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Dwarf Plutonian Planets

Dwarf Plutonian Planets. The Story of Eris (A.K.A. the Tentth Planet). Scott S. Sheppard Carnegie Institution of Washington Department of Terrestrial Magnetism. Planets. Dwarf Planets. 1. Spherical. Everything else is a “Small Solar System Body”. 1. Spherical 2. Cleared its Orbit.

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Dwarf Plutonian Planets

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  1. Dwarf Plutonian Planets The Story of Eris (A.K.A. the Tentth Planet) Scott S. Sheppard Carnegie Institution of Washington Department of Terrestrial Magnetism

  2. Planets Dwarf Planets 1. Spherical Everything else is a “Small Solar System Body” 1. Spherical 2. Cleared its Orbit As we know, there are known knowns. There are things we know we know. We also know there are known unknowns. That is to say, we know there are some things we do not know. But there are also unknown unknowns, The ones we don’t know we don’t know. -Donald Rumfield 2002

  3. The Largest Dwarf Planets Gravitational Self Compression > Material Strength Primordial Distribution of Angular Momentum Orcus 1400 km 2003 EL61 1600 km 2005 FY9 1800 km Sheppard 2006

  4. Dwarf Planets

  5. Dynamical Classes in the Outer Solar System Dynamically Disturbed and Collisionally Processed.

  6. Dwarf Planets 2003UB313 2003 EL61 2005 FY9 Pluto

  7. Light Curve for Eris (2003 UB313)

  8. More Eris Light Curve

  9. Phase Function for Eris

  10. Opposition Effect -Shadowing Effects -Coherent Backscattering

  11. Typical small KBO vs. Dwarf Planet Small KBO = 0.16 mags/deg Large Pluto = 0.03 mags/deg Eris (Tholen et al. 1994)

  12. Albedo vs Opp. Effect Belskaya et al. 2003

  13. Phase Angle vs. Size 97% significant Large Small Sheppard et al. 2007

  14. Amplitude vs. Size Small Large Sheppard et al. 2007

  15. Amplitude Vs. Period Sheppard et al. 2004

  16. Cumulative Luminosity Function Large Small Brown et al. 2006

  17. Size vs Albedo Eris EL61 Ixion AW197 Quaoar Huya TD10 Jewitt et al. 2001

  18. Ice Stability in the Solar System Brown 2000

  19. Methane on 2003 UB313 Brown et al. 2005

  20. Brown et al. 2006

  21. Crystalline Water Ice in the Kuiper Belt Jewitt & Luu 2004

  22. L A R G E M I D

  23. Brown et al. 2006

  24. Hubbard 2003 Eris

  25. Eris’ Story Very Eccentric Orbit ~0.45 Currently Near Aphelion ~97AU Very High Albedo 80% Surface is Methane Dominated No Detectable Rotation Shallow Phase Slope Likely has an atmosphere when near perihelion like Pluto. Currently this atmosphere is uniformly frozen on the surface. Effectively, the body is resurfaced every few hundred years. What about 2005 FY9? Large dwarf Plutonian planets are physically and chemically different than The smaller KBOs.

  26. Conclusions

  27. Density vs Size Large Small Sheppard et al. 2007

  28. Tri-Axial Rotational Deformation

  29. What About Eris?

  30. Brown et al. 2006

  31. Barkume et al. 2006

  32. Inclinations

  33. Ice Stability in the Solar System Brown 2000

  34. 2003 VS2 Single Double

  35. Amplitudes Sheppard et al. 2007

  36. Periods 9.5 +- 1 hrs 7.0 +- 1 hrs Sheppard et al. 2007

  37. Period vs Size Sheppard et al. 2007

  38. Light Curve Amplitude and Phase Angle Belskaya et al. 2006

  39. 1. Nonuniform Surface Markings Photometric Range ~ 2 mags B – V ~ 0.1 mags (Millis 1977) -synchronous rotation Iapetus Photometric Range ~ 0.3 mags -atmosphere

  40. 1/2 crit 2. Elongation For large objects (> 200 km) Spherical Gravitational Compression > Material Strength As angular momentum increases an object will go from being a sphere to biaxial to Triaxial elongation from rotational angular momentum P = (3 Pi / G rho) Centripetal acceleration = gravitational acceleration Rotational Triaxial Ellipsoids (Jacobi Ellipsoids) Fast Rotations < 7 hours (Leone et al. 1984)

  41. Axis Ratio from rotational light curve: 0.4 x delta mag a/b = 10 Leone et al. 1984

  42. Varuna Density ~ 1100 kg/m 3 Assume Rotationally distorted Strengthless Rubble Pile Chandrasekhar 1987 Leone et al. 1984 Cosmochemically Plausible Rock Fraction ~ 0.5 Porosity ~ 10 to 20% Jewitt and Sheppard 2002

  43. Asteroid and KBO Limiting Densities Sheppard and Jewitt 2002

  44. 3. Eclipsing Binaries • Probability of eclipse events to our line of sight decreases as the separation increases • Tidal interactions distort close components Photometric Range Max ~ 0.75 mags Photometric Range Max ~ 1.2 mags (Leone et al. 1984) 1999 TC36 (Trujillo and Brown 2002)

  45. Period = 13.7744 hours 2001 QG298 Diameter ~ 250 km Range = 1.1 mags

  46. 2001 QG298 is only the 3rd known minor planet with diameter > 50 km and a photometric range > 1 magnitude Kleopatra 2001 QG298 Hektor

  47. KBO 2001 QG298 Trojan Asteroid 624 Hektor Main Belt Asteroid 216 Kleopatra

  48. CFHT Adaptive Optics images of Kleopatra Merline, Dumas and Menard 1999

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