mallorca, Baleares, Spain

[3] Inst Estudis Espacials Catalunya IEEC, Barcelona 08034, Spain

[4] Inst Space Sci IEEC CSIC, Barcelona 08193, Spain

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2022年 / 926卷 / 02期

基金：

欧洲研究理事会;

关键词：

MODELS;

D O I：

10.3847/2041-8213/ac50a7

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The detection of a binary neutron star (BNS) merger in 2017 through both gravitational waves and electromagnetic emission opened a new era of multimessenger astronomy. The understanding of the magnetic field amplification triggered by the Kelvin-Helmholtz instability during the merger is still a numerically unresolved problem because of the relevant small scales involved. One of the uncertainties comes from the simplifications usually assumed in the initial magnetic topology of merging neutron stars. We perform high-resolution, convergent large-eddy simulations of BNS mergers, following the newly formed remnant for up to 30 ms. Here we specifically focus on the comparison between simulations with different initial magnetic configurations, going beyond the widespread-used aligned dipole confined within each star. The results obtained show that the initial topology is quickly forgotten, in a timescale of a few milliseconds after the merger. Moreover, at the end of the simulations, the average intensity (B similar to 10(16) G) and the spectral distribution of magnetic energy over spatial scales barely depend on the initial configuration. This is expected due to the small-scale efficient dynamo involved, and thus it holds as long as (i) the initial large-scale magnetic field is not unrealistically high (as often imposed in mergers studies), and (ii) the turbulent instability is numerically (at least partially) resolved, so that the amplified magnetic energy is distributed across a wide range of scales and becomes orders of magnitude larger than the initial one.

引用

页数：7

共 55 条

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