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Solar Wind Vs. Internal Processes Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes N. Krupp and the Europlanet N2 Discipline working group on Magnetospheres, Exospheres, Ionospheres special thanks to Fran Bagenal and Emma Bunce EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Jupiter’s magnetosphere EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Jupiter Different types of aurora Polar Aurora e k a w Secondary Oval o Main Oval I Io footprint Hubble Space Telescope Clarke et al. EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Cowley et al. 2003 EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Equatorial View Dawn Dusk Polar View Dawn Dusk Side View EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Equatorial View Dawn Dusk Polar View Hill Region Sub- corotating Dawn Dusk plasmasheet Main Auroral Oval Side View EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Equatorial View Dawn Dusk Polar View Inward motion --> less load on Dawn Dusk ionosphere Outward motion --> more load on ionosphere Outer Magnetosphere “Cushion Region” Side View EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes ? ? ? Equatorial View Dawn Dusk Polar View Dawn Dusk How important is the Dungey Cycle? How Much of ?? ?? ?? Polar Flux is Open? Side View EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Large-scale current system in the Jovian magnetosphere After Hill (1979) and Vasyliunas (1983) • Discovery of a local time asymmetry in the system of azimuthal currents which distend the field lines away from the planet (Bunce and Cowley, 2001a; Khurana, 2001) • Investigations of field-aligned currents associated with magnetosphere-ionosphere coupling currents found to be ~1μAm-2 (Bunce and Cowley, 2001b; Khurana, 2001) EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Origin of the Jovian main aurora Calculated upward field-aligned current profile • Bunce and Cowley (2001b), Cowley and Bunce (2001), Hill (2001) and Southwood and Kivelson (2001) suggest the main auroral oval is due to the breakdown of corotation of the equatorial plasma • Modulation of the oval in anti-correlation with solar wind dynamic pressure (C&B, 2001, 2003a&b; S&K, 2001) EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Galileo observations ¾ Most prominent and well defined boundary Æ change in the electron pitch angle distributions located between 10 and 17 RJ. Ions Dawn Dusk 180° 90° Electrons 0° 40RJ 20RJ 10RJ 20RJ 40RJ Inner Region Outer Region Pancake distribution Field aligned with electrons Mag. Field maximum at 900 bi-directional electrons Tomás et al., 2004a 40RJ c.a. 40RJ EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Tracing the magnetic field lines ¾ Comparing the footprints of the PAD boundary (VIP4 model) with the HST observations North Pole South Pole 00 1800 2700 900 2700 900 1800 00 HST observations * Io ∆ PAD boundaries * Secondary Oval Footprints 6 and 25 RJ (VIP4) * Main Oval ¾ Good conjugation between the PAD boundary and the secondary oval EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes The Precipitation energy flux ¾Considering: ¾The precipitation energy flux given by : m. a. o. Emax ε=E ⋅ j(E,)γ ⋅ dE ∫ E Emin 1 Sec. Oval ¾ Measured electron’s spectra at the PAD 140 kR boundary. ¾ Strong pitch-angle scattering. 65 kR Mean Brightness (kR) Brightness Mean E2 ¾ Electron’s energy : E1 Є [55, 304] keV. Pole Equator E2 Є [55, 188] keV. Courtesy of D. Grodent, Univ. Liège ¾ Sufficient to directly produce the observed auroral emissions of the secondary oval without the need of a field aligned potential drop. EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Dynamics in Jupiter’s magnetosphere Energetic Particle Injections & correlation to auroral emissions 24 hour Galileo Energetic Particle Spectrogram HST Image of Jupiter’s UV aurora Mauk et al., 1997; 1999, 2000 Extreme “storm-time” dynamics Auroral manifestation of observed in the vicinity of near-Europa storm Europa’s orbit dynamics EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Dynamics of the Jovian magnetotail 16 days 2 V 1 3 days e py k ro 0 t 2 0 1 iso - 5 An -1 6 -2 radial azimuthal 10 Ion anisotropy flow anisotropy Ion 5 0 south-north -5 Magnetic field [nT] -10 96266 96 268 96270 96272 96274 96276 96278 96280 91.31 96.76 101.33 105.08 108.06 110.32 111.87 112.74 02:05 02:15 02:25 02:34 02:43 02:51 02:58 03:06 UT, JSE [R ], Loc. Time r Jup South-north magneticfield Location: 90-113 Rj Krupp et al, 2004 More X outward Transient periodical disturbances - l in bursts Jupiter e with repetition period of several days Sun More inward bursts (the most characteristic 2-3 days) are observed in the Jovian magnetotail! ? M ? ag ne top au se EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Jupiter Aurora and tail disruptive events (Grodent et al., 2004) In Situ* Auroral Spots Russell et al., Woch et al., Krupp et al. Distance 70-120 Rj >100 Rj Local Time postmidnight premidnight Size ~25 Rj 5-50 Rj Duration Mins-hours 5 min-1hour Recurrence 4 hours-3days 1-2 days EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Jupiter Tail disruption events - numbers 25 Rj 2 Rj ~8000 Rj x 0.01 ions/cc = 500 tons per plasmoid 1 per day = 0.006 ton/s 1 per hour = 0.15 ton/s EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Saturn’s aurora Saturn’s magnetosphere is also believed to be corotation-dominated, like Jupiter’s It also has an auroral oval as shown in the HST-STIS images below Is this also due to corotation-enforcement currents? Saturn aurora (HST–STIS) Taken from Cowley et al. (2003) EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Field-aligned current density in the northern ionosphere calculated from the divergence of the horizontal current - effect of the large-scale flow variation Taken from Cowley and Bunce, 2003 Voyager-2 Voyager-1 12 ⎛ W ⎞ ⎜ th ⎟ −2 The limiting current is j|| i0 = eN ≈ 70 nA m ⎝ 2π me ⎠ EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Saturn’s polar ionospheric flows and their relation to the main auroral oval Cowley, Bunce and Prangé, 2004 EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes DAWN DUSK model estimates are in good agreement with HST-STIS images of Saturn’s auroral oval Image taken from Cowley et al., 2004 EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Electron beams Dawn Sun • FUV auroral images from HST STIS instrument (Gérard et al., JGR 209, 207, 2004) [no observations of the aurora during the electron beam events] • ~80 deg latitude feature corresponds to just inside m’pause; others are from much deeper in the magnetosphere. • Periods of electron counterstreaming map into auroral zone. Beams map well in a statistical sense into the regions of Saturn’s aurora. EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Outer magnetosphere dynamics: aurora and radio emissions show rotational modulation + solar wind control EPSC2006-A-00395 EPSC, September 19, 2006, Berlin, Germany Norbert Krupp et al. Planetary aurorae and their electrodynamic drivers; solar wind vs. internal processes Europlanet N2 DWG 2 Science Case 1 1 - Objective or science goal: Solar wind interaction at Jupiter and Saturn including aurorae? 2 - Needed data sets: Millennium Campaign at Jupiter (Cassini, Galileo, Hubble Space telescope (UV), Chandra X-ray Observatory, X-ray Multi-Mirror, InfraRed Telescope Facility), other ground-based observations Saturn Hubble campaign 2004 and 2007 3 - Problem description Modelling of the Solar wind-magnetosphere-ionosphere coupling e.g.
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