EDP Sciences
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sum" ty =cuntendihr eihr>>>>>"> Sub="3i>Sub="3i>atoear">v> > N 2014rhref=c/thdihrhr odeantddihrhr odemg srtddihrhc/thdihrh odeantddihrh odemospheres"> v>v>ain" clas < /a> Transirnal w//EN">>ain" clasleor).u-m ain" clas αof Proxima Centauri"> >>>>>>>-dkeyn=""/lystoclas htmk" tit-dkeyn=-1no-remeurl=t/authenticate/?or1051/0004-6361/20162882tent=">llins"> Subscrup>1an>up>, /lystoclas htmk" tit-dkeyn=-2no-remeurl=t/authenticate/?or1051/0004-6361/20162882tent="> Jones"> Subscrup>1an>up>er th/lystoclas htmk" tit-dkeyn=-3no-remeurl=t/authenticate/?or1051/0004-6361/20162882tent=">llins> Subscrup>2an>up> 1an>up>e of Hertfordshire, College Lane, Hatfield, Herts, AL110 9AB, UK"> 2an>up> of Physical Sciences, The Open University, Walton Halll, Milton Keyynes, MK7 6AA, UUK"> ReceWald: an>Subs29 April Actiptld: an>Subs2 Febru ty /a> /tation_fa> p>gate retrieval of the stellar rotation signal for Proxima Centauri. We make use of high-resolution spectra taken with UVES and HARPS of Proxima Centauri over a 13-yr period as well as photometric observations of Proxima Centauri from ASAS and HST. We measure the H<i>crysto16 whitsi so-mang" αan>Subs width and H<i>crysto16 whitsi so-mang" αan>Subs wness and kurtosis and introduce a method that investigates the symmetry of the line, the peak ratio, which appears to return better results than the other measurements. Our investigations return a most significant period of 82.6 ± 0.1 daycrysto16 whitsi so-mang" ±an>Subs confirming earlier photometric results and ruling out a more recent result of 116.6 days which we conclude to be an alias induced by the specific HARPS observation times. We conclude that whilst spectroscopic H<i>crysto16 whitsi so-mang" αan>Subs ts can be used for period recovery, in the case of Proxima Centauri the available photometric measurements are more reliable. We make 2D models of Proxima Centauri to generate simulated H<i>crysto16 whitsi so-mang" αan>Substhat reasonable distributions of plage and chromospheric features are able to reproduce the equivalent width variations in observed data and recover the rotation period, including after the addition of simulated noise and flares. However the 2D models used fail to generate the observed variety of line shapes measured by the peak ratio. We conclude that only 3D models which incorporate vertical motions in the chromosphere can achieve this."> n_articspt">kent="

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