origins of regular and irregular satellites
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Origins of Regular and Irregular Satellites. ASTR5830 March 19, 2013 12:30-1:45 pm. Regular vs. Irregular Satellites. Regular:. Irregular:. Exist in a large range of e and i . Typically, smaller. Thought to be captured from heliocentric orbit. Orbits extend to ~ 0.5 r H . - PowerPoint PPT PresentationTRANSCRIPT
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Origins of Regularand
Irregular Satellites
ASTR5830March 19, 201312:30-1:45 pm
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Regular vs. Irregular Satellites
Regular:• Coplanar, low eccentricity
and small inclination orbits.• Typically, larger.• Thought to have formed in
situ.• Inhabit a small fraction of
host planet’s Hill sphere.
Irregular:• Exist in a large range of e
and i.• Typically, smaller.• Thought to be captured
from heliocentric orbit.• Orbits extend to ~ 0.5 rH.
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Giant Planet Formation
• Core Accretion Model• Extended envelope that fills the planet’s Hill
sphere. (rH,J = 744 RJ)• Gap Opening– Mp= 100ME
– Continuing Accretion• Disk Formation– Accretion– Spin-out
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Observational Constraints on Regular Satellite Formation
• Coplanar, Circular orbits– e ~ 0.01 and i < few degrees– formed in a disk, miniature solar system
• MS= 10-4 MP
– similar processes.• 50/50 Ice-Rock Fraction
– low temperatures• Decreasing Ice-Rock fraction with distance
– Disk gradients or subsequent evolution?• Incomplete differentiation of Callisto and Titan
– Long formation timescales: >105 yr• Formed at the tail end of Giant planet formation.
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Minimum Mass Sub-Nebula (MMSN)
• Lunine and Stevenson (1982)• Augment solid mass of satellites to solar
composition and spread out mass based on satellite locations.
• Results in a very massive disk with numerous problems.
ΣS ≈ 3×103 g cm−2
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Problems with MMSN Approach
• Rapid Accretion of Satellites
• Orbital Decay– Gas drag on small particles: 103 yrs– Type I migration on larger bodies: 102 yrs– Type II migration on largest bodies: 103 yrs
τ A = 50 yr RS
2500 km⎛⎝⎜
⎞⎠⎟
ρS
2 g cm−3
⎛⎝⎜
⎞⎠⎟
10Fg
⎛⎝⎜
⎞⎠⎟
3×103 g cm−2
ΣS
⎛⎝⎜
⎞⎠⎟
r15 R J
⎛⎝⎜
⎞⎠⎟
MS
M J
>10−5
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Problems with MMSN Approach
• Temperature too hot unless disk is inviscid.
– Implies a disk lifetime of ~ 106 yrs• Dynamical Constraints– Forced eccentricity of satellites– Obliquity of Jupiter
α ≤10−6
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Gas-Starved Disk Model
• Canup and Ward (CW; 2002)• Solids build up slowly over time, analogous to
the accumulation of solids in a water pipe over time.
M J&M J
=τ J =106 yr
ΣS = few ×102 g cm−2
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Tanigawa et al. (2012)
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CW semi-analytic disk models
α =5 ×10−3
τ J = 5 ×106 yr
Canup and Ward (2002)
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Problems Solved by CW model
• Longer formation timescales
• Lower temperatures allow for condensation of ices.• Subsequent tidal evolution causes inner satellites to
thermally evolve and differentiate.• Solids are delivered by entrainment in accretion flow.
– Small enough to capture, small enough to deliver• Differential migration places satellites in Laplace
resonances.
τ A ≥ 105 yr for τ J ≥ 105 yr
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Satellite Formation and Survival
• Multiple generations of satellites are formed and lost through migration into the host planet.
• Quasi-steady state is achieved with ~10-4 MP in satellites retained in the disk.
• Inflow cutoff from the solar nebula may explain Jupiter-Saturn dichotomy.
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Common Mass Scaling for Satellite Systems of Gaseous Planets
Canup and Ward (2006)
The total mass in satellites, MT, scaled to the planet’s mass, MP, is shown versus time. The green, blue and red lines corresponding respectively to simulations with (a/f) = 10-6, 5x10-5 and 5x10-2.
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Jupiter-Saturn Dichotomy
Sasaki et al. (2010)
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Two-Phase Disk Model
• Mosqueira and Estrada (ME; 2003a,b)• Two-component disk based on the mass of
satellites, with a massive inner disk and a less massive outer disk.
• Requires very low viscosities.• Relies on planetessimal capture for delivery of
solids.• Satellites survive against migration by opening
gaps in the circumplanetary disk.
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What is Needed?
• Better understanding of the viscous processes at work in circumplanetary disks.
• Higher resolution, non-isothermal, viscous simulations of infall from the solar nebula onto circumplanetary disks.