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Hyades and Sirius supercluster members brighter than magnitude(V) 7.1. I - The first six hours of right ascension
This is the first of four papers listing the probable members of theHyades and Sirius superclusters among stars brighter than V = 7.1 mag.The star sample is contained in the Bright Star Catalogue and itsSupplement, augmented with a further supplement of 550 stars foundduring various observing programs over the past 40 years. Accurate,four-color and H-beta, or (RI), photometry is available for most of thesupercluster members. The criteria for membership are the comparisons ofthe proper motion, radial velocity, and luminosity obtained from thesupercluster parameters with the observed motions and the luminosityderived from the photometric parameters. New proper motions, based onall available catalogs, have been derived for the additional 550 starsdiscussed here, as well as for all supercluster members.
| A photometric study of the close binary Delta Orionis A
Green and blue photoelectric light curves show the historical intrinsicvariability of the Delta Ori A close binary superposed on theinteraction and eclipse effects. There is a considerable measure ofagreement between spectrographic and photometric determinations of therate of apsidal advance. The determinacy of orbital eccentricity,however, is confused because few minima of indifferent precision existto check the spectrographic value. No physical mechanism can be found toaccount for a possible diminution of orbital eccentricity, and this isprobably best attributed to unrecognized complications of at least oneof the existing light curves. After numerous trials, a less-than-perfecttheoretical representation of the light curve was achieved and shows thesystem to be detached. The absolute stellar parameters make clear thatboth components have evolved substantially. A mean stellar structureconstant k2 is derived but cannot be compared usefully to existingtheoretical values. The importance of the recently discovered visualcompanion, hz 42, is emphasized.
| The Kreinin-Murri Method for Absolute Determination of Equatorial-Star Declinations.
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