Spectral line formation
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Spectral line formation by John T. Jefferies

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Published by Blaisdell Pub. Co. in Waltham, Mass .
Written in English

Subjects:

  • Astronomical spectroscopy.

Book details:

Edition Notes

Includes bibliographies.

Statement[by] John T. Jefferies.
SeriesA Blaisdell book in the pure and applied sciences
Classifications
LC ClassificationsQB465 .J4
The Physical Object
Paginationxx, 298 p.
Number of Pages298
ID Numbers
Open LibraryOL5542249M
LC Control Number67020145

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Spectral line formation. Author: John T Jefferies. Publisher: Waltham, Mass., Blaisdell Pub. Co. [] Series: Blaisdell book in the pure and applied sciences. Edition/Format: Print book: English View all editions and formats. Spectral line formation theory is at the heart of astrophysical diagnostic. Our knowledge of abundances, in both stellar and interstellar contexts, comes almost enti­ rely from line analysis, as does a major fraction of our ability to model stellar atmospheres. 13 ⋅ Formation of Spectral Lines Figure shows the equivalent 'black' line profile (double cross-hatched area) appropriate for a specific spectral line (single cross-hatched area). The areas of the two profiles are equal and so the rectangular one can be characterized by its width alone. Such equivalent widths are usually measured in. adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86ACited by:

6. Sodium D line source functions for an atmosphere with continuous absorption r'zI = l0'. Studies in spectral line formation The integral equations for the problem were solved in the step function approximation, and the solutions Slz) and SO) (scaled to unit Wien function) are shown in Fig. 6. 3D SIMULATION OF CONVECTION AND SPECTRAL LINE FORMATION IN A-TYPE STARS M. Steffen1, B. Freytag2, and H.-G. Ludwig3 1Astrophysikalisches Institut Potsdam, An der Sternwa D Potsdam, Germany 2GRAAL, Universit´e de Montpellier II, F Montpellier, France 3Lund Observatory, S Lund, Sweden Abstract We present first realistic numerical . 14 ⋅ Shape of Spectral Lines In practice, all these effects are present and give the line its characteristic shape. The correct representation of these effects allows for the calculation of the observed line profile and in the process reveals a great deal about the conditions in the star that give rise to the spectrum. () NLTE Spectral Line Formation in a Three-Dimensional Atmosphere with Velocity Fields. In: Beckman J.E., Crivellari L. (eds) Progress in Stellar Spectral Line Formation Theory. NATO ASI Series (Series C: Mathematical and Physical Sciences), vol

We can use Bohr’s model of the atom to understand how spectral lines are formed. The concept of energy levels for the electron orbits in an atom leads naturally to an explanation of why atoms absorb or emit only specific energies or wavelengths of light. Spectral line formation theory is at the heart of astrophysical diagnostic. Our knowledge of abundances, in both stellar and interstellar contexts, comes almost enti rely from line analysis, as does a major fraction of our ability to model stellar atmospheres. Spectral line shapes in astrophysics VI Serbian Conference on Spectral Line Shapes in Astrophysics (VI SCSLSA), Sremski Karlovci, Serbia, June This edition published in by American Institute of Physics in Melville, N.Y. PDF | On , N. J. McCormick and others published Spectral-Line Formation by Noncoherent Scattering | Find, read and cite all the research you need on ResearchGate.