Is it possible to detect planets around young active G and K dwarfs?
Article
Article Title | Is it possible to detect planets around young active G and K dwarfs? |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Jeffers, S. V. (Author), Barnes, J. R. (Author), Jones, H. R. A. (Author), Reiners, A. (Author), Pinfield, D. J. (Author) and Marsden, S. C. (Author) |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 438 (4), pp. 2717-2731 |
Number of Pages | 15 |
Year | 2014 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/stt1950 |
Web Address (URL) | https://academic.oup.com/mnras/article/438/4/2717/1083966 |
Abstract | Theoretical predictions suggest that the distribution of planets in very young stars could be very different to that typically observed in Gyr old systems that are the current focus of radial velocity surveys. However, the detection of planets around young stars is hampered by the increased stellar activity associated with young stars, the signatures of which can bias the detection of planets. In this paper, we place realistic limitations on the possibilities for detecting planets around young active G and K dwarfs. The models of stellar activity based on tomographic imaging of the G dwarf HD 141943 and the K1 dwarf AB Dor also include contributions from plage and many small random starspots. Our results show that the increased stellar activity levels present on young solar-type stars strongly impacts the detection of Earth-mass and Jupiter-mass planets and that the degree of activity jitter is directly correlated with stellar v sin i. We also show that for G and K dwarfs, the distribution of activity in individual stars is more important than the differences in induced radial velocities as a function of spectral type. We conclude that Jupiter-mass planets can be detected close-in around fast-rotating young active stars, Neptune-mass planets around moderate rotators and that Super-Earths are only detectable around very slowly rotating stars. The effects of an increase in stellar activity jitter by observing younger stars can be compensated for by extending the observational base-line to at least 100 epochs. |
Keywords | magnetic fields; planetary systems; stars; late-type |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
519999. Other physical sciences not elsewhere classified | |
510903. Mesospheric, thermospheric, ionospheric and magnetospheric physics | |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | Georg August University of Gottingen, Germany |
University of Hertfordshire, United Kingdom | |
Computational Engineering and Science Research Centre | |
Institution of Origin | University of Southern Queensland |
https://research.usq.edu.au/item/q2780/is-it-possible-to-detect-planets-around-young-active-g-and-k-dwarfs
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