Differential rotation on both components of the pre‐main‐sequence binary system HD 155555
Identifieur interne : 002F49 ( Istex/Curation ); précédent : 002F48; suivant : 002F50Differential rotation on both components of the pre‐main‐sequence binary system HD 155555
Auteurs : N. J. Dunstone [Royaume-Uni] ; G. A. J. Hussain [Allemagne] ; A. Collier Cameron ; S. C. Marsden [Australie] ; M. Jardine ; J. R. Barnes ; J. C. Ramirez Velez [France] ; J. Donati [France]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2008-07-11.
English descriptors
- KwdEn :
- Binary, Binary orbit, Binary system, Binary systems, Brightness maps, Cameron, Characteristic signature, Collier, Collier cameron, Complete phase coverage, Convection, Convection zone, Convection zone depth, Convection zone depths, Convection zones, Convective, Convective envelope, Crosscorrelation technique, Data sets, Differential, Differential rotation, Differential rotation curves, Differential rotation measurement, Differential rotation measurements, Differential rotation parameters, Differential rotation rate, Differential rotation rates, Differential rotation strength, Donati, Donati collier cameron, Donati rees, Donati semel, Doppler, Doppler imaging, Doppler imaging process, Dots code, Dunstone, Eld, Equatorial rotation rate, Evolutionary models, Evolutionary stage, Fractional radius, G5iv k0iv, Higher level, Hussain, Image shear, Image shear technique, Imaging, Imaging code, Imaging process, Independent maps, Intensity spectra, Internal rotation, Internal structure, Internal velocity, Journal compilation, Large convection zone depths, Last section, Latitude, Latitude strip, Lled circle, Magnetic features, Magnetic images, Magnetic maps, Magnetic regions, Magnetic structures, Many advantages, Maps show, Marks show, Maximum ratio, Middle panel, Mnras, Original paper, Physical parameters, Primary side, Primary star, Primary stars, Probability contours, Radiative core, Results show, Rotation, Rotation parameters, Rotation rate, Rotational period, Second data, Second epoch, Secondary side, Secondary star, Secondary stars, Sheared image technique, Single star, Single stars, Solid line, Solid triangles, Spot features, Spot maps, Star, Stellar, Stellar convection zone, Stellar latitude, Stellar rotations, Stellar surface, Stokes, Strassmeier rice, Surface brightness distribution, Surface maps, Surface rotation parameters, Surface rotation properties, Synchronous rotation, Synchronously, Tidal, Tidal forces, Upper plot, Variable star, Vertical line.
- Teeft :
- Binary, Binary orbit, Binary system, Binary systems, Brightness maps, Cameron, Characteristic signature, Collier, Collier cameron, Complete phase coverage, Convection, Convection zone, Convection zone depth, Convection zone depths, Convection zones, Convective, Convective envelope, Crosscorrelation technique, Data sets, Differential, Differential rotation, Differential rotation curves, Differential rotation measurement, Differential rotation measurements, Differential rotation parameters, Differential rotation rate, Differential rotation rates, Differential rotation strength, Donati, Donati collier cameron, Donati rees, Donati semel, Doppler, Doppler imaging, Doppler imaging process, Dots code, Dunstone, Eld, Equatorial rotation rate, Evolutionary models, Evolutionary stage, Fractional radius, G5iv k0iv, Higher level, Hussain, Image shear, Image shear technique, Imaging, Imaging code, Imaging process, Independent maps, Intensity spectra, Internal rotation, Internal structure, Internal velocity, Journal compilation, Large convection zone depths, Last section, Latitude, Latitude strip, Lled circle, Magnetic features, Magnetic images, Magnetic maps, Magnetic regions, Magnetic structures, Many advantages, Maps show, Marks show, Maximum ratio, Middle panel, Mnras, Original paper, Physical parameters, Primary side, Primary star, Primary stars, Probability contours, Radiative core, Results show, Rotation, Rotation parameters, Rotation rate, Rotational period, Second data, Second epoch, Secondary side, Secondary star, Secondary stars, Sheared image technique, Single star, Single stars, Solid line, Solid triangles, Spot features, Spot maps, Star, Stellar, Stellar convection zone, Stellar latitude, Stellar rotations, Stellar surface, Stokes, Strassmeier rice, Surface brightness distribution, Surface maps, Surface rotation parameters, Surface rotation properties, Synchronous rotation, Synchronously, Tidal, Tidal forces, Upper plot, Variable star, Vertical line.
