#Solar wind ram pressure full#

(2017), Morphology of the UV aurorae Jupiter during Juno's first perijove observations, Geophys. (2000), Auroral emissions of the giant planets, Rev. (2014), Magnetospheric science objectives of the Juno mission, Space Sci.

(2015), Auroral processes at the giant planets: Energy deposition, emission mechanisms, morphology and spectra, Space Sci. G., Krupp N., Lamy L., Melin H., and Tao C. , Branduardi‐Raymont G., Galand M., Hess S. (2001), Spectroscopic evidence for high‐altitude aurora at Jupiter from Galileo extreme ultraviolet spectrometer and Hopkins ultraviolet telescope observations, Icarus, 152, 151.īadman, S. The color ratios are only shown for pixels where the brightness both exceeds 80 kR and is larger than 25% of the peak brightness.Ījello, J. The L = 6 and L = 30 auroral ovals are indicated. (b) (left) Juno‐UVS brightness map and (right) corresponding color ratio map of Jupiter, for 30 h of elapsed time (~38 s integrated time) starting at 12:00:00 spacecraft UT on 21 June 2016. See supporting information for an animation of the entire observation period. The color ratios are only shown for pixels where the brightness both exceeds 80 kR and is larger than 25% of the peak brightness.

#Solar wind ram pressure full#

Brightness (and color ratio) pixels have an angular size of 0.04° × 0.04°, which considerably oversamples the instrument spatial point‐spread function of along slit full width at half maximum FWHM ~ 0.20°, cross slit FWHM ~ 0.25°. The larger and smaller white ovals at the north and south poles in the brightness image indicate the regions included in estimating the northern and southern emitted auroral power, respectively. The Juno range and subspacecraft system III longitude and latitude are indicated, along with nominal L = 6 and L = 30 auroral ovals. (a) (left) Juno‐UVS brightness image and (right) corresponding color ratio image of Jupiter, for 1 h of elapsed time (~1.3 s integrated time) starting at 12:34:28 spacecraft UT on 21 June 2016. The brightening events which are not associated with the solar wind generally have a risetime of ~2 h and a decay time of ~5 h.

Only one of these brightening events correlates well with large transient increases in solar wind ram pressure. Four large auroral brightening events are evident in the synoptic data, in which the total emitted auroral power increases by a factor of 3-4 for a few hours. Here we compare synoptic Juno-UVS observations of Jupiter's auroral emissions, acquired during 3-29 June 2016, with in situ solar wind observations, and related Jupiter observations from Earth. Some of Jupiter's auroral emissions are expected to be controlled or modified by local solar wind conditions. Prior to the bow shock crossing on 24 June 2016, the Juno approach provided a rare opportunity to correlate local solar wind conditions with Jovian auroral emissions. Juno ultraviolet spectrograph (UVS) observations of Jupiter's aurora obtained during approach are presented.