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Radial velocity studies of cool stars

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Radial velocity studies of cool stars. / Jones, H.R.A.; Barnes, J.R.; Tuomi, Mikko; Jenkins, James S.; Anglada-Escude, Guillem.

In: Philosophical transactions of the royal society a-Mathematical physical and engineering sciences, Vol. 372, No. 2014, 20130088, 28.04.2014.

Research output: Contribution to journalLiterature review

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Jones, H.R.A. ; Barnes, J.R. ; Tuomi, Mikko ; Jenkins, James S. ; Anglada-Escude, Guillem. / Radial velocity studies of cool stars. In: Philosophical transactions of the royal society a-Mathematical physical and engineering sciences. 2014 ; Vol. 372, No. 2014.

Bibtex

@article{ce37c7c6b98f4a3f8b9ec3cef12b3874,
title = "Radial velocity studies of cool stars",
abstract = "Our current view of exoplanets is one derived primarily from solar-like stars with a strong focus on understanding our Solar System. Our knowledge about the properties of exoplanets around the dominant stellar population by number, the so called low-mass stars or M dwarfs, is much more cursory. Based on radial velocity discoveries, we find that the semi-major axis distribution of M dwarf planets appears to be broadly similar to those around more massive stars and thus formation and migration processes might be similar to heavier stars. However, we find that the mass of M dwarf planets is relatively much lower than the expected mass dependency based on stellar mass and thus infer that planet formation efficiency around low-mass stars is relatively impaired. We consider techniques to overcome the practical issue of obtaining good quality radial velocity data for M dwarfs despite their faintness and sustained activity and emphasize (i) the wavelength sensitivity of radial velocity signals, (ii) the combination of radial velocity data from different experiments for robust detection of small amplitude signals, and (iii) the selection of targets and radial velocity interpretation of late-type M dwarfs should consider H alpha behaviour.",
keywords = "M dwarfs, radial velocities, exoplanets, EXTRA-SOLAR PLANETS, GIANT PLANET, MASS PLANET, SEARCH, HARPS, DWARF",
author = "H.R.A. Jones and J.R. Barnes and Mikko Tuomi and Jenkins, {James S.} and Guillem Anglada-Escude",
note = "Hugh A. Jones; John Barnes; Mikko Tuomi; James S. Jenkins; and Guillem Anglada-Escude, 'Raial velocity studies of cool stars' Philosophical Transactions of the Royal Society A, Vol. 372 (2014), 20130088, first published 24 March 2014. The version of record is available at doi: 10.1098/rsta.2013.0088. {\circledC} 2014 The Author(s) Published by the Royal Society. All rights reserved.",
year = "2014",
month = "4",
day = "28",
doi = "10.1098/rsta.2013.0088",
language = "English",
volume = "372",
journal = "Philosophical Transactions A: Mathematical, Physical and Engineering Sciences",
issn = "1364-503X",
publisher = "Royal Society of London",
number = "2014",

}

RIS

TY - JOUR

T1 - Radial velocity studies of cool stars

AU - Jones, H.R.A.

AU - Barnes, J.R.

AU - Tuomi, Mikko

AU - Jenkins, James S.

AU - Anglada-Escude, Guillem

N1 - Hugh A. Jones; John Barnes; Mikko Tuomi; James S. Jenkins; and Guillem Anglada-Escude, 'Raial velocity studies of cool stars' Philosophical Transactions of the Royal Society A, Vol. 372 (2014), 20130088, first published 24 March 2014. The version of record is available at doi: 10.1098/rsta.2013.0088. © 2014 The Author(s) Published by the Royal Society. All rights reserved.

PY - 2014/4/28

Y1 - 2014/4/28

N2 - Our current view of exoplanets is one derived primarily from solar-like stars with a strong focus on understanding our Solar System. Our knowledge about the properties of exoplanets around the dominant stellar population by number, the so called low-mass stars or M dwarfs, is much more cursory. Based on radial velocity discoveries, we find that the semi-major axis distribution of M dwarf planets appears to be broadly similar to those around more massive stars and thus formation and migration processes might be similar to heavier stars. However, we find that the mass of M dwarf planets is relatively much lower than the expected mass dependency based on stellar mass and thus infer that planet formation efficiency around low-mass stars is relatively impaired. We consider techniques to overcome the practical issue of obtaining good quality radial velocity data for M dwarfs despite their faintness and sustained activity and emphasize (i) the wavelength sensitivity of radial velocity signals, (ii) the combination of radial velocity data from different experiments for robust detection of small amplitude signals, and (iii) the selection of targets and radial velocity interpretation of late-type M dwarfs should consider H alpha behaviour.

AB - Our current view of exoplanets is one derived primarily from solar-like stars with a strong focus on understanding our Solar System. Our knowledge about the properties of exoplanets around the dominant stellar population by number, the so called low-mass stars or M dwarfs, is much more cursory. Based on radial velocity discoveries, we find that the semi-major axis distribution of M dwarf planets appears to be broadly similar to those around more massive stars and thus formation and migration processes might be similar to heavier stars. However, we find that the mass of M dwarf planets is relatively much lower than the expected mass dependency based on stellar mass and thus infer that planet formation efficiency around low-mass stars is relatively impaired. We consider techniques to overcome the practical issue of obtaining good quality radial velocity data for M dwarfs despite their faintness and sustained activity and emphasize (i) the wavelength sensitivity of radial velocity signals, (ii) the combination of radial velocity data from different experiments for robust detection of small amplitude signals, and (iii) the selection of targets and radial velocity interpretation of late-type M dwarfs should consider H alpha behaviour.

KW - M dwarfs

KW - radial velocities

KW - exoplanets

KW - EXTRA-SOLAR PLANETS

KW - GIANT PLANET

KW - MASS PLANET

KW - SEARCH

KW - HARPS

KW - DWARF

U2 - 10.1098/rsta.2013.0088

DO - 10.1098/rsta.2013.0088

M3 - Literature review

VL - 372

JO - Philosophical Transactions A: Mathematical, Physical and Engineering Sciences

JF - Philosophical Transactions A: Mathematical, Physical and Engineering Sciences

SN - 1364-503X

IS - 2014

M1 - 20130088

ER -