H 3 + in Giant Planet Ionospheres Tom Stallard Tom Stallard H 3 + in Giant Planet Ionospheres R OYAL...
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Transcript of H 3 + in Giant Planet Ionospheres Tom Stallard Tom Stallard H 3 + in Giant Planet Ionospheres R OYAL...
H3+ in Giant Planet Ionospheres Tom Stallard
Tom Stallard
H3+ in Giant Planet Ionospheres
Royal Society Meeting: Chemistry, astronomy and physics of H3+
Henrik Melin, Steve Miller, James O’DonoghueStan W.H. Cowley, Sarah V. Badman, Alberto Adriani, Robert H. Brown, Kevin H. Baines
H3+ in Giant Planet Ionospheres Tom Stallard
1.8 μm 4.2 μm
Jupiter absorptionEarth absorption
H3+ in Giant Planet Ionospheres Tom Stallard
1
11
H2 + e* H2+ + e + e
2
2 H2 + h H2+ + e
H3+ in Giant Planet Ionospheres Tom Stallard
H, H2 H2 = H2+ H2
+ + H2 = H3+ … … … H3
+
1 2 3
Energetic particle precipitation
H3+ in Giant Planet Ionospheres Tom Stallard
H3+ in Giant Planet Ionospheres Tom Stallard
H3+ in Giant Planet Ionospheres Tom Stallard
Measured Calculated
Jupiter 940 K 203 K
Saturn 420 K 177 K
Uranus 800 K 138 K
Neptune 600 K 132 K
Lam et al., 1997
Yelle and Miller, 2004
Temperature changes and energy inputs in Giant Planet
atmospheres: what we are learning from H3
+ observations
H3+ in Giant Planet Ionospheres Tom Stallard
Uranus
1987
H3+ in Giant Planet Ionospheres Tom Stallard
Uranus
2007
H3+ in Giant Planet Ionospheres Tom Stallard
Melin et al., 2011
H3+ in Giant Planet Ionospheres Tom Stallard
Melin et al., 2011
H3+ in Giant Planet Ionospheres Tom Stallard
Jupiter
H3+ in Giant Planet Ionospheres Tom Stallard
Heating/cooling term 8 September 11 September
Joule heating and ion drag 67.0 mW m−2 277.0 mW m−2
Particle precipitation 10.8 mW m−2 12.0 mW m−2
Downward conduction (−)0.3 mW m−2 (−)0.4 mW m−2
E(H3+) cooling (−)5.1 mW m−2 (−)10.0 mW m−2
Hydrocarbon cooling (−)65.5 mW m−2 (−)103.3 mW m−2
Net heating rate 7.4 mW m−2 175.3 mW m−2
Stallard et al., 2001; 2002
Melin et al., 2005
H3+ in Giant Planet Ionospheres Tom Stallard
Heating/cooling term 8 September 11 September
Joule heating and ion drag 67.0 mW m−2 277.0 mW m−2
Particle precipitation 10.8 mW m−2 12.0 mW m−2
Downward conduction (−)0.3 mW m−2 (−)0.4 mW m−2
E(H3+) cooling (−)5.1 mW m−2 (−)10.0 mW m−2
Hydrocarbon cooling (−)65.5 mW m−2 (−)103.3 mW m−2
Net heating rate 7.4 mW m−2 175.3 mW m−2
Stallard et al., 2001; 2002
Melin et al., 2005
H3+ in Giant Planet Ionospheres Tom Stallard
Saturn
1
1 380 ± 70 K (17 September 1999)420 ± 70 K (2 February 2004)
Melin et al., 2007
22 440 ± 50 K (10 September 2008) Melin et al., 2011
H3+ in Giant Planet Ionospheres Tom Stallard
R-branch P-branchQ-branch
H3+ in Giant Planet Ionospheres Tom Stallard
Auroral variability:
•Solar wind variations•Variations at the planetary period•Variations associated with magnetospheric conditions
H3+ in Giant Planet Ionospheres Tom Stallard
H3+ in Giant Planet Ionospheres Tom Stallard
H3+ in Giant Planet Ionospheres Tom Stallard
Median Time of observation
Temperature Renormalised emission
a) + b) 04:35 611 K (±20) 0.934c) + d) 08:50 611 K (±20) 1.000e) + f) 13:04 567 K (±20) 0.498
• 44K in 254 minutes represents a temperature change of 2.887 mKs-1
• cooling rate of:
7.8x1012 W for the whole column above the homopause
3.2x1012W for the column above the main H3
+ emission layer
H3+ in Giant Planet Ionospheres Tom Stallard
SummaryUranus has shown long-term variability aligned with seasonal changes
• suggests connections with the magnetospheric structure or the deep atmosphere
Jupiter has shown the importance of Joule heating and ion drag
• suggests heating from the lower thermosphere
Saturn has shown significant variability, including significant cooling, on short timescales
• suggests in-situ energy exchange, through winds
By understanding why different planets are affected in such different ways and the energy inputs that drive these differences, we will make
significant strides into explaining why the upper atmospheres are so hot