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Planets in Debris Disks

Planets in Debris Disks. Planet-Debris co-evolution Where can debris exist? Cases: Solar system, upsilon Andromedae, 47 Ursae Majoris What we are learning from the Kuiper Belt. Renu Malhotra University of Arizona. Debris tells planets where to move; planets tell debris where to stay.

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Planets in Debris Disks

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  1. Planets in Debris Disks • Planet-Debris co-evolution • Where can debris exist? Cases: Solar system, upsilon Andromedae, 47 Ursae Majoris • What we are learning from the Kuiper Belt Renu Malhotra University of Arizona Debris tells planets where to move; planets tell debris where to stay. STScI May Symposium, 2005

  2. Final stages of planet formation: planet-debris co-evolution Two possible evolutionary paths: • Planet-planetesimal disk interactions: migration as in our solar system -- planet eccentricities remain damped while semimajor axes spread out. Evidence in the solar system: Asteroid belt, Kuiper Belt, Oort Cloud. • Planet-planet interactions: if the debris disk mass is insufficient, planet eccentricities will not remain damped, crossing orbits will develop, leading to mergers, scattering, ejection. Evidence in upsilon Andromedae (Ford et al 2005) STScI May Symposium, 2005 Malhotra

  3. Planet-debris co-evolution Model prediction Observed orbital distribution A simulation - Hahn & Malhotra, 1999 STScI May Symposium, 2005 Malhotra

  4. Dynamical constraints on debris location Single planet perturbations: • Hill stability ∆a/ap> 2.4(mp/m*)1/3 ≈ 3RH • Resonance overlap ∆a/ap> 1.5(mp/m*)2/7 • Eccentric planet r  (q-3RH,Q+3RH) STScI May Symposium, 2005 Malhotra

  5. Dynamical constraints on debris… Two planet system • No analytic global stability criterion • Direct numerical integration of test particles • Secular stability analysis • -- Laplace-Lagrange secular theory for planets: linear modes. • E.g. g5,g6 for Sun-Jupiter-Saturn system • -- Secular resonances of debris (test) particles • E.g. 5,6 for Sun-Jupiter-Saturn • -- Eccentricity excitation depends strongly on a, weakly on m1/m2 STScI May Symposium, 2005 Malhotra

  6. upsilon Andromedae • Possible debris locations: • 0.06 - 0.3 AU • beyond 8 AU • 47 Ursae Majoris • Possible debris locations: • 0.3 - 0.6 AU • beyond 7.5 AU Consistent with numerical simulations (e.g., Rivera & Lissauer) STScI May Symposium, 2005 Malhotra

  7. Solar system debris • Possible locations: • inward of 0.5 AU • 0.8 - 1.6 AU • 2.0 - 4.3 AU • beyond 18 AU STScI May Symposium, 2005 Malhotra

  8. Solar system debris: the Kuiper Belt Art by Don Dixon (2000) STScI May Symposium, 2005 Malhotra

  9. Kuiper Belt Dynamical Structure • Resonant KBOs (3:2, 2:1, 5:2) • Main belt (40<a<47 AU) hot and cold components • Scattered disk (a>50 AU & 30<q<36 AU) • Extended scattered disk (a>>50 AU & q>36 AU) • Edge at 50 AU … All these suggest • Resonance sweeping • 9 AU outward migration of Neptune • Excitation of e’s and i’s -- stellar encounter? rogue planets? long term chaos? STScI May Symposium, 2005 Malhotra

  10. Size distribution • Observed KBOs have diameter 10<D<1000 km. • N(D>100 km) ~ 5x104 Total mass (<50 AU) ~ 0.03 earth-mass. classical disk mass ~ 0.01 earth-mass. • Size-class corelations - excited KBOs have more large objects and fewer small objects compared to classical disk • Accretion models suggest that D>100 km KBOs must have formed in a massive (10-30 EM), dynamically cold disk (e,i<0.001) Bernstein et al., 2004 Red=“classical disk”: i<5 deg, 38<d<55 AU Green=“excited disk” • Some process has disturbed the Kuiper Belt, excited the KBO orbits and eroded its mass. • The origin of the short-period Jupiter-family comets is uncertain. STScI May Symposium, 2005 Malhotra

  11. Kuiper Belt dust • Dust density nearly constant in outer solar system (Pioneer 10,11; Voyagers 1,2) • KB dust production rate (1m--1mm) ~ 1015 g/y [eqv. D ~ 1 km comet ground to dust every year.] • Small particles (r < 0.5m) are blown out by radiation pressure • Bound dust grains spiral inward under Poynting-Robertson (PR) drag • Temporary trapping in Neptune’s MMRs produces azimuthal structure • Gravitational scattering by Jupiter,Saturn ejects most particles; very small fraction of KB dust enters the inner solar system Model from Moro-Martin & Malhotra, 2003 STScI May Symposium, 2005 Malhotra

  12. Lessons for debris disks Massive planets within debris disks will shepherd the dust grains Without planets with Solar System planets minimum at Neptune’s position (to avoid resonant planet) Neptune ring-like structure along Neptune’s orbit (trapping into Mean Motion Resonances) clearing of dust from inner 10 AU (due to gravitational scattering by Jupiter and Saturn) Uniform density disk Massive planets will also scatter and eject dust particles, creating gaps or `inner holes’. A planet-detection technique complementary to RV STScI May Symposium, 2005 Malhotra

  13. A history of Kuiper Belt dust A schematic history of the outer solar system dust production rate STScI May Symposium, 2005 Malhotra

  14. Summary and Conclusions • Planet-debris interactions: evidence in the architecture of planetary systems (Sol Sys, ups And) • Secular stability analysis: locates debris in a planetary system • The solar system debris has a complex dynamical structure • Cannot be explained simply by planetary perturbations. • Planet migration explains a lot, but probably not all. • Kuiper Belt dust and extra-solar debris disks: - spatial distribution sculpted by planetary perturbations - dust particle size distribution also perturbed - high dust densities (and dust outflows) at younger epochs - planetary architectures can be discerned by detailed study STScI May Symposium, 2005 Malhotra

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