Hostname: page-component-78c5997874-s2hrs Total loading time: 0 Render date: 2024-11-19T04:34:32.311Z Has data issue: false hasContentIssue false
  • English
  • Français

Chemical clues on the formation of planetary systems

Published online by Cambridge University Press:  10 November 2011

Elisa Delgado Mena ,
Garik Israelian ,
Jonay I. González Hernández ,
Jade C. Bond ,
Nuno C. Santos ,
Stéphane Udry  and
Michel Mayor
Elisa Delgado Mena
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: [email protected] Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain.
Garik Israelian
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: [email protected] Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain.
Jonay I. González Hernández
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain. email: [email protected] Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain.
Jade C. Bond
Affiliation:
Planetary Science Institute, 1700 E. Fort Lowell, Tucson, AZ 85719, USA.
Nuno C. Santos
Affiliation:
Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal. Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Portugal.
Stéphane Udry
Affiliation:
Observatoire de Genève, 51 ch. des Maillettes, CH-1290 Sauverny, Switzerland.
Michel Mayor
Affiliation:
Observatoire de Genève, 51 ch. des Maillettes, CH-1290 Sauverny, Switzerland.
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.

Theoretical studies suggest that C/O and Mg/Si are the most important elemental ratios in determining the mineralogy of terrestrial planets. The C/O ratio controls the distribution of Si among carbide and oxide species, while Mg/Si gives information about the silicate mineralogy. We find mineralogical ratios quite different from those of the Sun, showing that there is a wide variety of planetary systems which are not similar to Solar System. Many of planetary host stars present a Mg/Si value lower than 1, so their planets will have a high Si content to form species such as MgSiO3. This type of composition can have important implications for planetary processes like plate tectonics, atmospheric composition or volcanism. Moreover, the information given by these ratios can guide us in the search of stars more probable to form terrestrial planets.

Keywords

stars: abundancesstars: atmospheresstars: fundamental parametersplanetary systemsplanetary systems: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S276: The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution , October 2010 , pp. 25 - 29
Copyright
Copyright © International Astronomical Union 2011

References

Beirão, P., Santos, N. C., Israelian, G., & Mayor, M. 2005, A&A, 438, 251Google Scholar
Bodaghee, A., Santos, N. C., Israelian, G., & Mayor, M. 2003, A&A, 404, 715Google Scholar
Bond, J. C., Tinney, C. G., Butler, R. P., Jones, H. R. A., Marcy, G. W., Penny, A. J., & Carter, B. D. 2006, MNRAS, 370, 163CrossRefGoogle Scholar
Bond, J. C., et al. 2008, ApJ, 682, 1234CrossRefGoogle Scholar
Bond, J. C., Lauretta, D. S., & O'Brien, D. P. 2010a, Icarus, 205, 321CrossRefGoogle Scholar
Bond, J. C., O'Brien, D. P., & Lauretta, D. S. 2010b, ApJ, 715, 1050CrossRefGoogle Scholar
Boss, A. P. 1997, Science, 276, 1836CrossRefGoogle Scholar
Boss, A. P. 2002, ApJ, 567, 149CrossRefGoogle Scholar
Cai, K., Durisen, R. H., Michael, S., Boley, A. C., Mejía, A. C., Pickett, M. K., & D'Alessio, P. 2006, ApJL, 636, L149CrossRefGoogle Scholar
Gilli, G., Israelian, G., Ecuvillon, A., Santos, N. C., & Mayor, M. 2006, A&A, 449, 723Google Scholar
Gonzalez, G. 1998, A&A, 334, 221Google Scholar
Gonzalez, G., Laws, C., Tyagi, S., & Reddy, B. E. 2001, AJ, 121, 432CrossRefGoogle Scholar
Gonzalez, G. & Laws, C. 2007, MNRAS, 378, 1141CrossRefGoogle Scholar
González Hernández, J. I., Israelian, G., Santos, N. C., Sousa, S. G., Delgado Mena, E., Neves, V., & Udry, S. 2010, ApJ, 720, 1592CrossRefGoogle Scholar
Fischer, D. A. & Valenti, J. 2005, AJ, 622, 1102CrossRefGoogle Scholar
Kurucz, R. L. 1993, CD-ROMs, ATLAS9 Stellar Atmospheres Programs (Cambridge: Smithsonian Astrophys. Obs.)Google Scholar
Mayor, M. & Queloz, D., et al. 2003, The Messenger, 114, 20Google Scholar
Neves, V., Santos, N. C., Sousa, S. G., Correia, A. C. M., & Israelian, G. 2009, A&A, 497, 563Google Scholar
Pollack, J. B., Hubickyj, O., Bodenheimer, P., Lissauer, J. J., Podolak, M., & Greenzweig, Y. 1996, Icarus, 124, 62CrossRefGoogle Scholar
Sadakane, K., Ohkubo, M., Takeda, Y., Sato, B., Kambe, E., & Aoki, W. 2002, PASJ, 54, 911CrossRefGoogle Scholar
Santos, N. C., Israelian, G., & Mayor, M. 2000, A&A, 363, 228Google Scholar
Santos, N. C., Israelian, G., & Mayor, M. 2001, A&A, 373, 1019Google Scholar
Santos, N. C., Israelian, G., & Mayor, M. 2004, A&A, 415, 1153Google Scholar
Santos, N. C., Israelian, G., Mayor, M., Bento, J. P., Almeida, P. C., Sousa, S. G., & Ecuvillon, A., 2005, A&A, 437, 1127Google Scholar
Sousa, S. G., Santos, N. C., Israelian, G., Mayor, M., & Monteiro, M. J. P. F. G. 2007, A&A, 469, 783Google Scholar
Sousa, S. G., Santos, N. C., Mayor, M., Udry, S., Casagrande, L., Israelian, G., Pepe, F., Queloz, D., & Monteiro, M. J. P. F. G. 2008, A&A, 487, 373Google Scholar
Sneden, C. 1973 Ph.D Thesis, University of Texas.Google Scholar
Takeda, Y. 2007, PASJ, 59, 335CrossRefGoogle Scholar