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Warm Saturns: Rings Around Exoplanets that Reside Inside the Ice Line

Warm Saturns: Rings Around Exoplanets that Reside Inside the Ice Line. Hilke E. Schlichting (UCLA) Hubble Postdoctoral Fellow. Extreme Solar Systems II September. 14 th 2011 Schlichting & Chang (2011), ApJ 734, 117. Obvious Obstacles:. Poynting-Robertson drag timescale.

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Warm Saturns: Rings Around Exoplanets that Reside Inside the Ice Line

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  1. Warm Saturns:Rings Around Exoplanets that Reside Inside the Ice Line Hilke E. Schlichting (UCLA) Hubble Postdoctoral Fellow Extreme Solar Systems II September. 14th 2011 Schlichting & Chang (2011), ApJ 734, 117

  2. Obvious Obstacles: Poynting-Robertson drag timescale Rings must be rocky! • Best ring candidates have a > 0.1 AU • Ring lifetimes due to Poynting-Robertson drag 106-109 years

  3. Rings vs. Moons RRoche RP ρice ~ 1g/cm3 ρrock ~ 2-5g/cm3

  4. Roche Radius For Saturn: RRoche/RP~2.2 (ice:1g/cm3) RRoche/RP~1.5 (rock:3g/cm3) ρ =3g/cm3 ρ =5g/cm3 (Schlichting & Chang, 2011)

  5. Laplace Plane RL > RRoche RL < RRoche J2: Quadrupole Gravitational Harmonic

  6. Warped Rings For Reference: J2 of Uranus & Neptune ~ 0.003 J2 of Jupiter & Saturn ~ 0.01 (Schlichting & Chang, 2011)

  7. Ring Light Curves Transit duration ~ 6 hours Time in ingress/egress ~ 2 hours RP=1 RJ RR1=2.0 RP RP2=2.5 RP RP=1.8 RJ RP=1 RJ RR1=1.5 RP RP2=2.5 RP RP=1 RJ RR1=2.0 RP RP2=2.5 RP Quadratic Limb Darkening as in Mandel & Agol (2001), for Ring light curves see also Barnes & Fortney (2004)

  8. Ring Properties &Possibility for Detection • Rings may be common • Rings must consist of rocky material • Some Rings maybe warped J2 • Best candidates for ring detection have a > 0.1 AU • Obliquity damping, temperature, ideally want short cadence

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