Abstract
Classical novae are the most common astrophysical thermonuclear explosions, occurring on the surfaces of white dwarf stars accreting gas from companions in binary star systems1. Novae typically expel about 10-4 solarmasses ofmaterial at velocities exceeding 1,000 kilometres per second.However, the mechanismofmass ejection innovae is poorly understood, and could be dominated by the impulsive flash of thermonuclear energy2, prolonged optically thick winds3 or binary interaction with the nova envelope4. Classical novae are now routinely detected at gigaelectronvolt γ-ray wavelengths5, suggesting that relativistic particles are accelerated by strong shocks in the ejecta. Here we report high-resolution radio imaging of the γ-rayemitting nova V959 Mon. Wefind that its ejecta were shaped by the motion of the binary system: somegas 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 motion6,7. At the interface between the equatorial and polar regions, we observe synchrotronemission indicative of shocks and relativistic particle acceleration, thereby pinpointingthe locationof γ-ray production. Binary shaping of the nova ejecta and associated internal shocks are expected to be widespread among novae8, explaining why many novae are γ-ray emitters5.
| Original language | English |
|---|---|
| Pages (from-to) | 339-342 |
| Number of pages | 4 |
| Journal | Nature |
| Volume | 514 |
| Issue number | 7522 |
| DOIs | |
| Publication status | Published - Oct 8 2014 |
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Binary orbits as the driver of γ-ray emission and mass ejection in classical novae. / Chomiuk, Laura; Linford, Justin D.; Yang, Jun; O'Brien, T. J.; Paragi, Zsolt; Mioduszewski, Amy J.; Beswick, R. J.; Cheung, C. C.; Mukai, Koji; Nelson, Thomas; Ribeiro, Valério A.R.M.; Rupen, Michael P.; Sokoloski, J. L.; Weston, Jennifer; Zheng, Yong; Bode, Michael F.; Eyres, Stewart; Roy, Nirupam; Taylor, Gregory B.
In: Nature, Vol. 514, No. 7522, 08.10.2014, p. 339-342.Research output: Contribution to journal › Article
TY - JOUR
T1 - Binary orbits as the driver of γ-ray emission and mass ejection in classical novae
AU - Chomiuk, Laura
AU - Linford, Justin D.
AU - Yang, Jun
AU - O'Brien, T. J.
AU - Paragi, Zsolt
AU - Mioduszewski, Amy J.
AU - Beswick, R. J.
AU - Cheung, C. C.
AU - Mukai, Koji
AU - Nelson, Thomas
AU - Ribeiro, Valério A.R.M.
AU - Rupen, Michael P.
AU - Sokoloski, J. L.
AU - Weston, Jennifer
AU - Zheng, Yong
AU - Bode, Michael F.
AU - Eyres, Stewart
AU - Roy, Nirupam
AU - Taylor, Gregory B.
PY - 2014/10/8
Y1 - 2014/10/8
N2 - Classical novae are the most common astrophysical thermonuclear explosions, occurring on the surfaces of white dwarf stars accreting gas from companions in binary star systems1. Novae typically expel about 10-4 solarmasses ofmaterial at velocities exceeding 1,000 kilometres per second.However, the mechanismofmass ejection innovae is poorly understood, and could be dominated by the impulsive flash of thermonuclear energy2, prolonged optically thick winds3 or binary interaction with the nova envelope4. Classical novae are now routinely detected at gigaelectronvolt γ-ray wavelengths5, suggesting that relativistic particles are accelerated by strong shocks in the ejecta. Here we report high-resolution radio imaging of the γ-rayemitting nova V959 Mon. Wefind that its ejecta were shaped by the motion of the binary system: somegas 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 motion6,7. At the interface between the equatorial and polar regions, we observe synchrotronemission indicative of shocks and relativistic particle acceleration, thereby pinpointingthe locationof γ-ray production. Binary shaping of the nova ejecta and associated internal shocks are expected to be widespread among novae8, explaining why many novae are γ-ray emitters5.
AB - Classical novae are the most common astrophysical thermonuclear explosions, occurring on the surfaces of white dwarf stars accreting gas from companions in binary star systems1. Novae typically expel about 10-4 solarmasses ofmaterial at velocities exceeding 1,000 kilometres per second.However, the mechanismofmass ejection innovae is poorly understood, and could be dominated by the impulsive flash of thermonuclear energy2, prolonged optically thick winds3 or binary interaction with the nova envelope4. Classical novae are now routinely detected at gigaelectronvolt γ-ray wavelengths5, suggesting that relativistic particles are accelerated by strong shocks in the ejecta. Here we report high-resolution radio imaging of the γ-rayemitting nova V959 Mon. Wefind that its ejecta were shaped by the motion of the binary system: somegas 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 motion6,7. At the interface between the equatorial and polar regions, we observe synchrotronemission indicative of shocks and relativistic particle acceleration, thereby pinpointingthe locationof γ-ray production. Binary shaping of the nova ejecta and associated internal shocks are expected to be widespread among novae8, explaining why many novae are γ-ray emitters5.
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U2 - 10.1038/nature13773
DO - 10.1038/nature13773
M3 - Article
AN - SCOPUS:84908216559
VL - 514
SP - 339
EP - 342
JO - Nature
JF - Nature
SN - 0028-0836
IS - 7522
ER -