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![3 [1], [2], [3], [2], [4], [5], [3], [1], [1],](/docs-images/89/98141371/images/1-2.jpg "[1], [3], [2], [3], [1], [2] ISAS, [3], [4], [5]")
1 3 [1], [2], [3], [2], [4], [5], [3], [1], [1], [1], [3], [2], [3], [1], [2] ISAS, [3], [4], [5] NICT
2 - Launch : Sep 14, 2013, Epsilon rocket -Size 1m 1m 4m (w.o. solar panel) -Orbit 950km 1150km (LEO) - Inclination: 31 deg - Orbital period : 106 min NASA-PSP ISSI JSPS sakura JUNO (1) 2013/9-1 (2) 2014/ /3 (3) 3
![2016] (Poster P-120, 121) [Kimura et al.](/docs-images/89/98141371/images/3-2.jpg "2016, Tao et al. 2016a, 2016b, Kita et al.")
![2015] [Yoneda et al.](/docs-images/89/98141371/images/3-4.jpg "2015] (Poster P-119) [Masunaga et al.")
3 [Yoshioka et al. 2014, Kimura et al. 2015, Badman et al. 2015, Yoshikawa et al. 2016] (Poster P-120, 121) [Kimura et al. 2016, Tao et al. 2016a, 2016b, Kita et al. 2016, Murakami et al. 2016] [Tsuchiya et al. 2015] [Yoneda et al. 2015] (Poster P-119) [Masunaga et al. 2015, 2016] [Nara et al. 2016] [Kuwabara et al. 2016] EUV stars He
4 SPATIALLY RESOLVED SPECTRUM FROM HISAKI Yoshioka et al. Science, 2014
5 Electron density Core ele temp. Hot ele fraction Radial plasma distribution around Jupiter (Yoshioka et al. Science, 2014, Yoshioka et al., 2016) Observation Electron density is ~1500 /cc at 5.9RJ Core temperature ~5eV [S2+] > [S+] > [S3+] (2:4:1) Higher density of hot electrons at outer torus. Physical model (mass & energy balances) Hot ele density [S+] Plasma transport cased by interchange instability [S++] [S+++]
6 Energy coupling between middle and inner magnetospheres (Yoshikawa et al., 2016) Pairs of brightening of plasma in inner magnetosphere and aurorae Jan. 4, 01:10:40 UT (Kimura et al. 2015) Brightening of aurora (middle magnetosphere) is earlier than that of that in the inner magnetosphere by several hours. Evidence of fast radial transport of energy in the rotation dominant magnetosphere.
7 Jupiter: Discovery of internally-driven aurora & hot plasma injection Morphology of auroral explosion(hst) Internally-driven auroral explosions and hot plasma injection were found during the solar wind quiet period, Kimura et al. under review showing global activation of magnetosphere
8 Jupiter aurora enhancement (Kimura et al., GRL 2015, Tao et al., JGR, 2016a, 2016b) Poster P-120 (i) compression / plasma injection adiabatic change of plasma Auroral electron energy and flux are derived from aurora spectra Aurora power enhancements are mainly due to increased electron flux, not energy, independent of drivers. emission enhancement quiet (ii) change of emission location open-closed middle magnetosphere
![) [GW] [npa]](/docs-images/89/98141371/images/9-4.jpg "[GW] Day of")
9 Jupiter s aurora response to the solar wind (Kita et al., 2016) Poster P-121 ( ) [GW] [npa] [GW] Day of year (2014) [day]
![Electro-magnetic coupling between planet & satellite (Tsuchiya et al., JGR, 2015) (68.0nm)[ ] Brightness [R] 50 40 30 20 10 0 50 40 30 20 10 400 300 200-90 0 90 180 270 SIV 65.](/docs-images/89/98141371/images/10-4.jpg "7 [ ] SIII 68.0 Io upstream SIII 70.2 SIII 72.9 SIV 74.8 0 50 65 70 75 Wavelength [nm] downstream SII 76.5 15 10 5 0 15 10 5 SIV 80.9 SIII 82.2 OII 83.4 flow SII 87.5 SII 90.")
