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Tytuł pozycji:

Binary orbits as the driver of γ-ray emission and mass ejection in classical novae.

Tytuł:
Binary orbits as the driver of γ-ray emission and mass ejection in classical novae.
Autorzy:
Chomiuk L; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
Linford JD; Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA.
Yang J; 1] Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, SE-439 92 Onsala, Sweden [2] Joint Institute for VLBI in Europe, Postbus 2, NL-7990 AA Dwingeloo, The Netherlands [3] Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, 200030 Shanghai, China.
O'Brien TJ; Jodrell Bank Centre for Astrophysics, Alan Turing Building, University of Manchester, Manchester M13 9PL, UK.
Paragi Z; Joint Institute for VLBI in Europe, Postbus 2, NL-7990 AA Dwingeloo, The Netherlands.
Mioduszewski AJ; National Radio Astronomy Observatory, PO Box O, Socorro, New Mexico 87801, USA.
Beswick RJ; Jodrell Bank Centre for Astrophysics, Alan Turing Building, University of Manchester, Manchester M13 9PL, UK.
Cheung CC; Space Science Division, Naval Research Laboratory, Washington, DC 20375-5352, USA.
Mukai K; 1] Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA [2] CRESST and X-ray Astrophysics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA.
Nelson T; School of Physics and Astronomy, University of Minnesota, 115 Church Street Southeast, Minneapolis, Minnesota 55455, USA.
Ribeiro VA; Astrophysics, Cosmology and Gravity Centre, Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch 7701, South Africa.
Rupen MP; 1] National Radio Astronomy Observatory, PO Box O, Socorro, New Mexico 87801, USA [2] National Research Council, Herzberg Astronomy and Astrophysics, 717 White Lake Road, PO Box 248, Penticton, British Columbia V2A 6J9, Canada.
Sokoloski JL; Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA.
Weston J; Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA.
Zheng Y; Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA.
Bode MF; Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK.
Eyres S; Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy, University of Central Lancashire, Preston PR1 2HE, UK.
Roy N; Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany.
Taylor GB; Department of Physics and Astronomy, University of New Mexico, MSC07 4220, Albuquerque, New Mexico 87131-0001, USA.
Źródło:
Nature [Nature] 2014 Oct 16; Vol. 514 (7522), pp. 339-42. Date of Electronic Publication: 2014 Oct 08.
Typ publikacji:
Journal Article; Research Support, Non-U.S. Gov't; Research Support, U.S. Gov't, Non-P.H.S.
Język:
English
Imprint Name(s):
Publication: Basingstoke : Nature Publishing Group
Original Publication: London, Macmillan Journals ltd.
References:
Nature. 2006 Jul 20;442(7100):279-81. (PMID: 16855585)
Science. 2010 Aug 13;329(5993):817-21. (PMID: 20705855)
Science. 2014 Aug 1;345(6196):554-8. (PMID: 25082700)
Entry Date(s):
Date Created: 20141009 Date Completed: 20141112 Latest Revision: 20211021
Update Code:
20240104
DOI:
10.1038/nature13773
PMID:
25296250
Czasopismo naukowe
Classical novae are the most common astrophysical thermonuclear explosions, occurring on the surfaces of white dwarf stars accreting gas from companions in binary star systems. Novae typically expel about 10(-4) solar masses of material at velocities exceeding 1,000 kilometres per second. However, the mechanism of mass ejection in novae is poorly understood, and could be dominated by the impulsive flash of thermonuclear energy, prolonged optically thick winds or binary interaction with the nova envelope. Classical novae are now routinely detected at gigaelectronvolt γ-ray wavelengths, suggesting that relativistic particles are accelerated by strong shocks in the ejecta. Here we report high-resolution radio imaging of the γ-ray-emitting nova V959 Mon. We find that its ejecta were shaped by the motion of the binary system: some gas was expelled rapidly along the poles as a wind from the white dwarf, while denser material drifted out along the equatorial plane, propelled by orbital motion. At the interface between the equatorial and polar regions, we observe synchrotron emission indicative of shocks and relativistic particle acceleration, thereby pinpointing the location of γ-ray production. Binary shaping of the nova ejecta and associated internal shocks are expected to be widespread among novae, explaining why many novae are γ-ray emitters.

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