3 edition of atlas of spectral line profiles of P Cygni in 1981-83 found in the catalog.
atlas of spectral line profiles of P Cygni in 1981-83
N. Markova
Published
1989
by Valgus in Tallinn
.
Written in English
Edition Notes
| Other titles | Atlas profileĭ spektralʹnykh liniĭ zvezdy P Cygni v 1981-83 gg. |
| Statement | N. Markova and I. Kolka. |
| Contributions | Kolka, I. |
| Classifications | |
|---|---|
| LC Classifications | QB843.B12 M37 1989 |
| The Physical Object | |
| Pagination | 13 p. : |
| Number of Pages | 13 |
| ID Numbers | |
| Open Library | OL1769825M |
| ISBN 10 | 5440009922 |
| LC Control Number | 92122001 |
Abstract: P Cygni is a prototype for understanding mass loss from massive stars. This textbook star is known first of all because of two great eruptions in the 17th century. In the first half of this century it has given its name to a class of stars which are characterized by spectral lines consisting of nearly undisplaced emissions accompanied by a blue-displaced absorption component. An Atlas of Stellar Spectra Astrophys. monographs, Univ. Chicago Press () AN ATLAS OF STELLAR SPECTRA WITH AN OUTLINE OF SPECTRAL CLASSIFICATION Morgan * Keenan * Kellman Table of Contents INTRODUCTION THE O5-F2 STARS The O Stars O B0 B B1 B2 B3 B5 B8 The Spectrum of Draconis The A Stars B9 A0 A1 A2 A3 A5 A7 F0 F2 The Peculiar A Stars.
Charting the Spectral Profiles. At this point, using your imagery and the training samples feature class, you can create your spectral profiles chart: Right-click on the image to be classified in the Contents pane; Select Create Chart > Spectral Profile; In the Chart Properties pane, choose Mean Line as . spectral window to another in CASA use the refspwmap parameter in fluxscale. • For example, if spw 2 (of 4) has a poor calibration due to a strong absorption line, setting refspwmap=[0,1,3,3] will use the calibration of spw3 on spw2 (in the 2nd slot). Fourteenth Synthesis Imaging Workshop
Spectral line series, any of the related sequences of wavelengths characterizing the light and other electromagnetic radiation emitted by energized atoms. The simplest of these series are produced by hydrogen. When resolved by a spectroscope, the individual components of the radiation form images of the source (a slit through which the beam of radiation enters the device). HERUS: A CO ATLAS FROM SPIRE SPECTROSCOPY OF LOCAL ULIRGs. United States: N. p., [C i] μ m, and [N ii] μ m. We also detect H{sub 2}O lines in several objects. We construct CO spectral line energy distributions (SLEDs) for the sample, and compare their slopes with the far-infrared (FIR) colors and luminosities. We show that.
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Adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86ACited by: 1.
An Atlas of Spectral Line Profiles of P Cygni in – pp. 3–15, (Tartu Teated nr. ).Author: Indrek Kolka. P Cygni is a LBV (B1 Ia+) which exhibits photometric and spectroscopic this book is about 2 We present observational data from two periods (–82 and –90) pointing to three different variability by: 1.
Ca II line (thanks to Robin Leadbeater!). Version P Cygni profiles, P Cygni, 34 Cyg – – L L 13A 42 Detailed spectrum LBV star, early B-class, P Cygni profiles P Cygni 34 Cyg – However, a real “Spectral Atlas. New aspects of line-profile variability in P Cygni's optical spectrum Article (PDF Available) in Astronomy and Astrophysics Supplement Series (3) June with 12 Reads How we measure 'reads'.
An atlas of theoretical P Cygni-type line profiles is presented. The profiles are calculated by assuming resonance scattering and using the Sobolev approximation. This paper presents results on spectral line and profile variability, equivalent widths and line identification for α Cygni (A2 Ia) and ε Aurigae (A8 Ia).
The results are based upon photometrically precise spectra obtained with a Michelson-Fourier spectrophotometer. The wavelength interval extends from to microns, approximately.
