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Activity-Induced Radial Velocity Variation of M Dwarf Stars

Published online by Cambridge University Press:  29 April 2014

Jan Marie Andersen  and
Heidi Korhonen
Jan Marie Andersen
Affiliation:
Department of Astronomy, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA, email: [email protected] Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, ster Voldgade 5-7, DK-1350, Copenhagen, Denmark
Heidi Korhonen
Affiliation:
Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, ster Voldgade 5-7, DK-1350, Copenhagen, Denmark Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark
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Abstract

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Stellar magnetic activity manifests itself in a variety of ways including starspots–cool, dark regions on the stellar surface. Starspots can cause variations (‘jitter’) in spectral line-profiles which can mimic the radial velocity (RV) variations caused by an orbiting planet, or create RV noise that can drown out a planetary signature. Cool, low-mass M dwarf stars can be highly active, which can make detection of potentially habitable planets around these stars difficult. We investigate radial velocity variations caused by different activity (spot) patterns on M dwarf stars in order to determine the limits of detectability for small planets orbiting active M dwarfs. We report on our progress toward the aim of answering the following questions: What types of spot patterns are realistic for M dwarf stars? What effect will spots have on M dwarf RV measurements? Can jitter from M dwarf spots mimic planetary signals? What is the ideal observing wavelength to reduce M dwarf jitter?

Keywords

stars: activityatmospheresplanetary systemsrotationspotslow-masstechniques: radial velocities
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 197 - 200
Copyright
Copyright © International Astronomical Union 2014 

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