An auroral flare at Jupiter

Article

关键词: SOLAR-WIND CONTROL;    IO FLUX TUBE;    FOOTPRINT;    FIELD;    EMISSIONS;    PRESSURE;    MODELS;   

DOI  :  10.1038/35071018

来源: SCIE

【 摘 要 】

Jupiter's aurora is the most powerful in the Solar System(1). It is powered largely by energy extracted from planetary rotation(2), although there seems also to be a contribution from the solar wind(3,4). This contrasts with Earth's aurora, which is generated through the interaction of the solar wind with the magnetosphere. The major features of Jupiter's aurora (based on far-ultraviolet(5-7), near-infrared(8,9) and visible-wavelength(10) observations) include a main oval that generally corotates with the planet and a region of patchy, diffuse emission inside the oval on Jupiter's dusk side. Here we report the discovery of a rapidly evolving, very bright and localized emission poleward of the northern main oval, in a region connected magnetically to Jupiter's outer magnetosphere. The intensity of the emission increased by a factor of 30 within 70s, and then decreased on a similar timescale, all captured during a single four-minute exposure. This type of flaring emission has not previously been reported for Jupiter (similar, but smaller, transient events have been observed at Earth), and it may be related directly to changes in the solar wind.

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