Past and future observations of Jupiter with Cassini/RPWS

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Bethany Warren
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Past and future observations of Jupiter with Cassini/RPWS Flux density @ 1AU (Log W.m -2.

0 0 5 10 15 20 Circular polarization 10000 DAM Io-DAM LH 1.0 1000 100 HOM KOM 0.5 0.0-0.

1 Past and future observations of Jupiter with Cassini/RPWS Flux 1AU (Log W.m -2.Hz -1 ) DAM Io-DAM HOM KOM Circular polarization DAM Io-DAM LH HOM KOM RH DOY (h) L. Lamy, C. Louis, P. Zarka, B. Cecconi LESIA, CNRS-Observatoire de Paris

2 Outline 1- Catalog of Jovian emissions recorded outside the flyby period 2- Search for planet-satellites interactions during the flyby (a) Using time series of power (b) Using ExPRES simulations

Jupiter flyby 1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 2014 Few studies of Jupiter auroral radio emissions during the 2000-2001 flyby : e.g. - Beam width of HOM-DAM emissions (Kaiser et al.

3 Jupiter flyby Few studies of Jupiter auroral radio emissions during the flyby : e.g. - Beam width of HOM-DAM emissions (Kaiser et al., 2000) - Solar wind control of HOM-DAM (Gurnett et al., 2002 ; Hess et al., 2014) - Average spectrum over 3kHz-16MHz (Zarka, 2004) - DAM beaming (Imai, 2008, 2011, 2015) -

1- Catalog of Jovian emissions outside the flyby 1999 2000 2001 2002 2003 2004 2005 2006 2007 2008 2009 2010 2011 2012

4 1- Catalog of Jovian emissions outside the flyby Earth flyby Jupiter flyby Saturn SOI Flyby period excluded from the catalog (Beaudonnet, Wurmser, internship 2015)

1- Catalog of Jovian emissions outside the flyby 1999 2000 2001 2002 2003 2004

Saturn SOI Flyby period excluded from the catalog 6-month variation of Jupiter

5 1- Catalog of Jovian emissions outside the flyby Earth flyby Jupiter flyby Saturn SOI Flyby period excluded from the catalog 6-month variation of Jupiter radio activity : physical Detections rise again as the S/Cplanet distance decreases

6 1- Catalog of Jovian emissions outside the flyby Jupiter observed Jupiter observed

7 1- Catalog of Jovian emissions outside the flyby Io phase-cml diagram Mainly Io-C Mainly Io-D

8 1- Catalog of Jovian emissions outside the flyby Continuous RPWS observations make it an excellent tracker of Io emissions : => (very) long-term monitoring of the Io-Jupiter interaction => short-term monitoring as well (< 1 rot.) Example : Io-D Io-C

9 Io-D Io-C??? Io-C

10 Io-D Io-C

11 ?? Io-D Io-C

12 Io-D Io-C??

1- Catalog of Jovian emissions outside the flyby 1999 2000 2001 2002 2003

Jupiter observed Jupiter observed 2016-2017 : Cassini/RPWS will likely see

13 1- Catalog of Jovian emissions outside the flyby Jupiter observed Jupiter observed : Cassini/RPWS will likely see Jupiter HOM- DAM simultaneously to Juno/Waves => multi-point + polarization measurements

14 2- Search for planet-satellites interactions during the flyby Earth flyby Jupiter flyby Saturn SOI Flyby period excluded from the catalog High sensitivity + continuous observations

2- Search for planet-satellites interactions during the flyby Method (a) : power time series 10000

Hz -1 1000 100-20 -22-24 10-26 10000 300 320 340 360 Circular polarization degree LH 1000 100 0.

15 2- Search for planet-satellites interactions during the flyby Method (a) : power time series Flux density (@ 1AU) Log W.m -2.Hz Circular polarization degree LH RH DOY Time interval : Southern and Northern power time series (separated by circular polarization) - Normalized to 1 AU

5229 <10-18 ) RH median intensity North(>10-18.

o ) 200 100 Io-A Io-B Io Phase ( o ) 300 200 0 0 100 200 300 CML

occurrence (>10<30) Io : - f = [5-16MHz] 300 - A, B, C and D

16 2- Search for planet-satellites interactions during the flyby Method (a) : power time series LH median intensity South(> <10-18 ) RH median intensity North(> <10-18 ) Io Phase ( o ) Io-C Io-D Io Phase ( o ) Io-A Io-B Io Phase ( o ) CML ( o ) CML ( o ) LH occurrence (>10<30) RH occurrence (>10<30) Io : - f = [5-16MHz] A, B, C and D components all seen - intensity (instead of occurrence) plot => intensity reference Io Phase ( o ) 200

5229 <10-18 ) 300 300 Ganymede Phase ( o ) 200 100 Ga-C?

