January 11, 2007 Workshop 3e Zone, Nantes. Leslie Young Pluto occultation 2006 June 12 from Australia & New Zealand Leslie Young, Eliot Young, Catherine Ruhland, Catherine Olkin (SwRI) Richard French (Wellesley College) Marc Buie (Lowell Observatory) Jeff Regester (Greensboro Day School, NC) Kevin Shoemaker (Shoemaker Labs, Longmont CO) Martin George (Launceston Planetarium, Tasmania) John Broughton (Reedy Creek, Australia) Grant Christie,Tim Natusch (Auckland Observatory) Ross Dickie, Peter Jaquiery, Graham Blow (RASNZ) Dave Gault (Hawkesbury Heights, Australia) Blair Lade (Stockport Observatory, Australia)
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January 11, 2007 Workshop 3e Zone, Nantes. Leslie Young Pluto occultation 2006 June 12 from Australia & New Zealand Leslie Young, Eliot Young, Catherine.
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January 11, 2007 Workshop 3e Zone, Nantes. Leslie Young
Pluto occultation 2006 June 12from Australia & New Zealand
January 11, 2007 Workshop 3e Zone, Nantes. Leslie Young
Lower Atmosphere Inversion(Ref: Elliot, Person and Qu 2003)
• Small Planet Case• No Ray Crossing• Geometric Optics• Clear Atmosphere
January 11, 2007 Workshop 3e Zone, Nantes. Leslie Young
Immersion
R (km) v. T (K) R (km) v. dT/dr (K/km)
dry adiabat
January 11, 2007 Workshop 3e Zone, Nantes. Leslie Young
Emersion
R (km) v. T (K) R (km) v. dT/dr (K/km)
dry adiabat
January 11, 2007 Workshop 3e Zone, Nantes. Leslie Young
Monte Carlo-Based Error Estimates
• Monte Carlo errors based on 100 simulated lightcurves with appropriate noise.
• The Temperature Inversions: Similar overall shape, similar wiggles, but largest errors (up to ±18 K) above the temperature inversion at 1240 km.
R (km) v. T (K)- Nominal Case- 1-sigma env.
January 11, 2007 Workshop 3e Zone, Nantes. Leslie Young
Effects of an example haze layer
• Haze dramatically changes the lower temperature profile.
• Brings dT/dr closer to a dry adiabat.
Consider the effects of sudden haze onset at 1263 km with a scale height of 15 km.
R (km) v. T (K)
R (km) v. dT/dr (K/km)dry adiabat
January 11, 2007 Workshop 3e Zone, Nantes. Leslie Young
Conclusions• Pluto's bulk atmosphere (geometry):
– 1988 to 2006, pressure has increased by 0.98 ± 0.09 µbar, a factor of 2.17±0.21
– For N2 surface vapor pressure equilibrium, this implies an increase in surface temperature of 1.2-1.7 K.
– Pressures consistant between 2002 and 2006
• Pluto’s upper atmosphere (model fit): – Non-isothermal. dT/dr = -0.127±0.028 K/km– Average (103.9±3.2 K) same as 2002 (104±2 K, isothermal fit),
and 1988 (104.0±7.3 K). – 99.4±3.1 K (ingress, 30.0 S, summer), 105.5±3.5 K (egress, 53.2 N, winter)
dispite ~1500 less insolation averaged over the winter latitude, so not tied to insolation (in a straightforward way)
• Pluto’s lower atm, clear assumption (inversion):– As in 1988 & 2002, not isothermal. – Temperature inversion around 1210 - 1220 km.– Ingress & Egress are qualitatively similar, but the density perturbations differ in detail.
• Pluto’s lower atm, haze assumption (inversion, removing haze from model fit)– Top of haze poorly constrained.– Temperature purturbations qualitatively similar to those seen on Earth, Jupiter, Titan