Abstract
We present the first measurements of surface differential rotation on a pre‐main‐sequence binary system. Using intensity (Stokes I) and circularly polarized (Stokes V) time‐series spectra, taken over 11 nights at the Anglo‐Australian Telescope (AAT), we incorporate a solar‐like differential rotation law into the surface imaging process. We find that both components of the young, 18 Myr, HD 155555 (V824 Ara, G5IV + K0IV) binary system show significant differential rotation. The equator–pole lap times as determined from the intensity spectra are 80 d for the primary star and 163 d for the secondary. Similarly, for the magnetic spectra we obtain equator–pole lap times of 44 and 71 d, respectively, showing that the shearing time‐scale of magnetic regions is approximately half of that found for stellar spots. Both components are therefore found to have rates of differential rotation similar to those of the same spectral‐type main‐sequence single stars. The results for HD 155555 are therefore in contrast to those found in other, more evolved, binary systems where negligible or weak differential rotation has been discovered. We discuss two possible explanations for this: first that at the age of HD 155555 binary tidal forces have not yet had time to suppress differential rotation and secondly that the weak differential rotation previously observed on evolved binaries is a consequence of their large convection zone depths. We suggest that the latter is the more likely solution and show that both temperature and convection zone depth (from evolutionary models) are good predictors of differential rotation strength. Finally, we also examine the possible consequences of the measured differential rotation on the interaction of binary star coronae.
Url:
DOI: 10.1111/j.1365-2966.2008.13338.x
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A. Collier Cameron<affiliation><mods:affiliation>School of Physics and Astronomy, University of St Andrews, Fife KY16 9SS</mods:affiliation>
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<term>Differential rotation measurement</term>
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<term>Latitude strip</term>
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<term>Magnetic images</term>
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<term>Surface rotation parameters</term>
<term>Surface rotation properties</term>
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<term>Synchronously</term>
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<front><div type="abstract" xml:lang="en">We present the first measurements of surface differential rotation on a pre‐main‐sequence binary system. Using intensity (Stokes I) and circularly polarized (Stokes V) time‐series spectra, taken over 11 nights at the Anglo‐Australian Telescope (AAT), we incorporate a solar‐like differential rotation law into the surface imaging process. We find that both components of the young, 18 Myr, HD 155555 (V824 Ara, G5IV + K0IV) binary system show significant differential rotation. The equator–pole lap times as determined from the intensity spectra are 80 d for the primary star and 163 d for the secondary. Similarly, for the magnetic spectra we obtain equator–pole lap times of 44 and 71 d, respectively, showing that the shearing time‐scale of magnetic regions is approximately half of that found for stellar spots. Both components are therefore found to have rates of differential rotation similar to those of the same spectral‐type main‐sequence single stars. The results for HD 155555 are therefore in contrast to those found in other, more evolved, binary systems where negligible or weak differential rotation has been discovered. We discuss two possible explanations for this: first that at the age of HD 155555 binary tidal forces have not yet had time to suppress differential rotation and secondly that the weak differential rotation previously observed on evolved binaries is a consequence of their large convection zone depths. We suggest that the latter is the more likely solution and show that both temperature and convection zone depth (from evolutionary models) are good predictors of differential rotation strength. Finally, we also examine the possible consequences of the measured differential rotation on the interaction of binary star coronae.</div>
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