0 100 200 300 CML ( o ) LH occurrence (>10<30) RH

17 2- Search for planet-satellites interactions during the flyby Method (a) : power time series LH median intensity South(> <10-18 ) RH median intensity North(> <10-18 ) Ganymede Phase ( o ) Ga-C? Ganymede Phase ( o ) CML ( o ) CML ( o ) LH occurrence (>10<30) RH occurrence (>10<30) mede Phase ( o ) Ganymede : - f = [5-16MHz] - Ganymede C emission? mede Phase ( o )

5229 <10-18 ) 300 300 Europa Phase ( o ) 200 100 Eu-D?

18 2- Search for planet-satellites interactions during the flyby Method (a) : power time series LH median intensity South(> <10-18 ) RH median intensity North(> <10-18 ) Europa Phase ( o ) Eu-D? Europa Phase ( o ) CML ( o ) CML ( o ) LH occurrence (>10<30) RH occurrence (>10<30) ropa Phase ( o ) Europa : - f = [1-16MHz] - Europa D emission? ropa Phase ( o )

, 08) f ~ fce 1200 khz v e- e- B SPV - CMI-based visibility modeling with the ExPRES code (Hess et al.

19 2- Search for planet-satellites interactions during the flyby Method (b) : simulations of dynamic spectra 10 khz (Hess et al., 08) f ~ fce 1200 khz v e- e- B SPV - CMI-based visibility modeling with the ExPRES code (Hess et al., 08,11,16; Lamy et al.,08b,13) - updated magnetic field model : ISAaC (>VIPAL) constrained by the locus of both Io and Ganymede UV footprints (Hess, pers. com.) => long-term simulations of Io, Europa & Ganymede

20 2- Search for planet-satellites interactions during the flyby Method (b) : simulations of dynamic spectra Flux 1AU (Log W.m -2.Hz -1 ) Circular polarization LH North South RH DOY (h)

21 2- Search for planet-satellites interactions during the flyby Method (b) : simulations of dynamic spectra Flux 1AU (Log W.m -2.Hz -1 ) Circular polarization LH North South RH DOY (h) Io-D

22 2- Search for planet-satellites interactions during the flyby Method (b) : simulations of dynamic spectra Flux 1AU (Log W.m -2.Hz -1 ) Circular polarization LH North South RH DOY 2000

23 2- Search for planet-satellites interactions during the flyby Method (b) : simulations of dynamic spectra Flux 1AU (Log W.m -2.Hz -1 ) Circular polarization LH North South RH DOY 2000 Io-D

24 2- Search for planet-satellites interactions during the flyby Method (b) : simulations of dynamic spectra Flux 1AU (Log W.m -2.Hz -1 ) Circular polarization LH North South RH DOY 2000 Ga-D!

25 2- Search for planet-satellites interactions during the flyby Method (b) : simulations of dynamic spectra Flux 1AU (Log W.m -2.Hz -1 ) Circular polarization LH North South RH DOY (h) Io-C

26 2- Search for planet-satellites interactions during the flyby Method (b) : simulations of dynamic spectra Flux 1AU (Log W.m -2.Hz -1 ) Circular polarization LH North South RH DOY (h) Io-C Eu-C!

27 2- Search for planet-satellites interactions during the flyby Method (b) : simulations of dynamic spectra (Louis et al., in prep.) : - Catalog of Europa and Ganymede detections + Cassini/RPWS : candidates total : 105 Europa + 69 Ganymede + 3 Europa or Ganymede + Voyager/PRA : 1979 Voyager 1 => 15 candidates total : 10 Europa + 5 Ganymede Voyager 2 => 24 candidates total : 12 Europa + 12 Ganymede NB : One case where Europa was observed by both spacecraft - Search for multi-point measurements (Nançay decameter array). - Characterization of average properties in progress : ocurrence, spectrum, arc shape, multiplicity, intensity, variability etc.

28 Conclusions * Cassini/RPWS regularly tracked Jupiter emissions over and >2013 => unexpected support to Juno? * Outside the flyby period : mainly Io => Io activity can be tracked on long (years) and short (half a revolution) timescales * During the flyby : (a) Satellite phase-cml diagrams of intensity : => all components of Io => possible detection of Europa and Ganymede (b) Simulations of Europa and Ganymede induced emissions : => identification of Europa arcs! => identification of Ganymede arcs! => statistical study in progress.

Occurrence characteristics of Saturn s radio burst

Occurrence characteristics of Saturn s radio burst D. Maruno 1, Y. Kasaba 1, T. Kimura 2, A. Morioka 1, B. Cecconi 3 1 Department of Geophysics, Tohoku University 2 ISAS, JAXA 3 LESIA, Observatorire de