期刊
NATURE
卷 554, 期 7691, 页码 207-+出版社
NATURE PORTFOLIO
DOI: 10.1038/nature25452
关键词
-
资金
- Australian Government
- Hintze Centre for Astrophysical Surveys
- Hintze Family Charitable Foundation
- ERC starting grant (GRB/SN)
- ISF [1277/13]
- NSF [AST-1654815, AST-1412421]
- National Science Foundation CAREER award [1455090]
- I-Core Program of the Planning and Budgeting Committee
- Israel Science Foundation
- Australian Research Council [FT150100099]
- Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]
- GROWTH (Global Relay of Observatories Watching Transients Happen) project - NSF under PIRE grant [1545949]
- Netherlands Organization for Scientific Research through NWO VIDI grant [639.042.612-Nissanke]
- NWO TOP grant [62002444-Nissanke]
- Department of Science and Technology via SwarnaJayanti Fellowship [DST/SJF/PSA-01/2014-15]
- Advanced ERC grant TReX
- Science and Engineering Research Board, Department of Science and Technology, India
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1412421, 1455090] Funding Source: National Science Foundation
GW170817 was the first gravitational-wave detection of a binary neutron-star merger(1). It was accompanied by radiation across the electromagnetic spectrum and localized(2) to the galaxy NGC 4993 at a distance of 40 megaparsecs. It has been proposed that the observed gamma-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)(3-6). The presence of such a jet is predicted from models that posit neutron-star mergers as the drivers of short hard-gamma-ray bursts(7,8). 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 gamma-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 gamma-ray and X-ray emission (and possibly also the ultraviolet and optical emission)(9-15), 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 gamma-ray transients in the local Universe.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据