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Indicator of Exo-Solar Planet(s) in the Circumstellar Disk Around β Pictoris

Published online by Cambridge University Press:  26 May 2016

Nick Gorkavyi ,
Sara Heap ,
Leonid Ozernoy ,
Tanya Taidakova  and
John Mather
Nick Gorkavyi
Affiliation:
NRC/NAS; Code 685, NASA/GSFC, Greenbelt, MD 20771, USA
Sara Heap
Affiliation:
Code 681, NASA/GSFC, Greenbelt, MD 20771, USA
Leonid Ozernoy
Affiliation:
5C3, George Mason University, Fairfax, VA 22030-4444, USA
Tanya Taidakova
Affiliation:
Computational Consulting Service, MD 20740, USA
John Mather
Affiliation:
Code 685, NASA/GSFC, Greenbelt, MD 20771, USA

Abstract

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Our efficient numerical approach has been applied to modeling the asymmetric circumstellar dust disk around β Pictoris as observed with the HST/STIS. We present a new model on the origin of the warping of the β Pic disk. We suggest that the observed warp is formed by the gravitational influence of a planet with a mass of about 10 masses of Earth, at a distance of 70 AU, and a small inclination (∽ 2.5°) of the planetary orbit to the main dust disk. Results of our modeling are compared with the STIS observations.

Type
Part IV: Protoplanetary and β Pic disks
Information
Symposium - International Astronomical Union , Volume 202: Planetary Systems in the Universe – Observation, Formation and Evolution , 2004 , pp. 331 - 334
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

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