Download Interior of exoplanetes

Survey
yes no Was this document useful for you?
   Thank you for your participation!

* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project

Document related concepts

Neutron magnetic moment wikipedia , lookup

Superconducting magnet wikipedia , lookup

Geomagnetic storm wikipedia , lookup

Giant magnetoresistance wikipedia , lookup

Magnetic monopole wikipedia , lookup

Magnetometer wikipedia , lookup

Magnetosphere of Jupiter wikipedia , lookup

Magnetotactic bacteria wikipedia , lookup

Magnet wikipedia , lookup

Electromagnetic field wikipedia , lookup

Force between magnets wikipedia , lookup

Magnetosphere of Saturn wikipedia , lookup

Magnetism wikipedia , lookup

Multiferroics wikipedia , lookup

Ferrofluid wikipedia , lookup

Aurora wikipedia , lookup

Earth's magnetic field wikipedia , lookup

Magnetoreception wikipedia , lookup

Magnetochemistry wikipedia , lookup

Magnetohydrodynamics wikipedia , lookup

Magnetotellurics wikipedia , lookup

Electromagnet wikipedia , lookup

Ferromagnetism wikipedia , lookup

History of geomagnetism wikipedia , lookup

Transcript
Interior of exoplanetes
Doris Breuer, DLR Institute of Planetary Research
Basic parameters for the interior structure
• 
Radius and mass
à density (constraint on average composition)
Any other information (e.g. differentiated in a core and
mantle, sizes of the reservoirs) base on assumptions
Stevenson, 2004
Page 4 > Objectives and Accomplishments > Prof. Dr.Tilman Spohn
Interior structure of Exoplanets
~10%
(Wagner et al., Icarus, 2011)
~5%
Simulation of Exoplanets: Needed Accuracy
• 
Assume an Earth-size exoplanet (at any age) is found – can we assess how earthlike the interior structure is?
• 
Error in core-mantle fraction influenced by accuracy of radius determination:
εcmf = (14.08*εr)0.7745
Mantle
Mantle
What are the implications for mantle dynamics and the atmosphere?
Core
Core
Interior structure and atmosphere
Courtesy of L. Noack
• 
• 
• 
• 
Influence on outgassing: A smaller mantle would be expected to have a smaller
amount of volatiles → less-dense atmosphere
Influence on mantle temperature: Mantle may cool much faster (smaller amount of
radioactive heat sources) → outgassing may stop sooner
Influence on plate tectonics: Small mantle develops (if at all) small-scale convection
→ bad for plate tectonics
Influence on magnetic field: less easy to maintain high heat flux at the core-mantle
boundary → bad for magnetic fields
Propensity for Plate Tectonics
Implications for Habitability
How it works on Earth:
Space
Erosion
Magnetosphere
Shielding
Biosphere
Hydrosphere
Atmosphere
Crust
Subduction
Outgassing
Mantle
Cooling
Core
Dynamo
Implications for Habitability
No magnetic field
-> bad for life
Space
Erosion
Magnetosphere
Shielding
Biosphere
Hydrosphere
Atmosphere?
Crust
Subduction
Outgassing
Mantle
Cooling
Core
Dynamo
Implications for Habitability
No magnetic field
-> bad for life
Space
Erosion
No plate tectonics
-> bad for magnetic field
-> bad for life
Magnetosphere
Shielding
Biosphere
Hydrosphere
Atmosphere?
Crust
Subduction
Outgassing
Mantle
Cooling
Core
Dynamo
Implications for Habitability
No magnetic field
-> bad for life
Space
Erosion
No plate tectonics
-> bad for magnetic field
-> bad for life
Magnetosphere
Shielding
Biosphere
Hydrosphere
Atmosphere?
Crust
In addition: no outgassing
-> bad for life
Outgassing
Mantle
Cooling
Core
Dynamo?