saturn’s rings: …..some highlights 3d structure of rings: thickness, gravity wakes evolution of...
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Saturn’s Rings: …..some highlights
3D structure of rings: thickness, gravity wakes
Evolution of moonlets in & near the rings: embedded objects F ring region
Composition: a higher dimension: role of meteoroid bombardment
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15km/s
Vrel <<< 15km/s
“Classical” ring model
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Dynamically expected ring model:
Densely packed ring due to inelastic collisions
30m thick
Different powerlaw size distributions
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Cassini VIMS - low resolution, but large wavelength (albedo) range
Coherent backscattering fits better; classical model not supported
Nelson et al 2006; Hapke et al 2006 LPSC
Phase angle
I/F
Wid
th o
f pe
ak
Wavelength (microns)
Lowalbedo
High albedo
The Opposition Effect:
Shadow hiding betweenparticles at low volume density?
or Coherent backscattering from particle surfaces?
1.5
Mishchenko & Dlugach 1992; Akkermans et al 1988; Hapke 2000
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Salo and Karjalainen 2003; cf also Dones et al 1989, 1993; Salo et al 2005
Photometric modeling of non-classical (closely packed) layers(Monte Carlo modeling)
classical dense
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QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
Stellar occultationsby the rings:
Colwell et al submitted
Movie by H. Salo
azimuthal view angledetermines opacity
andelevation angle
gives wake thickness
300m
Self-gravity wakes
2
1
21
VK
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Self-gravity wake properties in the A ring
Colwell et al GRL 2006
To
tal o
ptic
al d
ep
th; G
ap
op
tica
l dep
th
Local, unresolved mixture of high-tau waves and low-tau gapswill affect ring I/F and must be included in photometric models
Wak
e he
ight
/wid
th
0.5
0.4
0.3
0.2
0.1
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ISS approach color composite
A
B
C
C D
F
D
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wavelength, microns
wavelength (microns)
R
IRTF
HST
model
Saturn’s entire B ring
Groundbased reflectance spectrum: water ice bands and reddish material
C ring & CD are darker & less red;‘polluted’ by meteoroid bombardment?
F. Poulet et al. (2003)
98% water ice, 2% carbon, 1% tholins
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Meteoroid Bombardment and Ballistic Transport
Cook & Franklin 1970; Morfill 1983; Ip 1983; Durisen et al 1984, 1989, 1992, 1996; Cuzzi & Estrada 1998
Main rings intercept roughly their own mass in the age of the solar system; large uncertainties in mass flux!
Rings get “polluted”; ejecta moves material around
Structural and compositional evolution; model ages ~ few 108 yr
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wavelength, microns
wavelength (microns)
R
IRTF
HST
model
Saturn’s entire B ring
New Cassini VIMS results: correlation between spectral properties
with high radial resolution (SOI)
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Nicholson et al 2006; Icarus submitted(?)
0.3 - 0.5 slope
0.6 - 0.9 slope
ice band depths
C B A
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Outer A ring
Multiple strandsPrometheus, Pandora,other new objects
F ring
“propellor objects” Encke and Keeler gaps;
containing Pan and Daphnis
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Moonlets within the rings
320 km wide
30 km wide
Pan in Encke gap:complex edges
Daphnis ( r=3.5km )
in Keeler gap
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“Propellor” disturbances by 100 m diameter objects in the A ring
ISS SOI images; 50 m/pxl !
Seiss et al GRL 2005
Tiscareno et al Nature 2006
unlit face of the rings
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A ring“propellors”
(Tiscareno et al Nature 2006)Zebker et al (Voyager)
main ring particles
Fully populated?
N(>
R)
km-2
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So what are these things..?Primordial shards of the ring creation event?
Home-grown by accretion of local ring material?
