.2018 Feb 8;554(7691):207-210.

doi: 10.1038/nature25452. Epub 2017 Nov 20.

A mildly relativistic wide-angle outflow in the neutron-star merger event GW170817

K P Mooley^{1 2 3}, E Nakar⁴, K Hotokezaka⁵, G Hallinan³, A Corsi⁶, D A Frail², A Horesh⁷, T Murphy^{8 9}, E Lenc^{8 9}, D L Kaplan¹⁰, K De³, D Dobie^{8 9 11}, P Chandra^{12 13}, A Deller^{14 15}, O Gottlieb⁴, M M Kasliwal³, S R Kulkarni³, S T Myers², S Nissanke¹⁶, T Piran⁷, C Lynch^{8 9}, V Bhalerao¹⁷, S Bourke¹⁸, K W Bannister¹¹, L P Singer¹⁹

Affiliations

¹ Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK.
² National Radio Astronomy Observatory, Socorro, New Mexico 87801, USA.
³ California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, California 91125, USA.
⁴ The Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel.
⁵ Department Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, New Jersey 08544, USA.
⁶ Department of Physics and Astronomy, Texas Tech University, Box 41051, Lubbock, Texas 79409-1051, USA.
⁷ Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel.
⁸ Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, New South Wales 2006, Australia.
⁹ ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Australia.
¹⁰ Department of Physics, University of Wisconsin - Milwaukee, Milwaukee, Wisconsin 53201, USA.
¹¹ ATNF, CSIRO Astronomy and Space Science, PO Box 76, Epping, New South Wales 1710, Australia.
¹² National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune University Campus, Ganeshkhind Pune 411007, India.
¹³ Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden.
¹⁴ Centre for Astrophysics and Supercomputing, Swinburne University of Technology, John Street, Hawthorn, Victoria 3122, Australia.
¹⁵ ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav), Australia.
¹⁶ Institute of Mathematics, Astrophysics and Particle Physics, Radboud University, Heyendaalseweg 135, 6525 AJ Nijmegen, The Netherlands.
¹⁷ Department of Physics, Indian Institute of Technology Bombay, Mumbai 400076, India.
¹⁸ Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, S-439 92 Onsala, Sweden.
¹⁹ Astroparticle Physics Laboratory, NASA Goddard Space Flight Center, Mail Code 661, Greenbelt, Maryland 20771, USA.

PMID:29261643
DOI: 10.1038/nature25452

A mildly relativistic wide-angle outflow in the neutron-star merger event GW170817

K P Mooley et al. Nature.2018.

.2018 Feb 8;554(7691):207-210.

doi: 10.1038/nature25452. Epub 2017 Nov 20.

Authors

Affiliations

¹ Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK.
² National Radio Astronomy Observatory, Socorro, New Mexico 87801, USA.
³ California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, California 91125, USA.
⁴ The Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel.
⁵ Department Astrophysical Sciences, Princeton University, Peyton Hall, Princeton, New Jersey 08544, USA.
⁶ Department of Physics and Astronomy, Texas Tech University, Box 41051, Lubbock, Texas 79409-1051, USA.
⁷ Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel.
⁸ Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, New South Wales 2006, Australia.
⁹ ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Australia.
¹⁰ Department of Physics, University of Wisconsin - Milwaukee, Milwaukee, Wisconsin 53201, USA.
¹¹ ATNF, CSIRO Astronomy and Space Science, PO Box 76, Epping, New South Wales 1710, Australia.
¹² National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune University Campus, Ganeshkhind Pune 411007, India.
¹³ Department of Astronomy, Stockholm University, AlbaNova, SE-106 91 Stockholm, Sweden.
¹⁴ Centre for Astrophysics and Supercomputing, Swinburne University of Technology, John Street, Hawthorn, Victoria 3122, Australia.
¹⁵ ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav), Australia.
¹⁶ Institute of Mathematics, Astrophysics and Particle Physics, Radboud University, Heyendaalseweg 135, 6525 AJ Nijmegen, The Netherlands.
¹⁷ Department of Physics, Indian Institute of Technology Bombay, Mumbai 400076, India.
¹⁸ Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, S-439 92 Onsala, Sweden.
¹⁹ Astroparticle Physics Laboratory, NASA Goddard Space Flight Center, Mail Code 661, Greenbelt, Maryland 20771, USA.

PMID:29261643
DOI: 10.1038/nature25452

Abstract

GW170817 was the first gravitational-wave detection of a binary neutron-star merger. It was accompanied by radiation across the electromagnetic spectrum and localized to the galaxy NGC 4993 at a distance of 40 megaparsecs. It has been proposed that the observed γ-ray, X-ray and radio emission is due to an ultra-relativistic jet being launched during the merger (and successfully breaking out of the surrounding material), directed away from our line of sight (off-axis). The presence of such a jet is predicted from models that posit neutron-star mergers as the drivers of short hard-γ-ray bursts. Here we report that the radio light curve of GW170817 has no direct signature of the afterglow of an off-axis jet. Although we cannot completely rule out the existence of a jet directed away from the line of sight, the observed γ-ray emission could not have originated from such a jet. Instead, the radio data require the existence of a mildly relativistic wide-angle outflow moving towards us. This outflow could be the high-velocity tail of the neutron-rich material that was ejected dynamically during the merger, or a cocoon of material that breaks out when a jet launched during the merger transfers its energy to the dynamical ejecta. Because the cocoon model explains the radio light curve of GW170817, as well as the γ-ray and X-ray emission (and possibly also the ultraviolet and optical emission), it is the model that is most consistent with the observational data. Cocoons may be a ubiquitous phenomenon produced in neutron-star mergers, giving rise to a hitherto unidentified population of radio, ultraviolet, X-ray and γ-ray transients in the local Universe.

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A chirp, a roar and a whisper.
Wijers R.Wijers R.Nature. 2018 Feb 8;554(7691):178-179. doi: 10.1038/d41586-018-01570-9.Nature. 2018.PMID:29420500No abstract available.

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A mildly relativistic wide-angle outflow in the neutron-star merger event GW170817

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A mildly relativistic wide-angle outflow in the neutron-star merger event GW170817

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