EPJ Web of Conferences
Volume 47, 2013Hot Planets and Cool Stars
|Number of page(s)||6|
|Section||Characterization of Host Stars|
|Published online||25 April 2013|
Realistic limitations of detecting planets around young active stars
1 Institut fur Astrophysik, Georg-August Universitat Goettingen, Friedrich-Hund-Platz 1, 37077 Goettingen, Germany
2 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Herts AL10 9AB, UK
a e-mail: firstname.lastname@example.org
Current planet hunting methods using the radial velocity method are limited to observing middle-aged main-sequence stars where the signatures of stellar activity are much less than on young stars that have just arrived on the main-sequence. In this work we apply our knowledge from the surface imaging of these young stars to place realistic limitations on the possibility of detecting orbiting planets. In general we find that the magnitude of the stellar jitter is directly proportional to the stellar vsini. For G and K dwarfs, we find that it is possible, for models with high stellar activity and low stellar vsini, to be able to detect a 1 MJupiter mass planet within 50 epochs of observations and for the M dwarfs it is possible to detect a habitable zone Earth-like planet in 10s of observational epochs.
© Owned by the authors, published by EDP Sciences, 2013
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 2.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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