A systematic method for the analysis of high-resolution fraunhofer line profiles

Solar Physics ◽  
1967 ◽  
Vol 1 (1) ◽  
pp. 27-59 ◽  
Author(s):  
C. De Jager ◽  
L. Neven
Keyword(s):  
High Resolution ◽  
Line Profiles ◽  
Systematic Method ◽  
Fraunhofer Line

scholarly journals Anomalous Fraunhofer Line Profiles

Nature ◽  
1962 ◽  
Vol 193 (4817) ◽  
pp. 762-762 ◽  
Author(s):  
J. F. GRAINGER ◽  
J. RING
Keyword(s):  
Line Profiles ◽  
Fraunhofer Line

scholarly journals High resolution spectroscopy of RY Tauri: variability of the Na D line profiles

1990 ◽  
Vol 137 ◽  
pp. 219-220
Author(s):  
P.P. Petrov
Keyword(s):  
High Resolution ◽  
Large Scale ◽  
Young Stars ◽  
High Resolution Spectroscopy ◽  
Line Profiles

Ejection and accretion of gas clouds in the vicinity of RY Tau were discovered. The existense of large scale “stellar prominences” around young stars is suggested.

scholarly journals New Progress in Mode Detection and Identification in δ Scuti Stars by the Analysis of Line Profile Variations

2000 ◽  
Vol 176 ◽  
pp. 463-464
Author(s):  
L. Mantegazza ◽  
E. Poretti ◽  
M. Bossi ◽  
N. S. Nuñez ◽  
A. Sacchi ◽  
...  
Keyword(s):  
High Resolution ◽  
Line Profile ◽  
High Resolution Spectroscopy ◽  
Line Profiles ◽  
Powerful Technique ◽  
Mode Detection ◽  
Detection And Identification ◽  
Scuti Stars ◽  
Δ Scuti Stars ◽  
Nonradial Pulsation

Abstractδ Sct stars are among the most promising targets to perform ground-based asteroseismology. High resolution spectroscopy offers us a powerful technique to identify radial and nonradial pulsation modes, since we can easily detect oscillations and travelling features in the line profiles.

scholarly journals Kinematic Structure and Chemical Composition of the Double Shell PN NGC 3242

1989 ◽  
Vol 131 ◽  
pp. 200-200
Author(s):  
K. C. Sahu ◽  
S. R. Pottasch ◽  
B. G. Anandarao ◽  
J. N. Desai
Keyword(s):  
Chemical Composition ◽  
High Resolution ◽  
Outer Shell ◽  
Expansion Velocity ◽  
Kinematic Structure ◽  
Line Profiles ◽  
Kinematic Study ◽  
Fabry Perot

Kinematic study of the multiple shell PN NGC 3242 was carried out by obtaining Hα and [O III] line profiles at 9 positions of the nebula using a high-resolution (R ≅ 50,000) Fabry-Pérot spectrometer. The positions cover both the bright inner shell and the faint outer shell. It is shown here that the two apparently continuous shells are kinematically separate: the faint outer shell was ejected ∼ 5000 years earlier and has less expansion velocity than the bright inner shell.

scholarly journals Zodiacal Light - Scattered Fraunhofer Line Profiles

1996 ◽  
Vol 150 ◽  
pp. 337-340
Author(s):  
David Clarke
Keyword(s):  
Line Shape ◽  
Brightness Variation ◽  
Line Profiles ◽  
Scattering Function ◽  
Zodiacal Light ◽  
Successful Model ◽  
Fraunhofer Line ◽  
Shape Changes

AbstractThe scattering function of Hong's successful model for the brightness variation with elongation, B(ε), of the Zodiacal Light has been used to calculate profiles of Doppler shifted Fraunhofer lines. Substantial line shape changes with ε are predicted with an indication of a bifurcation at ε < 30°, so offering an explanation for reported F corona observations.

