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The Possible Belts for Extrasolar Planetary Systems

Published online by Cambridge University Press:  22 February 2018

Ing-Guey Jiang ,
M. Duncan  and
D.N.C. Lin
Ing-Guey Jiang
Affiliation:
National Central Univ., Taiwan
M. Duncan
Affiliation:
Queen’s University, Canada
D.N.C. Lin
Affiliation:
University of California, USA

Abstract

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More than 100 extrasolar planets have been discovered since the 1990s. Unlike those of the solar system, these planets’ orbital eccentricities cover a huge range from 0 to 0.7. Incidentally, the first Kuiper belt object was discovered in 1992. Thus an interesting and important question will be whether extrasolar planetary systems could have structures like the Kuiper belt or asteroid belt. We investigate the stability of these planetary systems with different orbital eccentricities by similar procedures to Rabl & Dvorak (1988) and Holman & Wiegert (1999). We claim that most extrasolar planetary systems can have their own belts at the outer regions. However, we find that orbits with high eccentricity are very powerful in depletion of these populations.

Resumen

Resumen

Desde la década de los 90 se han descubierto más de 100 planetas extrasolares. A diferencia del Sistema Solar, estos planetas tienen excentricidades en un amplio intervalo, desde 0 hasta 0.7. El primer objetodel Cinturón de Kuiper se descubrió en 1992. Se plantea la cuestión de si los sistemas planetarios extrasolares podrían tener estructuras como el Cinturón de Kuiper o el de los asteroides. Investigamos la estabilidad de estos sistemas para distintas excentricidadescon los métodos de Rabl & Dvorak (1988) y Holman & Wiegert (1999). Sostenemos que la mayor parte de los sistemas planetarios extrasolares pueden tener cinturones en las regiones externas. No obstante, encontramos que las órbitas de gran excentricidad son muy efectivas para destruir estas estructuras.

Keywords

StarsPlanetary Systems
Type
Companions of Very Low Mass
Information
International Astronomical Union Colloquium , Volume 191: The Environment and Evolution of Double and Multiple Stars , August 2004 , pp. 217 - 221
Copyright
Copyright © Instituto de Astronomia – Mexico 2004

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