A generic description of planetary aurora J. De Keyser, R. Maggiolo, and L. Maes Belgian Institute for Space Aeronomy, Brussels, Belgium

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A generic description of planetary aurora J. De Keyser, R. Maggiolo, and L. Maes Belgian Institute for Space Aeronomy, Brussels, Belgium

Context We consider a rotating planetary body that orbits a star. The star is assumed to have a stellar wind. The motion of the body relative to the stellar wind is supersonic, i.e. the wind speed is supersonic or the planet orbits the star very closely at a high orbital speed. This situation reflects planets in the Solar System, but it may be applicable to many exoplanets as well November 2013ESWW10, Antwerp1

Classification of magnetospheres November 2013ESWW10, Antwerp2

Classical magnetospheres In “classical magnetospheres” The planetary object has an intrinsic magnetic field It is rotating. It has a conducting ionosphere. Plasma escapes from the ionosphere. There may be additional inner sources of plasma. Such magnetospheres have a plasmasphere, a magnetopause & boundary layer, a magnetotail with a current sheet November 2013ESWW10, Antwerp3

Plasma circulation Plasma of solar wind origin : Limited entry of solar wind is possible through various mechanisms (reconnection, diffusion, plasma transfer). Plasma of terrestrial origin : Escape from the ionosphere is due to energy input from solar radiation or precipitating particles. These produce a plasmasphere reservoir on closed field lines, which loses mass via a plasmaspheric wind and plumes November 2013ESWW10, Antwerp4

Magnetospheric electric field November 2013ESWW10, Antwerp5

Magnetosphere – ionosphere coupling November 2013ESWW10, Antwerp6 ionospheric potential magnetospheric potential parallel potential difference

Current continuity November 2013ESWW10, Antwerp7

Structure at the midnight meridian November 2013ESWW10, Antwerp8

18-22 November 2013ESWW10, Antwerp9

18-22 November 2013ESWW10, Antwerp10

18-22 November 2013ESWW10, Antwerp11

18-22 November 2013ESWW10, Antwerp12

18-22 November 2013ESWW10, Antwerp13

Earth : corotation border November 2013ESWW10, Antwerp14

Observations indeed show : ionosphereic electron depletion very strong ionospheric flows (> 1 km/s) ion-neutral collisions may produce stable auroral red arcs (630 nm) local heating of the ionosphere and upward flow November 2013ESWW10, Antwerp15

Earth : aurora Higher latitude : More or less permanent oval with transient appearance of discrete auroral arcs and black aurora November 2013ESWW10, Antwerp16

18-22 November 2013ESWW10, Antwerp17

Inner plasma sources November 2013ESWW10, Antwerp18

Jovian aurora Corotation boundary : permanent aurora Higher latitude : varying, depending on magnetospheric activity Footpoints of the moons November 2013ESWW10, Antwerp19 Io Ganymede Europa corotation oval variable auroral structures

Io For Jupiter, especially the volcanic moon Io is a source of gas November 2013ESWW10, Antwerp20

Conjugate aurora Not only the footpoints, also much or the other aurora are magnetically conjugate November 2013ESWW10, Antwerp21

Saturn : same story Also Saturn has a permanent corotation boundary oval, more transient higher latitude auroras, and moon footpoint auroral spots November 2013ESWW10, Antwerp22

Enceladus For Saturn, the icy moon Enceladus is a source of gas release from fissures in its crust, fueled by tidal deformation November 2013ESWW10, Antwerp23

18-22 November 2013ESWW10, Antwerp24

18-22 November 2013ESWW10, Antwerp25

Conclusions Moon as inner source Corotation boundary Higher latitude conjugate footpoint spots permanent eastward drift and aurora with transient intensification transient aurora conjugate footpoint spots permanent westward drift with transient intensification (SAPS/SAID) permanent aurora + transient arcs conjugate spots only when moon is on closed field lines variable The major structure of auroral patterns of magnetized planets can be understood in terms of a simple model of the auroral current circuit. Details of the actual aurora depend on the size of the dipole field, its strength relative to the stellar wind pressure, and of course on the composition of the planet’s atmosphere November 2013ESWW10, Antwerp26

18-22 November 2013ESWW10, Antwerp27 References J. De Keyser, M. Roth, and J. Lemaire. The magnetospheric driver of subauroral ion drifts. Geophys. Res. Lett., 25: , J. De Keyser. Formation and evolution of subauroral ion drifts in the course of a substorm. J. Geophys. Res., 104(6):12,339-12,350, J. De Keyser. Storm-time energetic particle penetration into the inner magnetosphere as the electromotive force in the subauroral ion drift current circuit. In S. Ohtani, ed., Magnetospheric Current Systems, Geophysical Monograph Series 118, pages AGU, M. M. Echim, M. Roth, and J. De Keyser. Sheared magnetospheric plasma flows and discrete auroral arcs: a quasi-static coupling model. Ann. Geophys., 25, 317–330, M. M. Echim, R. Maggiolo, M. Roth, and J. De Keyser. A magnetospheric generator driving ion and electron acceleration and electric currents in a discrete auroral arc observed by Cluster and DMSP. Geophys. Res. Lett., 36:L12111, F. Darrouzet, D. L. Gallagher, N. André, D. L. Carpenter, I. Dandouras, P. M. E. Décréau, J. De Keyser, R. E. Denton, J. C. Foster, J. Goldstein, M. B. Moldwin, B. W. Reinisch, B. R. Sandel, and J. Tu. CLUSTER and IMAGE Observations of the Plasmasphere: Plasma Structure and Dynamics. Space Sci. Rev., 145(1-2):55–106, doi: /s J. De Keyser and M. Echim. Auroral and subauroral phenomena: An electrostatic picture. Ann. Geophys., 28:633–650, J. De Keyser, R. Maggiolo, and M. Echim. Monopolar and bipolar auroral electric fields and their effects. Ann. Geophys., 28(11):2027–2046, J. De Keyser, R. Maggiolo, M. Echim, and I. Dandouras. Wave signatures and electrostatic phenomena above aurora: Cluster observations and modeling. J. Geophys. Res., 116:A06224, 2011.