2014
DOI: 10.1051/0004-6361/201322136
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Exploring the magnetic field complexity in M dwarfs at the boundary to full convection

Abstract: Context. Magnetic fields play a pivotal role in the formation and evolution of low-mass stars, but the dynamo mechanisms generating these fields are poorly understood. Measuring cool star magnetism is a complicated task because of the complexity of cool star spectra and the subtle signatures of magnetic fields. Aims. Based on detailed spectral synthesis, we carry out quantitative measurements of the strength and complexity of surface magnetic fields in the four well-known M dwarfs GJ 388, GJ 729, GJ 285, and G… Show more

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Cited by 53 publications
(59 citation statements)
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“…The HARPS instrument and its data reduction software has demonstrated long-term 1 m/s precision since its installation in 2003 (Mayor et al 2003). Each of the points to be tested are evaluated for (1) a stable and inactive M dwarf (Barnard's star), (2) a G4 dwarf with strong correlations between FWHM and RVs (ζ (West et al 2015), an average magnetic field of the order of 3-4 kG, and local field strengths up to 7 kG (Shulyak et al 2014). We obtained 45 CARMENES VIS observations spanning 480 days (from 2016-01-08 to 2017-05-01).…”
Section: Resultsmentioning
confidence: 99%
“…The HARPS instrument and its data reduction software has demonstrated long-term 1 m/s precision since its installation in 2003 (Mayor et al 2003). Each of the points to be tested are evaluated for (1) a stable and inactive M dwarf (Barnard's star), (2) a G4 dwarf with strong correlations between FWHM and RVs (ζ (West et al 2015), an average magnetic field of the order of 3-4 kG, and local field strengths up to 7 kG (Shulyak et al 2014). We obtained 45 CARMENES VIS observations spanning 480 days (from 2016-01-08 to 2017-05-01).…”
Section: Resultsmentioning
confidence: 99%
“…These lines are magnetically sensitive, and their Zeeman broadening can be exploited in cool stars to measure the magnetic field strength (cf. Johns-Krull & Valenti 1996;Shulyak et al 2014), particularly in M dwarfs. These lines are among the sparse atomic transitions in the NIR with accurate available data, whereas magnetically sensitive molecular lines in the NIR (e.g.…”
Section: Discussionmentioning
confidence: 99%
“…Previous studies applied this diagnostic method to atomic and molecular lines in the Stokes I spectra of many low-mass stars and brown dwarfs, detecting fields with typical strengths of 2-4 kG (Johns-Krull & Valenti 1996;Reiners & Basri 2007;Shulyak et al 2014). In a recent study by Shulyak et al (in prep., see also summary in Kochukhov et al 2017) magnetic fields of up to 6.4 kG were found in several active, rapidly rotating (P rot = 0.4-0.8 d) M4-6 dwarfs.…”
Section: Total Magnetic Fluxmentioning
confidence: 99%