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Saturday, August 8, 2020 | History

1 edition of Photoelectric line-photometry of early B-type stars. found in the catalog.

Photoelectric line-photometry of early B-type stars.

Photoelectric line-photometry of early B-type stars.

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Published by Almquist & Wiksell in Stockholm .
Written in English

    Subjects:
  • Astronomical photometry.,
  • Stars.

  • Edition Notes

    Bibliography: p. 123-124.

    StatementBy U. Sinnerstad [and others]
    SeriesArkiv för astronomi,, bd. 5, nr. 5
    ContributionsSinnerstad, Ulf.
    Classifications
    LC ClassificationsQB1 .A293 bd. 5, nr. 5
    The Physical Object
    Pagination105-124 p.
    Number of Pages124
    ID Numbers
    Open LibraryOL5158249M
    LC Control Number74445283

    discontinuity has been quite successful. The growth of precise multicolor photoelectric photometry has permitted distinctions to be made between space reddening and tem­ perature reddening, between stars of the two population types, and even permitted colorimetric identification of the white dwarfs. A complete explanation of the observed. Photoelectric Light Curve off 44 Bootis, Information Bulletin on Variable Stars, () Our Turn at Kitt Peak, Sky and Telescope, Vol. 63, p. () New Books and Equipment for Photoelectric Photometry/Abstract, Journal of the AAVSO, Vol. , p. () Photoelectric Photometry, Comet News Service, Vol. , p.

    Photoelectric Photometry of Variable Stars, second revised edition, Willman-Bell, Inc. NEAR-INFRARED PHOTOMETRY OF MERCURY Here, Cecilia Payne-Gaposchkin reported highlights from a conference at Mexico's Tonantzintla Observatory, soon to play its own key role in the photoelectric photometry of bright stars. Class A stars are white or bluish-white. About % of the stars in the sky are class A. Class F stars are white and make up about 3% of stars. Class G stars are yellowish white. Our sun is a.

    The photoelectric factor (PeF) was introduced in the early's as a supplementary measurement to the bulk density measurement by Schlumberger, who signaled its appearance by the designation 'Lithodensity' log. Other logging companies typically use a variant of Z-densilog as the name, where 'Z' represents atomic number whose aggregate content. Other articles where Photographic photometry is discussed: photometry: The fact that photographic plates are sensitive to violet and ultraviolet radiation, rather than to the green and yellow wavelengths to which the eye is most sensitive, led to the establishment of two separate magnitude scales, the visual and the photographic. The difference between the magnitudes given by.


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Photoelectric line-photometry of early B-type stars Download PDF EPUB FB2

Photoelectric measurements of H-alpha line strengths are presented for early-type stars intended for use as standard stars in a photometric H-alpha system to supplement the H-beta standard system.

adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86ACited by: 1. Photoelectric photometry of variable stars: A practical guide for the smaller observatory Unknown Binding – January 1, by Douglas S Hall (Author) › Visit Amazon's Douglas S Hall Page.

Find all the books, read about the author, and more. 4/5(1). SAO/NASA Astrophysics Data System (ADS) Title: Photoelectric line-photometry of early B-type stars Authors: Sinnerstad, U., Arkling, J., Alm, S.

H., & Brattlund, P. Photoelectric Photometry of Variable Stars: A Practical Guide for the Smaller Observatory Hardcover – July 1, by Douglas S.

Hall (Author) › Visit Amazon's Douglas S. Hall Page. Find all the books, read about the author, and more.

See search results for this author. Are you an author. Cited by: 2. Photometry, in astronomy, the measurement of the brightness of stars and other celestial objects (nebulae, galaxies, planets, etc.). Such measurements can yield large amounts of information on the objects’ structure, temperature, distance, age, etc.

The earliest observations of the apparent. K-Line Photometry of a Stars. whereas for B-type dwarfs photometry is at least two times more precise than MK classification. A precision of ± tenths of a spectral class seems attainable.

