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The key role of magnetic fields in binary neutron star mergers

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Abstract

The first multimessenger observation of a binary neutron star (BNS) merger in August 2017 demonstrated the huge scientific potential of these extraordinary events. This breakthrough led to a number of discoveries and provided the best evidence that BNS mergers can launch short gamma-ray burst (SGRB) jets and are responsible for a copious production of heavy r-process elements. On the other hand, the details of the merger and post-merger dynamics remain only poorly constrained, leaving behind important open questions. Numerical relativity simulations are a powerful tool to unveil the physical processes at work in a BNS merger and as such they offer the best chance to improve our ability to interpret the corresponding gravitational wave (GW) and electromagnetic emission. Here, we review the current theoretical investigation on BNS mergers based on general relativistic magnetohydrodynamics simulations, paying special attention to the magnetic field as a crucial ingredient. First, we discuss the evolution, amplification, and emerging structure of magnetic fields in BNS mergers. Then, we consider their impact on various critical aspects: (i) jet formation and the connection with SGRBs, (ii) matter ejection, r-process nucleosynthesis, and radioactively-powered kilonova transients, and (iii) post-merger GW emission.

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Notes

  1. We note that while the BNS hypothesis remains favoured, the possibility of a NS-black hole system cannot be completely ruled out (e.g., [5, 60]).

  2. For a more general discussion on BNS mergers and the progress of numerical relativity simulations, we refer the reader to a number of other reviews on the subject, e.g. [11, 37, 41, 100, 108].

  3. Isolated NSs with much stronger magnetic fields exist, up to the typical \(10^{14}{-}10^{15}\,\hbox {G}\) of magnetars. However, there is no evidence for such high magnetizations in BNSs.

  4. Such an outflow is naturally explained in terms of a “structured jet” composed by a highly collimated and energetic core surrounded by a less energetic wide-angle cocoon, where the latter is formed via the early interaction of the incipient jet with the baryon-polluted environment around the merger site (e.g., [79]).

  5. Although we restrict the present discussion to BNS mergers, an accreting BH with the right properties to power a SGRB could also result from a NS–BH merger (see, e.g., [107] and refs. therein).

  6. The interaction between the outflow and the dense surrounding environment contributes to the differences in terms of collimation with respect to the findings of, e.g., [129] (where the evolution also lasts over 200 ms).

  7. After the present review was submitted, Ref. [98] further confirmed that superimposing by hand an extended dipolar magnetic field on a differentially rotating NS produces a collimated outflow, as found, e.g., in [75, 129, 139, 146]. In this case, the initial data were directly taken from the outcome of a nonmagnetized BNS merger simulation at 17 ms after merger and neutrino radiation was included. While this represents an important step forward with respect to studies like [75, 129, 139, 146], a main caveat remains: there is no guarantee that collimated outflows with properties similar to those reported in [98], which were obtained by imposing an ad hoc dipolar field at an arbitrary time, could also be obtained for magnetized BNSs going through the full merger process.

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Acknowledgements

We thank Daniele Viganò, David Radice, Bruno Giacomazzo, Wolfgang Kastaun, Davide Lazzati, and Albino Perego for useful discussions.

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  1. INAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122, Padua, Italy

    Riccardo Ciolfi

  2. INFN–Sezione di Padova, Via Francesco Marzolo 8, 35131, Padua, Italy

    Riccardo Ciolfi

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Correspondence to Riccardo Ciolfi.

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Ciolfi, R. The key role of magnetic fields in binary neutron star mergers. Gen Relativ Gravit 52, 59 (2020). https://doi.org/10.1007/s10714-020-02714-x

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