2 edition of Metallic line profiles of the AOV star Vega found in the catalog.
Metallic line profiles of the AOV star Vega
by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, D.C.?, Springfield, Va
Written in English
|Statement||J. Murray Fletcher ... [et al.].|
|Series||NASA contractor report -- NASA CR-186906.|
|Contributions||Fletcher, J. Murray., United States. National Aeronautics and Space Administration.|
|The Physical Object|
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Metallic Line Profiles of the A0V Star Vega J. Murray Fletcher Dominion Astrophysical Observatory Austin F. Gulliver 1 Department of Physics and Astronomy, Brandon University Saul J. Adelman 1 Department of Physics, The Citadel and Charles R.
Cowley I Department of Astronomy, University of Michigan (NASA-C,_-I.:IAg06) MFTALLIC LINa P_:_rlLES qF. Metallic line profiles of the AOV star Vega. High dispersion ultrahigh signal to noise Reticon spectra of Vega were obtained with the coude spectrograph of the m telescope.
A mean signal to noise ratio of over the spectral region lambdas from to was achieved. Get this from a library. Metallic line profiles of the AOV star Vega. [J Murray Fletcher; United States.
National Aeronautics and Space Administration.;]. Examination of the line profiles confirmed the presence of two different types of profiles which were previously seen in IIIaJ and lower signal to noise Reticon spectra.
The profiles of the strong lines are essentially classical rotational profiles with enhanced wings which are slightly stronger than expected while those of weak lines are clearly flat-bottomed resulting in a. By fitting to the flat-bottomed line profiles of Fe 1 lambda and Ti 2 lambdawe find least-squares fit values of V sin i = plus or minus km/sec polar T(sub eff) = plus or.
Compare the above Vega spectrum with the blackbody curve at K. The blackbody curve peak is at å which is in the UV part of the electromagnetic spectrum. Vega's spectrum continuum shape shows us its blackbody temperature. Vega is also known as Alpha Lyrae (α Lyrae, Alpha Lyr, α Lyr), as it is the principle star in the constellation Lyra, the lyre.
Vega has been one of the most important stars to humanity since ancient times because it is very bright and easily recognized by its blue color. Absolute Flux Calibrated Spectrum of Vega L. Colina, R. Bohlin, F. Castelli Ap ABSTRACT An absolute ﬂux calibrated reference spectrum of Vega, the primary calibration standard in the optical, is presented.
The spectrum covers the entire to microns wavelength. The ultraviolet spectrum is based on IUE Size: KB. Vega is the brightest star in the northern constellation of has the Bayer designation α Lyrae, which is Latinised to Alpha Lyrae and abbreviated Alpha Lyr or α star is relatively close at only 25 light-years from the Sun, and, together with Arcturus and Sirius, one of the most luminous stars in the Sun's is the fifth-brightest star in the night sky, and the Constellation: Lyra.
Vega was the North Star several thousand years ago, and it will regain that status in ab years. Locating Vega Vega is almost directly overhead at.
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Here you'll find current best sellers in books, new releases in books, deals in books, Kindle eBooks, Audible audiobooks, and. Vega, the second brightest star visible in the northern hemisphere, is used by astronomers as a standard against which other stars are calibrated.
The intensity of light throughout its spectrum is. Vega is the fifth brightest star in the sky, and the brightest in the constellation Lyra, overhead in summer to observers in the northern hemisphere. Vega has been extensively studied, leading it to be termed "arguably the next most important star in the sky after the Sun".
each spectrum, a mean polarized line proﬁle with a signal-to-noise ratio of ab The technique of Zeeman-Doppler Imaging is then used to determine the rotation period of the star and reconstruct the large-scale magnetic geometry of Vega at two di erent epochs.
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Vega's rapid rotation causes the star to bulge considerably at its equator. As a result of its brightness and close proximity Vega is the most studied star apart from the sun. In 10, years Vega will replace Polaris as the northern pole star.
In Vega became the first star. Vega is a Rapidly Rotating Star T.A. Pauls1 and D.M. Peterson2 1Remote Sensing Division 2Stony Brook University A star’s most important attributes are its mass, temperature, radius, composition, and rate of rotation. The Sun, for example, rotates once every 28 days, which implies a surface speed of about 2 kilometers per second at the equator.
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Warranty:. In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Electromagnetic radiation from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with spectral line indicates a particular chemical element or molecule, with the line strength.
3 II: Flux and luminosity Definition: The observed flux of a star is the energy received from the star per unit time per unit area. The area under consideration must be oriented face-on to line- of-sight to the star In principle, this definition works for any kind of energy emitted by the star most commonly, we mean e/m radiationFile Size: 1MB.Vega is a classic class A (A0) white main sequence dwarf star, like the Sun quietly running off the nuclear fusion of hydrogen deep in its core, with a sort of average effective surface temperature of about degrees Kelvin.
Its white color and apparent brightness made it a basic standard against which the apparent magnitudes of other stars are compared.The Wandering Star (The Vega Chronicles Book 1) - Kindle edition by Mengel, A.L. Download it once and read it on your Kindle device, PC, phones or tablets.
Use features like bookmarks, note taking and highlighting while reading The Wandering Star (The Vega Chronicles Book 1)/5(2).