Activity-induced radial velocity variation of M dwarf stars
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Activity-induced radial velocity variation of M dwarf stars. / Andersen, Jan Marie; Korhonen, Heidi Helena.
In: Proceedings of the International Astronomical Union, Vol. 8, No. S293, 08.2012, p. 197-200.Research output: Contribution to journal › Conference article › Research › peer-review
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TY - GEN
T1 - Activity-induced radial velocity variation of M dwarf stars
AU - Andersen, Jan Marie
AU - Korhonen, Heidi Helena
N1 - Conference code: 293
PY - 2012/8
Y1 - 2012/8
N2 - 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?
AB - 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?
KW - atmospheres
KW - low-mass
KW - planetary systems
KW - rotation
KW - spots
KW - stars: activity
KW - techniques: radial velocities
UR - http://www.scopus.com/inward/record.url?scp=84899875011&partnerID=8YFLogxK
U2 - 10.1017/S1743921313012829
DO - 10.1017/S1743921313012829
M3 - Conference article
AN - SCOPUS:84899875011
VL - 8
SP - 197
EP - 200
JO - Proceedings of the International Astronomical Union
JF - Proceedings of the International Astronomical Union
SN - 1743-9213
IS - S293
Y2 - 27 August 2012 through 31 August 2012
ER -
ID: 183471442