Pulsar revival in neutron star mergers: multimessenger prospects for the discovery of pre-merger coherent radio emission

Author:

Cooper A J12ORCID,Gupta O34ORCID,Wadiasingh Z567,Wijers R A M J1ORCID,Boersma O M12,Andreoni I568,Rowlinson A12ORCID,Gourdji K910ORCID

Affiliation:

1. API, Anton Pannekoek Institute for Astronomy, University of Amsterdam , Science Park 904, NL-1098 XH Amsterdam, the Netherlands

2. ASTRON, Netherlands Institute for Radio Astronomy , Oude Hoogeveensedijk 4, NL-7991 PD, Dwingeloo, the Netherlands

3. Department of Physical Sciences, Indian Institute of Science Education and Research (IISER) Kolkata , Mohanpur 741246, West Bengal, India

4. Department of Astronomy, University of Texas at Austin , Austin, TX 78712, USA

5. Department of Astronomy, University of Maryland , College Park, ML 20742, USA

6. Astrophysics Science Division, NASA Goddard Space Flight Center , Mail Code 661, Greenbelt, ML 20771, USA

7. Center for Research and Exploration in Space Science and Technology , NASA/GSFC, Greenbelt, ML 20771, USA

8. Joint Space-Science Institute, University of Maryland , College Park, ML 20742, USA

9. Centre for Astrophysics and Supercomputing, Swinburne University of Technology , Hawthorn VIC 3122, Australia

10. OzGrav: ARC Centre of Excellence for Gravitational Wave Discovery , Hawthorn VIC 3122, Australia

Abstract

ABSTRACT We investigate pre-merger coherent radio emission from neutron star mergers arising due to the magnetospheric interaction between compact objects. We consider two plausible radiation mechanisms, and show that if one neutron star has a surface magnetic field Bs ≥ 1012G, coherent millisecond radio bursts with characteristic temporal morphology and inclination angle dependence are observable to Gpc distances with next-generation radio facilities. We explore multi-messenger and multi-wavelength methods of identification of a neutron star merger origin of radio bursts, such as in fast radio burst surveys, triggered observations of gamma-ray bursts and gravitational wave events, and optical/radio follow-up of fast radio bursts in search of kilonova and radio afterglow emission. We present our findings for current and future observing facilities, and make recommendations for verifying or constraining the model.

Funder

NOVA

API

NWO

LKBF

NASA

Australian Research Council

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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