A bibliography of papers concerning Strömgren four-color photometry and H Photoelectric line-photometry of early B-type stars. book photometry is presented, covering the years – The papers. Comparison of the Hyades, Coma, and Pleiades Clusters Based on Photoelectric u, v, b, y and Hp Photometry* DAVID L.

CRAWFORD Kitt Peak National Observatory, Tucson, Arizona, U.S.A.* and BENGT STROMGREN Institute for Advanced Study, Princeton, New Jersey, U.S.A. ON the basis of photoelectric U, B, V photometry, JOHNSON and KNUCKLES () carried out a comparison of.

early{type emission{line stars by Wackerling () with those of the IRAS Point Source Catalogue (PSC) was car-ried out by Dong & Hu (). These authors selected only objects with a very strong IR excess, V −[25] 8 mag, and found such ob-jects.

Only about 30% of this sample consists of objects with a known nature: Herbig Ae/Be stars. Photoelectric Photometry of Variable Stars Books, Find the lowest price on new, used books, textbooks Compare Book Prices at Stores. Help Bookmark Tell a Friend Out-of-Print Wish List Home. Photoelectric Photoometry of Variable Stars, 2nd Edition.

Photoelectric Photometry of Variable Stars, 2nd Edition, A Practical Guide for the Smaller Observatory, edited by Douglas S. Hall and Russell M.

Genet. 6" x 9", pages, hardbound. Rigel / ˈ r aɪ dʒ əl /, designated β Orionis (Latinized to Beta Orionis, abbreviated Beta Ori, β Ori), is a blue supergiant star in the constellation of Orion, approximately light-years ( pc) from is the brightest and most massive component—and the eponym—of a star system of at least four stars that appear as a single blue-white point of light to the naked eye.

Instead it was agreed that we should attempt to arrange a separate symposium, dealing with the fundamental problems of the cali­ bration of absolute magnitudes and temperatures of stars. The Executive Committee of the IAU accepted our proposal, and IAU Symposium No.

54 was held in Geneva on September, sponsored by thefollowing IAU. ISBN: OCLC Number: Description: 1 online resource (xiii, pages) Contents: I/An Introduction to the Early Type Stars and to the Means of Observing Them The early type stars Techniques by which information is obtained Stellar spectrographs The classification and description of early type spectra --II/Improved Systems of Spectral.

Inthe AAVSO developed a photoelectric photometry (PEP) observing program, targeting variable stars of all types that exhibit a small amplitude of variation, often less than one magnitude. In order to participate, you need an equatorially driven telescope of at least 6-inch aperture and a photoelectric.

Photoelectric photometry is an observational technique used to obtain highly precise, calibrated observations of small amplitude variables. The AAVSO PEP Program was formally established inbut our archive has PEP observations dating back to the 's. Photoelectric Line-photometry of early B-type stars Arkiv för Astronomi, Band 5,Nr.5 Sinnerstad, U., J.

Arkling S.h. Alm u. a.: Published by Almqvist & Wiksell Verlag (). Wolpert, R.C: A Photon-Counting Stellar Photometer, p. in Photoelectric Photometry of Variable Stars, D.S.

Hall and R.M. Genet (eds.), International Amateur-Professional Photoelectric Photometry, Fairborn OH Google Scholar. In this book you learn how dedicated amateurs, using either home built or commercial equipment, regularly produce data that is published in professional journals.

One example, Louis Boyd (shown on the front cover) designed and built an automatic photoelectric telescope that makes hundreds of observations each clear night. The American Astronomical Society (AAS), established in and based in Washington, DC, is the major organization of professional astronomers in North America.

Its membership of. This article discusses the three photometric data categories: Type A, Type B and Type C. These types describe the photometric web surrounding the light source and were designed to match the type of source being measured or tested. At present, onl.similar stars, the opacity distribution function (ODF) ap-proach remains preferable due to its higher computational efficiency.

Piskunov & Kupka () have presented a new software toolkit based on this approach using a modified ver-sion of the ATLAS9 code of Kurucz (b).

It is suitable for spectral types from early B type to early F type.