Need to understand accretion within the Roche limit RR (Smoluchowski 1978,1979; Weidenschilling et al 1984; Longaretti 1989)
Canup & Esposito 1995
Accretion allowed
“tidally corrected”
classical force balance: c ~ CMp/a3 or ac ~ (CMp/)1/3
RR
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Critical density for growth at distance a:
c=9Mp/4a30.15 in A ring
c≈27Mp/4a3CE95) or 9Mp/4a3bc (Weiss et al 2006)
Smoluch., Weid. et al, Longaretti
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….. and the survey says (Porco et al 2006 LPSC)
Critical density for growth at distance a:
Moonlets in and near the rings obey accretion-limited critical density, may be dense shards buried in local ring material.Implication is that “propellor” objects are similar, just smaller.
c=9Mp/4a30.15 in A ring
c≈27Mp/4a3CE95) or 9Mp/4a3bc (Weiss et al 2006)
Smoluch., Weid. et al, Longaretti
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The F ring: tinsel on a massive moonlet belt?
VGR-1 RSSMarouf et al 1986
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1200km
Data: Pioneer 11magnetospheric e,p
Simpson et al 1980
The F ring “moonlet belt”
Unlike G ring
in
out
Van Allen 1982Conjectures:
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F
Van Allen 1982, Cuzzi & Burns 1988
1200km
Data: Pioneer 11magnetospheric e,p
??
Simpson et al 1980
F ring itself a collisional product (1015-16 g; every 102-103 yrs)
Transient clumps of cm-size rubble released in collisions between members of a 2000 km wide belt of moonlets;
mass 1020 - 1021 g (Prometheus + Pandora)
Conjectures:
The F ring “moonlet belt”
Unlike G ring
in
out
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F
Van Allen 1982, Cuzzi & Burns 1988
1200km
Data: Pioneer 11magnetospheric e,p
??
Simpson et al 1980
F ring itself a collisional product (1015-16 g; every 102-103 yrs)
Transient clumps of cm-size rubble released in collisions between members of a 2000 km wide belt of moonlets;
mass 1020 - 1021 g (Prometheus + Pandora)
Conjectures:
Pandora & Prometheus themselves now known to be chaotic (French et al 2003, Goldreich & Rappaport 2003 a.b)
Scargle et al 1993 DPS: Entire F region is probably chaotic (higher order Pandora & Prometheus resonances)
Some Uranian ringmoons appear chaotic; may collide in 0.5Myr(Duncan & Lissauer 1997; Showalter & Lissauer 2006; Showalter this mtg)
Subsequent developments:
HST and Cassini observations of large clumps in F region->
The F ring “moonlet belt”
Unlike G ring
in
out
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McGhee et al 2001 Icarus 152, 282
Arcs 60,000 km long; ~ 10-3
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Transient object 2004S6?
Porco et al 2005, Spitale et al 2006 AJ
PIA07558
PIA07716
10000 km
10-2
1000 km
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S6’
1500km
Pr Pa
S6
C
MM
MM
MA
AA
AA
AA
A
AA
S3/4
JH143141
F ring core
3
S6’’
A collection of F region features….
I/F,
Distance from Saturn
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UVIS
F ring
(Tiscareno et al Nature 2006)Zebker et al (Voyager)Esposito et al 2006, submitted
Actual moonlets in the F ring region
A ring“propellors”
main ring particles
N(>
R)
km-2
Spitale et al 2006
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UVIS
F ring
(Tiscareno et al Nature 2006)Zebker et al (Voyager)Esposito et al 2006, submitted
Optically thin moonlet belt still quite massive (1020-1021g)
CB88
A ring“propellors”
main ring particles
N(>
R)
km-2
Spitale et al 2006
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F ring
(Tiscareno et al Nature 2006)Zebker et al (Voyager)Esposito et al 2006, submitted
Evolution of the F ring (strand) itself: ?
A ring“propellors”
main ring particles Barbara & Esposito 2004Esposito et al 2006
(km-2 in a narrow ringlet)
3x1020g
N(>
R)
km-2
Spitale et al 2006
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Summary
Gaining good 3D understanding of micro-ring structure: key implications for ring photometry, particle albedo.“Classical” photometric models are obsolete for A, B rings.
