13 november 2007 class #21 astronomy 340 fall 2007
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1 3 N O V E M B E R 2 0 0 7
C L A S S # 2 1
Astronomy 340Fall 2007
Review/Announcements
HW #4 due nowHW #5 handed out on Thursday, due Nov 29Last Time
Moons of Jupiter Io Europa
Titan
Discovered in 1655 by Huygens2nd largest moon
R = 2575 km Density = 1.9 gm cm-3
Orbital properties 4:3 resonance with Hyperion Somewhat eccentric effect of tidal forces?
Titan’s Atmosphere
1st detected 1944Composition (pre-Cassini)
CH4 plus some C2H6, CH3D, C2H2, HCN Voyager detected N2 98% N2 Pressure comparable to Earth’s
CH4 cycle Liberated from ethane/methane oceans Some migrates upwards Dissociation & photolysis H2 + hydrocarbons
H2 may escape CxHy haze/clouds remain Possible methane/ethane snow/rain
Titan’s Atmosphere
Titan’s Clouds (Griffith et al. 2000)
Techniques Variations in brightness = variation in albedo = presence of
clouds Spectral windows = different depths
Stratosphere reflects at 2.17-2.4 μm Deep into atmosphere, but not surface 2.12-2.17 μm Surface 2.0-2.11 μm
Results Variations in brightness in 2.12-2.17 μm window Low covering factor (<5%) Altitude ~ 25-30 km
Titan’s Clouds (Samuelson et al 1983)
Effects of surface temperature variationTsurf ~90-95K, lows ~70 K, highs ~180 K
Atmospheric processes Greenhouse effect Absorption via hydrocarbons Photolysis of CH4 reservoir
Titan’s Surface
Titan’s Surface – Radar Mapping
Titan’s Surface
Titan’s Surface
Note variation in color variation in surface featuresBright spot is of particular interest CO2 ice?
Titan’s Surface
Cassini Trajectory
Surface Liquid on Titan?
Hydrocarbon lake?
Old river beds?
The surface of Saturn's largest satellite—Titan—is largely obscured by an optically thick atmospheric haze, and so its nature has been the subject of considerable speculation and discussion1. The Huygens probe entered Titan's atmosphere on 14 January 2005 and descended to the surface using a parachute system2. Here we report measurements made just above and on the surface of Titan by the Huygens Surface Science Package3, 4. Acoustic sounding over the last 90 m above the surface reveals a relatively smooth, but not completely flat, surface surrounding the landing site. Penetrometry and accelerometry measurements during the probe impact event reveal that the surface was neither hard (like solid ice) nor very compressible (like a blanket of fluffy aerosol); rather, the Huygens probe landed on a relatively soft solid surface whose properties are analogous to wet clay, lightly packed snow and wet or dry sand. The probe settled gradually by a few millimetres after landing.
Zarnecki et al. 2005 Nature 438 792
Structure of Titan
Surface landing site was firm possible liquid below
Evidence of some liquid on surface
Surface pressure is sufficient (1.5 bar)
Methane on Titan
D/H ratio 80-90 ppm higher than solar, less than ocean water, comets,
chondrites (300 ppm) Methane likely not from comets
Lifetime Photolyzed in 10 million years Requires replenishing
Surface ocean? Interior outgassing? Implies D/H ratio reflects initial composition
CO, N2 CH4, NH3 (Lewis & Prinn 1980)
CH4 present in the feeding zone at 10 AU Satellites form via accretion, methane locked in interior Requires periodic (constant?) outgassing
Outgassing Model (Tobie, Lunine, Sotin 2006)
Planetary Rings
A Little History 1610 Galileo discovered rings; they disappeared in 1612 1659 Christian Huygens discovered disk-like nature 1977 Uranus’ rings discovered during occultation 1979 Voyager 1 discovered Jupiter’s rings 1980s Neptune’s arc-like rings discovered via occulation
Cassini-Huygens Science - Rings
Study configuration of the rings and dynamic processes responsible for ring structure
Map the composition and size distribution of ring material
Investigate the interrelation of Saturn’s rings and moons, including imbedded moons
Determine the distribution of dust and meteoroid distribution in the vicinity of the rings
Study the interactions between the rings and Saturn’s magnetosphere, ionosphere, and atmosphere
Basic Properties
Solid disk vs particles Too big to rotate as solid body Maxwell rings are particles
100m thick vs 105 km wide (Saturn)Just one ring? NoAll reside within Roche limit of planet
Ring Comparison
Jupiter Main ring – bigger particles, more scattering Halo – interior component, orbits scattered by interaction with
Jupiter’s magnetic field Gossamer – very low density, farther out more inclined orbit
so its fatterUranus
6 identified rings Thickness ~10 km, width ~250000 km Very close to being in circular orbit
Rings: Uranus & Neptune
Uranus’ rings Neptune rings
Particle Size Distribution
Power law n(r) = n0r-3 number of 10 m particles is 10-9 times less than # of 1 cm particles
Total mass distribution is uniform across all binsCollisions
Net loss of energy flatten ring Fracture particles power law distribution of particle size But, ring should actually be thinner and radially distribution
should gradually taper off, not have sharp edges
Measuring Composition
Poulet et al 2003 Astronomy & Astrophysics 412 305
Ring Composition
Water ice plus impurities
Color variation = variation in abundance of impurities
What could they be?
Ring Composition
Red slope arises from complexcarbon compounds
Variation in grain size includedin model 90% water ice overall
Comparative Spectroscopy
olivine
Ring particle
Ring Dynamics
Inner particles overtake outer particles gravitational interaction
Ring Dynamics
Inner particles overtake outer particles gravitational interaction Inner particle loses energy, moves closer to planet Outer particle gains energy, moves farther from planet Net effect is spreading of the ring
Spreading timescale = diffusion timescale
Ring Dynamics
Spreading stops when there are no more collisionsIgnores radiation/magnetic effects that are linearly
proportional to the sizeExact distribution affected by
Differential rotation Presence of moons and resonances with those moons
Saturn’s Rings
D ring: 66900-74510 C ring: 74568-92000
Titan ringlet 77871 Maxwell Gap: 87491
B ring: 92000-117580Cassini divisionA ring: 122170-136775F ring: 140180 (center)G ring: 170000-175000E ring: 181000-483000
Structure in the Rings
Let’s look at some pictures and see what there is to see….
Structure in the Rings
Let’s look at some pictures and see what there is to see…. Gaps Ripples Abrupt edges to the rings Presence of small moons
Moons and Rings
Perturb orbits of ring particles Confine Uranus’ rings, create arcs around Neptune
Shepherding – two moons on either side of ring Outer one has lower velocity slows ring particle, particle
loses energy Inner one has higher velocity accelerates ring particle,
particle gains energy Saturn’s F ring is confined between Prometheus and Pandora
Shepherds in Uranus’ ring system
Moons and Rings
Perturb orbits of ring particles Confine Uranus’ rings, create arcs around Neptune
Shepherding – two moons on either side of ring Outer one has lower velocity slows ring particle, particle
loses energy Inner one has higher velocity accelerates ring particle,
particle gains energy Saturn’s F ring is confined between Prometheus and Pandora
Resonances Similar to Kirkwood Gap in asteroid belt 2:1 resonance with
Mimas