Universität zu Köln

Allegrini, F., Mauk, B., Clark, G., Gladstone, G. R., Hue, V, Kurth, W. S., Bagenal, F., Bolton, S., Bonfond, B., Connerney, J. E. P., Ebert, R. W., Greathouse, T., Imai, M., Levin, S., Louarn, P., McComas, D. J., Saur, J., Szalay, J. R., Valek, P. W. and Wilson, R. J. (2020). Energy Flux and Characteristic Energy of Electrons Over Jupiter's Main Auroral Emission. J. Geophys. Res-Space Phys., 125 (4). WASHINGTON: AMER GEOPHYSICAL UNION. ISSN 2169-9402

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Abstract

Jupiter's ultraviolet (UV) aurorae, the most powerful and intense in the solar system, are caused by energetic electrons precipitating from the magnetosphere into the atmosphere where they excite the molecular hydrogen. Previous studies focused on case analyses and/or greater than 30-keV energy electrons. Here for the first time we provide a comprehensive evaluation of Jovian auroral electron characteristics over the entire relevant range of energies (similar to 100 eV to similar to 1 MeV). The focus is on the first eight perijoves providing a coarse but complete System III view of the northern and southern auroral regions with corresponding UV observations. The latest magnetic field model JRM09 with a current sheet model is used to map Juno's magnetic foot point onto the UV images and relate the electron measurements to the UV features. We find a recurring pattern where the 3- to 30-keV electron energy flux peaks in a region just equatorward of the main emission. The region corresponds to a minimum of the electron characteristic energy (<10 keV). Its polarward edge corresponds to the equatorward edge of the main oval, which is mapped at M shells of similar to 51. A refined current sheet model will likely bring this boundary closer to the expected 20-30 RJ. Outside that region, the >100-keV electrons contribute to most (>similar to 70-80%) of the total downward energy flux and the characteristic energy is usually around 100 keV or higher. We examine the UV brightness per incident energy flux as a function of characteristic energy and compare it to expectations from a model.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Allegrini, F. UNSPECIFIED UNSPECIFIED UNSPECIFIED Mauk, B. UNSPECIFIED UNSPECIFIED UNSPECIFIED Clark, G. UNSPECIFIED UNSPECIFIED UNSPECIFIED Gladstone, G. R. UNSPECIFIED UNSPECIFIED UNSPECIFIED Hue, V UNSPECIFIED UNSPECIFIED UNSPECIFIED Kurth, W. S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Bagenal, F. UNSPECIFIED UNSPECIFIED UNSPECIFIED Bolton, S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Bonfond, B. UNSPECIFIED UNSPECIFIED UNSPECIFIED Connerney, J. E. P. UNSPECIFIED UNSPECIFIED UNSPECIFIED Ebert, R. W. UNSPECIFIED UNSPECIFIED UNSPECIFIED Greathouse, T. UNSPECIFIED UNSPECIFIED UNSPECIFIED Imai, M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Levin, S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Louarn, P. UNSPECIFIED UNSPECIFIED UNSPECIFIED McComas, D. J. UNSPECIFIED UNSPECIFIED UNSPECIFIED Saur, J. UNSPECIFIED UNSPECIFIED UNSPECIFIED Szalay, J. R. UNSPECIFIED UNSPECIFIED UNSPECIFIED Valek, P. W. UNSPECIFIED UNSPECIFIED UNSPECIFIED Wilson, R. J. UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-338198
DOI:	10.1029/2019JA027693
Journal or Publication Title:	J. Geophys. Res-Space Phys.
Volume:	125
Number:	4
Date:	2020
Publisher:	AMER GEOPHYSICAL UNION
Place of Publication:	WASHINGTON
ISSN:	2169-9402
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language HUBBLE-SPACE-TELESCOPE; DETECTION EFFICIENCY; MAGNETIC-FIELD; JOVIAN AURORA; ACCELERATION; MAGNETOSPHERE; IONOSPHERE; PRECIPITATION; SPECTROSCOPY; COROTATION Multiple languages Astronomy & Astrophysics Multiple languages
URI:	http://kups.ub.uni-koeln.de/id/eprint/33819