Ring composition varies in slow and systematic ways across abrupt mass boundaries; ring composition = intrinsic icy-organic with added ‘cometary’ pollution?Need a better estimate of mass flux to age-date the rings.
Embedded and nearby ringmoons seem to obey accretion- limited densities; any primordial shards are deeply buried.Size distribution for 10m < r < few km is telling us something.
1500-km wide F region may be full of chaotically moving moonlets. Evolutionary modeling should allow for this.Large distributed mass may have dynamical implications.
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1914-2006
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Structural evolution creates
familiar structures in << Tss;“ramps” seen at inner B & A edges
Compositional evolution createsglobal compositional variations: smooth color/composition profiles
across abrupt ring boundaries
Simultaneously,
Durisen et al 1996
Implication: rings started as icy-organic material
and became polluted by dark,neutrally-colored
material.
Meteoroid Bombardment and Ballistic Transport
Estrada et al 2003
May be able to age-date the ringsthis way; several unknowns
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Scargle et al 1993: F region chaos ( higher order resonances)?
2000km
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QuickTime™ and a decompressor
are needed to see this picture.
SOI
RPWS experiment detects “tones” from meteoroids hitting the rings (?)
Gurnett et al Fall AGU 2004
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Mass flux - the big unknown!
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Transient objects?“2004S6”.. Or not?
Charnoz et al Science 2006
X
Spitale et al
Moonlet belt collision? Meteoroid impact?
Cuzzi & Burns 1988, Showalter 1998, Poulet et al 2000, Barbara & Esposito 2002
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See Mitchell et al Science 2006
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F
Cuzzi & Burns Icarus 1988
1200km
Pioneer 11 data
L
c ~ 10(1km/L)
c ~ 10-3,
L~20000?
??
Van Allen 1982
F ring itself a collisional product (more rare; 102-103 yrs)
Transient clumps of cm-size rubble released in collisions between members of a 2000 km wide belt of 0.3-3 km moonlets and total mass of about 1021 g (Prometheus) .
Conjectures:
The F ring “moonlet belt”
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Particle sizes from radio occultation
Blue = small; red = large, white = very opaque
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Stellar Occultation Variation Summary
UVIS
Colwell et al GRL 2006cassini
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135000
140000
142000
145000
Smoluchowski 1978, 1979; Canup & Esposito 1995; Karjalainen & Salo 2004 Icarus
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The Opposition Effect: Shadow hiding and low volume density?
or
Coherent backscattering?
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Ring microstructure
A ring wakes: gaining full 3D picture: what does it mean?B ring wakes? C ring and CD ?
Colwell et al, Sremcevic et al this mtg
Ring thermal & RSS observations Leyrat et al, Marouf et al this mtg
Implications: Photometric models must treat dense layers: Deau et al , Dones et al, Weiss et al, Chambers et al
More complications for photometric modeling:
wakes: high & low optical depth in same pixel!
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Implications for shards / propellors:
Accretion in the rings is possible but limited by needed compaction to keep rho > rho_crit
Objects can keep growing AT rho_crit until they open a gap around themselves. Propellor objects, perhaps, or maybe larger (likely size dist)
Can’t learn about primordial material from studying these, on surface, too bad, but lots of intriguing parallels to protoplanetary evolution and time-dependent ring structure come to mind
Next treat a related but different problem
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“Narrow, stranded” F ring: the tail, not the dog?
Objects between Pandora & Prometheus lead chaotic lives
Orbits become eccentric; collisions occur in 1500km wide zoneResulting debris clumps spread & are swept up by other objects
Evidence exists for transient clumps/arcs of length ~ 103 - 105 km HST and Cassini, in addition to Pioneer 11 microsignatures
Prediction: Cassini will see more and larger clumps and arcs
Speculation: F ring itself only one of the larger, more recent events
Speculation: might 1021g (or more!) have an influence on nearby orbits?
Collisional belt modeling must be redone with induced chaotic e’s