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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3765
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dc.contributor.authorMekkaden, M. V-
dc.contributor.authorGeyer, E. H-
dc.date.accessioned2008-09-22T11:51:47Z-
dc.date.available2008-09-22T11:51:47Z-
dc.date.issued1988-04-
dc.identifier.citationAstronomy and Astrophysics , Vol. 195, No. 1 - 2, pp. 214 - 217en
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/2248/3765-
dc.description.abstractUBVRI photometry of the chromospherically active star HD 127535 obtained during April 1987 is presented. The analysis shows that the light variation is quasi-sinusoidal and the amplitude and the phase of the light minimum have changed drastically compared to the previous observations. These changes are attributed to the formation and evolution of magnetically active regions on the stellar surface. Furthermore, a quantitative analysis of the observations available in the literature since 1981 indicates that the sudden changes in activity on HD 127535 may be caused by short-lived spot groups rather than a single spot of longer life time. The maximum activity on HD 127535 occured during 1985.en
dc.language.isoenen
dc.publisherEuropean Southern Observatoryen
dc.relation.urihttp://adsabs.harvard.edu/abs/1988A%26A...195..214Men
dc.subjectH alpha lineen
dc.subjectLuminous intensityen
dc.subjectPhotometryen
dc.subjectStarspotsen
dc.subjectStellar atmospheresen
dc.subjectUBV spectraen
dc.subjectComputational astrophysicsen
dc.subjectLight curveen
dc.subjectLight sourcesen
dc.subjectRadio emissionen
dc.titleThe variation of photospheric active regions in HD 127535en
dc.typeArticleen
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