![6 SIII 90.1 0 15 80 85 90 Wavelength [nm] upstream Io downstream Jupiter Observed spectra 0-90 degrees 180-270degrees Observation downstream upstream Model spectra (T e =4.](/docs-images/89/98141371/images/10-5.jpg "3eV) f he =1.0% f he =1.7% f he =2.")
10 Electro-magnetic coupling between planet & satellite (Tsuchiya et al., JGR, 2015) (68.0nm)[ ] Brightness [R] SIV 65.7 [ ] SIII 68.0 Io upstream SIII 70.2 SIII 72.9 SIV Wavelength [nm] downstream SII SIV 80.9 SIII 82.2 OII 83.4 flow SII 87.5 SII 90.6 SIII Wavelength [nm] upstream Io downstream Jupiter Observed spectra 0-90 degrees degrees Observation downstream upstream Model spectra (T e =4.3eV) f he =1.0% f he =1.7% f he =2.5% Model Brightness enhancement downstream of Io Spectrum analysis Electron heating Efficient heating mechanism Energy extracted at Io : 1TW Electron heating : 140GW
11 Venus : Periodic EUV dayglow variations Masunaga et al., 2015, 2016 SOHO Solar EUV flux [cm-2s-1] Hisaki OI 1356 Brightness [R] Venus Duskside Sun Earth (Hisaki) Normalized power Dawnside 99 % confidence level 3.7 days Poster P-119 Solar rotational effect ~4 day periodic dayglow variations on the dawnside of Venus Coupling between the upper and middle atmospheres via atmospheric waves?
12 Detection of (Nara et al., ICARUS, 2016) LBH bands in the Venus atmospehere Due to long exposure time, a lot of emissions are newly identified in the Venusian spectrum. By using the information about relative intensities of molecular bands, blended emissions are resolved. N a-x Lyman-Birge- Hopfield (LBH) bands are detected for the first time. - synthetic CO A-X bands - Venusian spectrum - synthetic CO A-X bands - residual spectrum - synthetic CO A-X bands - residual spectrum - synthetic N a-x bands - residual spectrum - synthetic N a-x bands - residual spectrum Repeatedly, the fitted synthetic spectra are subtracted from the Venusian spectrum.
13 Coupling effect between exosphere & plasmasphere (Kuwabara et al. 2016) Observational results Lyman-alpha column brightness increase during geomagnetic storms Changes in the Lyman-alpha brightness lagged behind geomagnetic storms by several hours Mechanism Charge exchange ( ) -> provides a hot hydrogen and contributes dominantly to the loss of neutral atom 1. Plasmapause location moves inward during increasing magnetic disturbance 2. Collisional region along the LoS decreases 3. Charge exchange is suppressed 4. Column density of neutral hydrogen increases due to a decrease in the loss
14
15 JUNO/ NASA JUNO In-situ: continuous close-up: once flyby / 2 months NASA HST 10s nights / year Ground-based telescope Visible/IR/Radio Subaru: several nights / year IRTF: 10s nights / year continuous JAXA HISAKI Dedicated telescope continuous
16 ( ) NASA-PSP Hisaki Participating scientist program Modeling NASA/JUNO-HISAKI : US:9, Japan:18 Three meetings in 2016 ISSI ( The influence of Io on Jupiter s Magnetosphere : UK:3, US:2, Belgium:1, France:1, Japan:7 First meeting on Sep JSPS SAKURA program ( Coordinated observational and theoretical researches for Jovian and Kronian auroral radio emissions : France:9, Japan:14 Three meetings in 2016
17 - MHD Fukazawa et al. (2006) (NASA-PSP) Delamere et al. (2004, 2005) (NASA-PSP ISSI) Smith, T.. Fukazawa et al. (2006)
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