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Strong dipole magnetic fields in fast rotating fully convective stars
Georg August Univ, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany..
Georg August Univ, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany..
Georg August Univ, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany..
Canada France Hawaii Telescope Corp, 65-1238 Mamalahoa Highway, Kamuela, HI 96743 USA.;Univ Montreal, Dept Phys, Inst Rech Exoplanetes, CP 6128, Montreal, PQ H3C 3J7, Canada..
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2017 (English)In: NATURE ASTRONOMY, ISSN 2397-3366, Vol. 1, no 8Article in journal (Refereed) Published
Abstract [en]

M dwarfs are the most numerous stars in our Galaxy, with masses between approximately 0.5 and 0.1 solar masses. Many of them show surface activity qualitatively similar to our Sun and generate flares, high X-ray fluxes and largescale magnetic fields(1-4). Such activity is driven by a dynamo powered by the convective motions in their interiors(2),(5-8). Understanding properties of stellar magnetic fields in these stars finds a broad application in astrophysics, including theory of stellar dynamos and environment conditions around planets that may be orbiting these stars. Most stars with convective envelopes follow a rotation-activity relationship where various activity indicators saturate in stars with rotation periods shorter than a few days(2,6,8). The activity gradually declines with rotation rate in stars rotating more slowly. It is thought that, due to a tight empirical correlation between X-ray radiance and magnetic flux(9), the stellar magnetic fields will also saturate, to values around 4kG (ref. (10)). Here we report the detection of magnetic fields above the presumed saturation limit in four fully convective M dwarfs. By combining results from spectroscopic and polarimetric studies, we explain our findings in terms of bistable dynamo models(11,12):stars with the strongest magnetic fields are those in a dipole dynamo state, whereas stars in a multipole state cannot generate fields stronger than about 4kG. Our study provides observational evidence that the dynamo in fully convective M dwarfs generates magnetic fields that can differ not only in the geometry of their large-scale component, but also in the total magnetic energy.

Place, publisher, year, edition, pages
2017. Vol. 1, no 8
National Category
Astronomy, Astrophysics and Cosmology
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URN: urn:nbn:se:uu:diva-342612DOI: 10.1038/s41550-017-0184ISI: 000415185700008OAI: oai:DiVA.org:uu-342612DiVA, id: diva2:1185061
Funder
Swedish Research CouncilSwedish National Space BoardAvailable from: 2018-02-23 Created: 2018-02-23 Last updated: 2018-02-23Bibliographically approved

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Kochukhov, Oleg

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