Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-09T13:06:29.942Z Has data issue: false hasContentIssue false
  • English
  • Français

Thermal evolution and magnetism of terrestrial planets.

Published online by Cambridge University Press:  01 October 2007

Chihiro Tachinami ,
Hiroki Senshu  and
Shigeru Ida
Chihiro Tachinami
Affiliation:
Department of Earth and Planetary Sciences, Tokyo Institute of Technology2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan email: [email protected]
Hiroki Senshu
Affiliation:
Department of Earth and Planetary Sciences, Tokyo Institute of Technology2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan email: [email protected]
Shigeru Ida
Affiliation:
Department of Earth and Planetary Sciences, Tokyo Institute of Technology2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, Japan email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We evaluate a numerical model on the thermal evolution of terrestrial planets to estimate life-time of planetary intrinsic magnetic field for various mass planets. In this model, we take into account the pressure-dependency of density profile of the planet by using Birch-Murnaghun equation of state, and simulate thermal evolution of the planet by means of mixing length theory. According to our numerical results, the planetary mass must be between 0.1 and 1.4 Earth mass to sustain the intrinsic magnetic field for 4.5Gyr. If existence of intrinsic magnetic field were a key factor to make the planet habitable, the mass range above indicates that super-Earths would not be habitable.

Keywords

Thermal evolutionterrestrial planethabitability
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S249: Exoplanets: Detection, Formation and Dynamics , October 2007 , pp. 159 - 162
Copyright
Copyright © International Astronomical Union 2008

References

Alfé, D., Price, G. D., & Gillan, M. J. 2002, Phys. Rev. B 65 (16), 165118CrossRefGoogle Scholar
Ida, S. & Lin, D. N. C. 2004, ApJ, 604, 388CrossRefGoogle Scholar
Ida, S. & Lin, D. N. C. 2004, ApJ, 616, 567CrossRefGoogle Scholar
Mayer, M. & Queloz, D. 1995, Nature, 378, 355CrossRefGoogle Scholar
Sasaki, S., & Nakazawa, K. 1986, J, Geophys. Res. 91, 9231CrossRefGoogle Scholar
Stevenson, D. J., Spohn, T., & Schubert, G. 1983, Icarus 54 (3), 466CrossRefGoogle Scholar
Stixrude, L., & Lithgow-Bertelloni, C. 2005, Geophys. J. Int. 162, 610CrossRefGoogle Scholar
Valencia, D., OConnell, R. J., & Sasselov, D. 2006, Icarus 181, 545CrossRefGoogle Scholar
Yukutake, T. 2000, Phys. Earth Planet. Inter. 121, 103CrossRefGoogle Scholar