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Sunday, July 12, 2020 | History

3 edition of Emission lines in the long period Cepeheid [script l] Carinae found in the catalog.

Emission lines in the long period Cepeheid [script l] Carinae

Emission lines in the long period Cepeheid [script l] Carinae

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • Cepheids.,
  • Emission-line galaxies.

  • Edition Notes

    StatementErika Böhm-Vitense and Stanley G. Love.
    SeriesNASA contractor report -- NASA CR-190853.
    ContributionsLove, Stanley G., United States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL17677859M

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    The correct answer that would best complete the given statement above would be option B. Non-intersecting lines that are separated by equal distances at every point can best be described as PARALLEL. When the lines are parallel, they do not intersect. Hope this answers your question. 3. Why does each metal have its own distinctive flame test color? When an element is burned it gives off an emission spectrum. Every element has different electron configurations and it is the outermost electrons that are excited by the heat energy. When relaxed they give off energy, therefore in the relaxation process each element emits light of a different energy giving it a different color.


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Emission lines in the long period Cepeheid [script l] Carinae Download PDF EPUB FB2

Get this from a library. Emission lines in the long period Cepeheid [script l] Carinae. [E Böhm-Vitense; Stanley G Love; United States. National Aeronautics and Space Administration.].

Eta Carinae (η Carinae, abbreviated to η Car), formerly known as Eta Argus, is a stellar system containing at least two stars with a combined luminosity greater than five million times that of the Sun, located around 7, light-years (2, parsecs) distant in the constellation usly a 4th-magnitude star, it brightened in to become brighter than Rigel, marking the start of Constellation: Carina.

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Spectral Lines. Atoms and molecules can emit and absorb radiation at distinct wavelengths, causing the appearance of spectral lines. When acquiring a spectrum of an astronomical object, astronomers rely upon spectral lines to determine a myriad of physical properties, such as composition, temperature, ionization state, velocity, redshift and more.

Measurements of the asymmetry of the emission peaks in the core of the Ca ii H line for giant stars are reported. The asymmetry is quantified with the parameter V/R, defined as the ratio between the maximum number of counts in the blueward peak and the redward peak of the emission Ca ii H and K emission lines probe the differential motion of certain chromospheric layers Cited by: 1.

Abstract. Profiles of the H and K lines of Mg II and the K line of Ca II are computed using a two-level atom for five model atmospheres distinguished from each other mainly by the location of the temperature minimum.

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