Volume 633, January 2020
|Number of page(s)||9|
|Section||Stellar structure and evolution|
|Published online||23 January 2020|
Differences in radio emission from similar M dwarfs in the binary system Ross 867-8
Leiden Observatory, Leiden University, PO Box 9513, 2300 Leiden, The Netherlands
2 Joint Institute for VLBI ERIC (JIVE), Oude Hoogeveensedijk 4, 7991 Dwingeloo, The Netherlands
3 International Centre for Radio Astronomy Research – Curtin University, GPO Box U1987, 6845 Perth, Australia
4 ASTRON, Netherlands Institute for Radio Astronomy, Oude Hoogeveensedijk 4, 7991 Dwingeloo, The Netherlands
5 National Radio Astronomy Observatory, 520 Edgemont Rd., Charlottesville, VA 22903, USA
6 National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801-0387, USA
Accepted: 17 November 2019
Serendipitously, we rediscovered radio emission from the binary system Ross 867 (M4.5V) and Ross 868 (M3.5V) while inspecting archival Giant Metrewave Radio Telescope (GMRT) observations. The binary system consists of two M-dwarf stars that share common characteristics such as spectral type, astrometric parameters, age, and emission at infrared, optical, and X-ray frequencies. The GMRT data at 610 MHz taken on July 2011 shows that the radio emission from Ross 867 is polarized and highly variable on hour timescales with a peak flux of 10.4 ± 0.7 mJy beam−1. Additionally, after reviewing archival data from several observatories (VLA, GMRT, JVLA, and LOFAR), we confirm that although the two stars are likely coeval, only Ross 867 was detected, while Ross 868 remains undetected at radio wavelengths. As the stars have a large orbital separation, this binary stellar system provides a coeval laboratory to examine and constrain the stellar properties linked to radio activity in M dwarfs. We speculate that the observed difference in radio activity between the dwarfs could be due to vastly different magnetic field topologies or that Ross 867 has an intrinsically different dynamo.
Key words: stars: flare / binaries: general / radiation mechanisms: non-thermal / stars: individual: Ross 867 / stars: individual: Ross 868 / radio continuum: stars
© ESO 2020
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