دورية أكاديمية
Asymmetric mass ratios for bright double neutron-star mergers.
العنوان: | Asymmetric mass ratios for bright double neutron-star mergers. |
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المؤلفون: | Ferdman RD; Faculty of Science, University of East Anglia, Norwich, UK. r.ferdman@uea.ac.uk., Freire PCC; Max-Planck-Institut für Radioastronomie, Bonn, Germany., Perera BBP; Arecibo Observatory, Arecibo, Puerto Rico., Pol N; Department of Physics and Astronomy, West Virginia University, Morgantown, WV, USA.; Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV, USA., Camilo F; South African Radio Astronomy Observatory, Cape Town, South Africa., Chatterjee S; Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY, USA.; Department of Astronomy, Cornell University, Ithaca, NY, USA., Cordes JM; Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY, USA.; Department of Astronomy, Cornell University, Ithaca, NY, USA., Crawford F; Department of Physics and Astronomy, Franklin and Marshall College, Lancaster, PA, USA., Hessels JWT; Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, The Netherlands.; ASTRON, Netherlands Institute for Radio Astronomy, Dwingeloo, The Netherlands., Kaspi VM; Department of Physics, McGill University, Montreal, Quebec, Canada.; McGill Space Institute, McGill University, Montreal, Quebec, Canada., McLaughlin MA; Department of Physics and Astronomy, West Virginia University, Morgantown, WV, USA.; Center for Gravitational Waves and Cosmology, West Virginia University, Morgantown, WV, USA., Parent E; Department of Physics, McGill University, Montreal, Quebec, Canada.; McGill Space Institute, McGill University, Montreal, Quebec, Canada., Stairs IH; Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia, Canada., van Leeuwen J; ASTRON, Netherlands Institute for Radio Astronomy, Dwingeloo, The Netherlands. |
المصدر: | Nature [Nature] 2020 Jul; Vol. 583 (7815), pp. 211-214. Date of Electronic Publication: 2020 Jul 08. |
نوع المنشور: | Journal Article; Research Support, Non-U.S. Gov't; Research Support, U.S. Gov't, Non-P.H.S. |
اللغة: | English |
بيانات الدورية: | Publisher: Nature Publishing Group Country of Publication: England NLM ID: 0410462 Publication Model: Print-Electronic Cited Medium: Internet ISSN: 1476-4687 (Electronic) Linking ISSN: 00280836 NLM ISO Abbreviation: Nature Subsets: PubMed not MEDLINE; MEDLINE |
أسماء مطبوعة: | Publication: Basingstoke : Nature Publishing Group Original Publication: London, Macmillan Journals ltd. |
مستخلص: | The discovery of a radioactively powered kilonova associated with the binary neutron-star merger GW170817 remains the only confirmed electromagnetic counterpart to a gravitational-wave event 1,2 . Observations of the late-time electromagnetic emission, however, do not agree with the expectations from standard neutron-star merger models. Although the large measured ejecta mass 3,4 could be explained by a progenitor system that is asymmetric in terms of the stellar component masses (that is, with a mass ratio q of 0.7 to 0.8) 5 , the known Galactic population of merging double neutron-star systems (that is, those that will coalesce within billions of years or less) has until now consisted only of nearly equal-mass (q > 0.9) binaries 6 . The pulsar PSR J1913+1102 is a double system in a five-hour, low-eccentricity (0.09) orbit, with an orbital separation of 1.8 solar radii 7 , and the two neutron stars are predicted to coalesce in [Formula: see text] million years owing to gravitational-wave emission. Here we report that the masses of the pulsar and the companion neutron star, as measured by a dedicated pulsar timing campaign, are 1.62 ± 0.03 and 1.27 ± 0.03 solar masses, respectively. With a measured mass ratio of q = 0.78 ± 0.03, this is the most asymmetric merging system reported so far. On the basis of this detection, our population synthesis analysis implies that such asymmetric binaries represent between 2 and 30 per cent (90 per cent confidence) of the total population of merging binaries. The coalescence of a member of this population offers a possible explanation for the anomalous properties of GW170817, including the observed kilonova emission from that event. |
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تواريخ الأحداث: | Date Created: 20200710 Date Completed: 20200716 Latest Revision: 20210326 |
رمز التحديث: | 20221213 |
DOI: | 10.1038/s41586-020-2439-x |
PMID: | 32641814 |
قاعدة البيانات: | MEDLINE |
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