Differential rotation on both components of the pre-main-sequence binary system HD 155555
Identifieur interne : 002A71 ( Istex/Curation ); précédent : 002A70; suivant : 002A72Differential 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.-F. Donati [France]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2008-07-11.
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.
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DOI: 10.1111/j.1365-2966.2008.13338.x
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N. J. Dunstone<affiliation><mods:affiliation></mods:affiliation><wicri:noCountry code="syntax">???</wicri:noCountry></affiliation><affiliation wicri:level="1"><mods:affiliation>E-mail: njd2@st-andrews.ac.uk</mods:affiliation><country wicri:rule="url">Royaume-Uni</country></affiliation><affiliation><mods:affiliation>School of Physics and Astronomy, University of St Andrews, Fife KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation><affiliation><mods:affiliation>School of Physics and Astronomy, University of St Andrews, Fife KY16 9SS</mods:affiliation><wicri:noCountry code="subField">9SS</wicri:noCountry></affiliation><affiliation><mods:affiliation>Centre for Astrophysics Research, University of Hertfordshire, Hertfordshire AL10 9AB</mods:affiliation><wicri:noCountry code="subField">9AB</wicri:noCountry></affiliation>Le document en format XML
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Belin, F-31400 Toulouse</wicri:regionArea></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbrev">Monthly Notices of the Royal Astronomical Society</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2008-07-11">2008-07-11</date><biblScope unit="volume">387</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="1525">1525</biblScope><biblScope unit="page" to="1536">1536</biblScope></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass></profileDesc></teiHeader><front><div type="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.</div></front></TEI></record>Pour manipuler ce document sous Unix (Dilib)
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