A solar-like magnetic cycle on the mature K-dwarf 61 Cygni A (HD 201091)

Boro Saikia, S. and Jeffers, S. V. and Morin, J. and Petit, P. and Folsom, C. P. and Marsden, S. C. and Donati, J.-F. and Cameron, R. and Hall, J. C. and Perdelwitz, V. and Reiners, A. and Vidotto, A. A. (2016) A solar-like magnetic cycle on the mature K-dwarf 61 Cygni A (HD 201091). Astronomy and Astrophysics, 594 (A29). ISSN 000-46361

Text (Published Version)
Boro Saikia 2016 A&A 594 A29.pdf

Download (2240Kb) | Preview


Context. The long-term monitoring of magnetic cycles in cool stars is a key diagnostic in understanding how dynamo generation and amplification of magnetic fields occur in stars similar in structure to the Sun.
Aims. We investigated the temporal evolution of a possible magnetic cycle of 61 Cyg A. The magnetic cycle is determined from 61 Cyg A’s large-scale field over its activity cycle using spectropolarimetric observations and compared to the solar large-scale magnetic field.
Methods. We used the tomographic technique of Zeeman Doppler imaging (ZDI) to reconstruct the large-scale magnetic geometry of 61 Cyg A over multiple observational epochs spread over a time span of nine years. We investigated the time evolution of the different components of the large-scale field and compared it with the evolution of the star’s chromospheric activity by measuring the flux in three different chromospheric indicators: Ca II H&K, Hα and Ca II infrared triplet lines. We also compared our results with the star’s coronal activity using XMM-Newton observations.
Results. The large-scale magnetic geometry of 61 Cyg A exhibits polarity reversals in both poloidal and toroidal field components, in phase with its chromospheric activity cycle. We also detect weak solar-like differential rotation with a shear level similar to that of the Sun. During our observational time span of nine years, 61 Cyg A exhibits solar- like variations in its large-scale field geometry as it evolves from minimum activity to maximum activity and vice versa. During its activity minimum in epoch 2007.59, ZDI reconstructs a simple dipolar geometry which becomes more complex when it approaches activity maximum in epoch 2010.55. The radial field flips polarity and reverts back to a simple geometry in epoch 2013.61. The field is strongly dipolar and the evolution of the dipole component of the field is reminiscent of solar behaviour. The polarity reversal of the large-scale field indicates a magnetic cycle that is in phase with the chromospheric and coronal cycle.

Statistics for USQ ePrint 30364
Statistics for this ePrint Item
Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: Access to Published version in accordance with the copyright policy of the publisher.
Faculty / Department / School: Current - Faculty of Health, Engineering and Sciences - School of Agricultural, Computational and Environmental Sciences
Date Deposited: 08 Mar 2017 05:05
Last Modified: 13 Feb 2019 23:53
Uncontrolled Keywords: dynamo, stars: activity, stars: chromospheres, stars: magnetic field, stars: solar-type
Fields of Research : 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems
Socio-Economic Objective: E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences
Identification Number or DOI: 10.1051/0004-6361/201628262
URI: http://eprints.usq.edu.au/id/eprint/30364

Actions (login required)

View Item Archive Repository Staff Only