FORMATION OF STABLE MAGNETARS FROM BINARY NEUTRON STAR MERGERS

By B. Giacomazzo, R. Perna. 2013

146 citations recorded by the source corpus.

By performing fully general relativistic magnetohydrodynamic simulations of binary neutron star mergers, we investigate the possibility that the end result of the merger is a stable magnetar. In particular, we show that, for a binary composed of two equal-mass neutron stars (NSs) of gravitational mass M ∼ 1.2 M☉ and equation of state similar to Shen et al. at high densities, the merger product is a stable NS. Such NS is found to be differentially rotating and ultraspinning with spin parameter J/M2 ∼ 0.86, where J is its total angular momentum, and it is surrounded by a disk of ≈0.1 M☉. While in our global simulations the magnetic field is amplified by about two orders of magnitude, local simulations have shown that hydrodynamic instabilities and the onset of the magnetorotational instability could further increase the magnetic field strength up to magnetar levels. This leads to the interesting possibility that, for some NS mergers, a stable and magnetized NS surrounded by an accretion disk could be formed. We discuss the impact of these new results for the emission of electromagnetic counterparts of gravitational wave signals and for the central engine of short gamma-ray bursts.

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Citations in the corpus

The birth of black holes: neutron star collapse times, gamma-ray bursts and fast radio bursts (2014, background): “…where N(μBNS, σ BNS) specifies a normal distribution with mean μBNS and standard deviation σ BNS. Binary NS mergers are believed to approximately conserve rest mass (Mrest), with 0.01 M of material ejected during the merger (Rezzolla et al. 2011; Giacomazzo & Perna 2013; Hotokezaka et al. 2013).”
THE MILLISECOND MAGNETAR CENTRAL ENGINE IN SHORT GRBs (2015, background): “If Mp is smaller than the nonrotating Tolman-Oppenheimer-Volkoff maximum mass MTOV, the magnetar will be stable in equilibrium state (Cook et al. 1994; Giacomazzo & Perna 2013, Ravi & Lasky 2014).”
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis (2018, background): “…(Baumgarte et al. 2000; Shibata & Taniguchi 2006; Baiotti et al. 2008; Sekiguchi et al. 2011; Bernuzzi et al. 2016), or long-lived massive NS remnants, expected to be stable on secular timescales or, in some cases, indefinitely (Giacomazzo & Perna 2013; Foucart et al. 2016a; Radice et al. 2018a).”
Optical and X-ray emission from stable millisecond magnetars formed from the merger of binary neutron stars (2013, background): “This makes it more likely that a massive NS remnant could remain (e.g.,̈Ozel et al. 2010; Bucciantini et al. 2012; Giacomazzo & Perna 2013; Kiziltan et al. 2013).”
Properties of the Binary Neutron Star Merger GW170817 (2018, background): “Stiffer EOS and lower masses result in the formation of a stable or quasistable NS remnant [145,146].”
Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817 (2017, background): “Mmax, the BNS merger produces an indefinitely stable NS remnant (e.g. Bucciantini et al. 2012; Giacomazzo & Perna 2013).”
A Nearby Repeating Fast Radio Burst in the Direction of M81 (2021, background): “On the other hand, it has been suggested (e.g., Giacomazzo & Perna 2013) that young neutron stars can be formed by compact object mergers, which could occur in the halo.”
The physics of gamma-ray bursts & relativistic jets (2014, background): “On the other hand, if a NS–NS merger leaves behind a supra-massivemillisecondmagnetarwhich is possible based on uncertainties of our understanding of equation-ofstate of nuclear matter [703,830], then very bright electromagnetic counterparts can be detected with gravitational wave bursts without a s”
BRIGHT “MERGER-NOVA” FROM THE REMNANT OF A NEUTRON STAR BINARY MERGER: A SIGNATURE OF A NEWLY BORN, MASSIVE, MILLISECOND MAGNETAR (2013, background): “…the uncertainties of nuclear matter equation-of-state and NS mass distributions of the merger systems, it is possible that at least some NS-NS mergers would leave behind a stable (for hours to days), rapidly rotating NS (e.g. Dai et al. 2006; Fan & Xu 2006; Zhang 2013; Giacomazzo & Perna 2013).”