Structure and evolution of large kuiper belt objects and dwarf planets
This presentation is the property of its rightful owner.
Sponsored Links
1 / 15

Structure and Evolution of Large Kuiper Belt Objects and Dwarf Planets PowerPoint PPT Presentation


  • 46 Views
  • Uploaded on
  • Presentation posted in: General

Structure and Evolution of Large Kuiper Belt Objects and Dwarf Planets. William B. McKinnon 1 , S. Alan Stern 2 , E. Asphaug 3 1 Dept. EPSC and McDonnell Center for the Space Sci.,Washington Univ., St. Louis, MO USA 2 Southwest Research Inst., Boulder, CO USA 3 UC Santa Cruz, CA USA

Download Presentation

Structure and Evolution of Large Kuiper Belt Objects and Dwarf Planets

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Presentation Transcript


Structure and evolution of large kuiper belt objects and dwarf planets

Structure and Evolution of Large Kuiper Belt Objects and Dwarf Planets

William B. McKinnon1, S. Alan Stern2, E. Asphaug3

1Dept. EPSC and McDonnell Center for the Space Sci.,Washington Univ., St. Louis, MO USA

2Southwest Research Inst., Boulder, CO USA

3UC Santa Cruz, CA USA

TNO 2006, Catania, 5 July 2006


Structure and evolution of large kuiper belt objects and dwarf planets

r min

r max

Stern, McKinnon & Lunine 1997

Jewitt & Sheppard 2002

Axial ratio ≥ 1.5:1:0.7 –>

1090 kg/m3 ≤ r ≤ 1270 kg/m3

The nature of the beast…


Structure and evolution of large kuiper belt objects and dwarf planets

r min

r max

  • ≤ 1270 kg/m3

    740

    530

    375

Sheppard & Jewitt 2002


Structure and evolution of large kuiper belt objects and dwarf planets

Stansberry et al. 2006

1999 TC36

1998 SM165 Spencer et al., this meeting

Dprimary ≈ 250–330 km; r = 0.35 –0.85 g cm-3

porosity

vs.

solid density


Porosity

R

r

  • Real geological rubble, regoliths have f ≈ 0.4

  • Cometary porosities (f ≥ 0.5) are possible ... for comets!

Carrier et al. 1991

Porosity

  • Pressures in large KBOs (r ≥ 100 km) non-negigible:

  • Pc = 30 MPa for spherical Varuna of ice density

  • Real geological rubble, regoliths have f ≈ 0.4

  • Cometary porosities (f ≥ 0.5) are possible ... for comets!


Structure and evolution of large kuiper belt objects and dwarf planets

Phydro

Durham, McKinnon & Stern, 2005


Structure and evolution of large kuiper belt objects and dwarf planets

Ice Compaction

DMS2005


Structure and evolution of large kuiper belt objects and dwarf planets

EOS Comparison


Structure and evolution of large kuiper belt objects and dwarf planets

ACM 2005


Structure and evolution of large kuiper belt objects and dwarf planets

ACM 2005


Structure and evolution of large kuiper belt objects and dwarf planets

Radius (km)

rrock = 2.63 g cm-3

ACM 2005


Structure and evolution of large kuiper belt objects and dwarf planets

Phoebe Thermal Evolution


Structure and evolution of large kuiper belt objects and dwarf planets

2003 EL61

1999 TC36

Brown, Rabinowitz and coworkers

Yes, Gerard,

there is a

Santa KBO…


Structure and evolution of large kuiper belt objects and dwarf planets

1999 TC36


Structure and evolution of large kuiper belt objects and dwarf planets

Discussion

  • Range of believable densities outside the Pluto/Triton + porosity paradigm

  • Moderate to large KBOs have a range of densities/compositions-- classes?

  • Asteroid compositional classes – S, M, C, P, D, etc due to different factors:

Distance from Sun --> ice content

Internal differentiation and collisional evolution

  • Large ice-rich and rock-rich KBOs require strong collisional evolution

  • Pluto and EL61 imply different collisional environments

  • More constraints on formation models (Viva Niza!)

  • Much more to come on internal evolution of big KBOs!


  • Login