High resolution spectral atlas of P Cygni (Heidelberg) An Atlas of Ultraviolet P Cygni Profiles (ADS) Feibelman,W.A.:PASP.,The IUE Absorption Spectrum of the Nucleus of NGC Mostly C IV (P-Cygni line) and O VI; Markova,N., Zamanov,R.:AASup.,P Cygni-spectral atlas with complete line identifications in the.
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.
P Cygni (34 Cyg) is a variable star in the constellation Cygnus. The designation "P" was originally assigned by Johann Bayer in Uranometria as a nova. Located about to light-years (– parsecs) from Earth, it is a hypergiant luminous blue variable (LBV) star of spectral type B1Ia+ that is one of the most luminous stars in the Milky Way.
The eclipsing binary system 31 Cygni (K4 Ib + B3 V) was observed during total and chromospheric eclipse with the Far Ultraviolet Spectrosocopic Explorer (FUSE) satellite.
The observations from the eight different FUSE channels have been coadded to produce a single spectrum from each phase, and we present an atlas of these spectra with line identifications. Spectral Atlas for Amateur Astronomers: A Guide to the Spectra of Astronomical Objects and Terrestrial Light Sources Richard Walker Featuring detailed commented spectral profiles of more than one hundred astronomical objects, in colour, this spectral guide documents most of the important and spectroscopically observable objects accessible using.
Atlas of Spectral Data and Physical Constants for Organic Compounds Volume 1 of Atlas of spectral data and phyisical constants for organic compounds, Jeanette G. Grasselli, ISBNAuthors: Jeanette G.
Grasselli, William M. Ritchey: Editors: Jeanette G. Grasselli, William M. Ritchey: Edition: 2: Publisher: CRC Press. This spectral atlas contains a sample of the standard spectral type stars, peculiar stars, variable stars, and some special stars.
The atlas is divided into pages for each spectral type, with each page containing a short description of the stellar type, characteristic spectral features, and a brief physical explantaion.
A single spectral line at a certain spectral position is fully characterized by its strength (the intensity, or integrated absorption coefficient) and its line half-width (plus knowledge of the broadening mechanism, i.e., collision and/or Doppler broadening).
However, a vibration–rotation band has many closely spaced spectral lines that may overlap considerably. Buy Atlas of Spectral Interferences in Icp Spectroscopy on FREE SHIPPING on qualified orders Atlas of Spectral Interferences in Icp Spectroscopy: Parsons, Malcolm: : Books.
The gain curve has the same shape as the fluorescent line, and the loss is essentially independent of frequency, at least over a reasonably small range. All modes for which the gain is greater than loss can be present in the laser output.
Thus, the spectral form of the output can be as shown in Figure c. Line profiles. A great deal of information can be extracted by detailed examination of spectral lines, such as redshift, radial velocity, expansion velocity, temperature, and much more.
This section will grow as more authors cover particular spectral methods that appear in the literature. P Cygni profiles. P Cygni stars. The characteristic star of this group is P Cygni, a nova which flared up in P Cygni is now a variable B1 supergiant of mean magnitude. P Cygni stars lines shows a profile type called "P Cyg": an emission component to the red side of an aborption line.
Spectral-line emission and absorption are intrinsically quantum phenomena. Classical particles and waves are idealized concepts like infinitesimal points or perfectly straight lines in geometry; they don’t exist in the real world.
Some things are nearly waves (e.g., radio waves) and others are nearly particles (e.g., electrons), but all share characteristics of both particles and waves. Spectral line shape describes the form of a feature, observed in spectroscopy, corresponding to an energy change in an atom, molecule or line shapes include Lorentzian, Gaussian and Voigt functions, whose parameters are the line position, maximum height and half-width.
Actual line shapes are determined principally by Doppler, collision and proximity broadening.The shape of the P-Cygni profile is effected by several properties of the supernova atmosphere. We demonstrate the effect of four important ones here: 1.
The velocity of the photosphere. 2. The optical depth of the line. 3. The density structure of the atmosphere.
4. The line source function.Widths of spectral lines • Real spectral lines are broadened because: –Energy levels are not infinitely sharp. –Atoms are moving relative to observer. • Threemechanisms determine the line profile f (n) –Quantum mechanical uncertainty in the energy E of levels with finite lifetimes.
Determines the natural width of a line (generally.