High resolution J = 2 - 1 and J = 1 - 0 carbon monoxide self-reversed line profiles toward molecular clouds

1981 ◽  
Vol 245 ◽  
pp. 495 ◽  
Author(s):  
R. B. Loren ◽  
R. L. Plambeck ◽  
J. H. Davis ◽  
R. L. Snell
Keyword(s):  
Carbon Monoxide ◽  
High Resolution ◽  
Molecular Clouds ◽  
Line Profiles ◽  
Reversed Line

scholarly journals A high-resolution study of the outer parts of the Galaxy

1964 ◽  
Vol 20 ◽  
pp. 131-134 ◽  
Author(s):  
B. F. Burke ◽  
K. C. Turner ◽  
M. A. Tuve
Keyword(s):  
High Resolution ◽  
West Virginia ◽  
Single Channel ◽  
Longitudinal Section ◽  
Line Profiles ◽  
Carnegie Institution ◽  
Pointing Error ◽  
Frequency Scale ◽  
The Galaxy ◽  
Resolution Study

The 300-foot transit telescope at the N.R.A.O. at Green Bank, West Virginia, was used in conjunction with the Carnegie 90-channel H-line spectrograph to study the far parts of the Galaxy between l = 11° and l = 50° (lII and bII are to be understood throughout). A travelling feed was constructed at the Carnegie Institution which enabled us to track one point in the sky for approximately 5m40s. This made it possible to make two completely independent frequency scans of a given point each day. On successive days, duplicate curves were taken with the frequency scale shifted, in order to guard against single channel anomalies and pointing error. Line profiles were taken at 160 points in the region under study, in meridional sections every 5° of l, from b = −0°8 to +2°0 in steps of 0°. In addition, a single longitudinal section was taken at b = +0°4 in steps of 1°.

Improved Non-LTE Model Atmospheres for Subluminous O-Stars

1988 ◽  
Vol 132 ◽  
pp. 117-122
Author(s):  
U. Heber ◽  
K. Hunger ◽  
T. Rauch ◽  
K. Werner
Keyword(s):  
High Resolution ◽  
New Method ◽  
Balmer Line ◽  
Pure Hydrogen ◽  
Line Profiles ◽  
Stark Broadening ◽  
Echelle Spectrograph ◽  
Helium Spectra ◽  
Model Atom

Improved non-LTE model atmospheres designed for the analysis of very hot subluminous O stars are presented. The calculations are based on the new method of the accelerated lambda iteration (ALI) which proves capable of treating up to 100 levels of various ions. Presented here are improved calculations for (i) pure hydrogen model atmospheres including Stark broadening, (ii) for hydrogen- and helium-composed model atmospheres and (iii) first preliminary models which include in addition a detailed carbon model atom. These models remove an apparent mismatch of Balmer line profiles noted previously and fit high S/N, high-resolution hydrogen and helium spectra obtained with the ESO-Cassegrain echelle spectrograph very well.

scholarly journals The Structure of the Envelopes of Symbiotic Novae

1990 ◽  
Vol 122 ◽  
pp. 431-432
Author(s):  
G.B. Baratta ◽  
A. Damineli Neto ◽  
C. Rossi ◽  
R. Viotti
Keyword(s):  
High Resolution ◽  
Uv Spectra ◽  
Emission Lines ◽  
Broad Line ◽  
Line Profiles ◽  
Composite Spectrum ◽  
Multiple Structure ◽  
Broad Emission ◽  
Light History

Symbiotic novae are composite spectrum stars whose light history is characterized by one single major outburst. At high resolution their optical and UV spectra are very rich of emission lines belonging to a wide ionization range. Generally one can identify both narrow and broad line systems. The latter includes emission lines with multiple structure, broad emission wings, WR features, and P Cygnl lines. Frequently the broad line profiles are largely variable with time. They should be associated with the major stellar outburst. An overview of the problem with extensive references can be found in Viotti (1989).

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