Turbulent magnetic-field amplification in the first 10 milliseconds after a binary neutron star merger: Comparing high-resolution and large-eddy simulations

被引：44

作者：

Aguilera-Miret, Ricard ^{[1
,2
,3
,4
,5
]}

Vigano, Daniele ^{[4
,5
,6
]}

Carrasco, Federico ^{[4
,7
]}

Minano, Borja ^{[1
,2
,3
,4
,5
]}

Palenzuela, Carlos ^{[1
,2
,3
,4
,5
]}

机构：

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

[2] Univ Illes Balears, IAC3, E-07122 Palma De Mallorca, Baleares, Spain

[3] Inst Estudis Espacials Catalunya, E-07122 Palma De Mallorca, Baleares, Spain

[4] Univ Illes Balears, Inst Aplicac Computationals IAC3, E-07122 Palma De Mallorca, Baleares, Spain

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

[6] CSIC, Ins Space Sci, ICE, Barcelona 08193, Spain

[7] Max Planck Inst Gravitat Phys, D-14476 Potsdam, Germany

来源：

PHYSICAL REVIEW D | 2020年 / 102卷 / 10期

基金：

欧盟地平线“2020”;

关键词：

INSTABILITY; MODELS;

D O I：

10.1103/PhysRevD.102.103006

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The detection of binary neutron star mergers represents one of the most important and complex astrophysical discoveries of the recent years. One of the unclear aspects of the problem is the turbulent magnetic field amplification, initially triggered by the Kelvin-Helmholtz instability at much smaller scales than any reachable numerical resolution nowadays. Here we present numerical simulations of the first 10 milliseconds of a binary neutron star merger. First, we confirm in detail how the simulated amplification depends on the numerical resolution and is distributed on a broad range of scales, as expected from turbulent magnetohydrodynamics theory. We find that an initial large-scale magnetic field of 10(11) G inside each star is amplified in the remnant to root-mean-square values above 10(16) G within the first 5 milliseconds for our highest-resolution run. Then, we run large eddy simulations, exploring the performance of the subgrid-scale gradient model, already tested successfully in previous turbulent box simulations. We show that the addition of this model is especially important in the induction equation, since it leads to an amplification of the magnetic field comparable to a higher-resolution run, but with a greatly reduced computational cost. In the first 10 milliseconds, there is no clear hint for an ordered, large-scale magnetic field, which should indeed occur in longer timescales through magnetic winding and the magnetorotational instability.

引用

页数：15

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