I. A Proposed Method for the Measurement and Reduction of Spectrograms for the Determination of the Radial Velocities of Celestial Objects.- II. Application to a Study of the Variable Star W Sagittarii

1904 ◽  
Vol 16 ◽  
pp. 243
Author(s):  
R. H. Curtiss
Keyword(s):  
Variable Star ◽  
Radial Velocities

On the Inhomogeneity of Chemical Composition over the Surface of 21 Per

1976 ◽  
Vol 32 ◽  
pp. 343-349
Author(s):  
Yu.V. Glagolevsky ◽  
K.I. Kozlova ◽  
V.S. Lebedev ◽  
N.S. Polosukhina
Keyword(s):  
Chemical Composition ◽  
Spectral Line ◽  
Variable Star ◽  
Radial Velocities ◽  
Crimean Astrophysical Observatory ◽  
Line Intensities ◽  
Magnetic Variable

SummaryThe magnetic variable star 21 Per has been studied from 4 and 8 Å/mm spectra obtained with the 2.6 - meter reflector of the Crimean Astrophysical Observatory. Spectral line intensities (Wλ) and radial velocities (Vr) have been measured.

A Proposed Method for the Determination of Radial Velocities of Stars

1906 ◽  
Vol 23 ◽  
pp. 148 ◽  
Author(s):  
George C. Comstock
Keyword(s):  
Radial Velocities

Note on the Determination of Radial Velocities of Nebulae

1913 ◽  
Vol 25 ◽  
pp. 288
Author(s):  
W. W. Campbell
Keyword(s):  
Radial Velocities

scholarly journals Formation Depths of Spectral Lines in Cepheids

1995 ◽  
Vol 155 ◽  
pp. 373-374
Author(s):  
Michael D. Albrow ◽  
P. L. Cottrell
Keyword(s):  
Spectral Line ◽  
Velocity Fields ◽  
Radial Velocities ◽  
Spectral Lines ◽  
Line Formation ◽  
Ionisation Potential ◽  
Velocity Gradients ◽  
Different Levels ◽  
Line Depth

There has been a number of observational programmes that have endeavoured to investigate the atmospheric velocity fields in Cepheids (e.g., Sanford 1956, Wallerstein et al. 1992, Butler 1993). These studies measured the radial velocities of lines of different strength, excitation and ionisation potential as these provide an indication of line formation at different levels in the atmosphere. From these measurements, the presence of velocity gradients can be inferred, but determination of the magnitude of such gradients requires knowledge of the spectral line depth of formation. Through dynamical modelling we are endeavouring to ascertain what is actually being measured in the above observational programmes.

scholarly journals A Determination of Secular Parallaxes of Reference Stars from Relative Proper Motions of Open Clusters

1970 ◽  
Vol 7 ◽  
pp. 74-76
Author(s):  
A. N. Deutsch
Keyword(s):  
Systematic Errors ◽  
Open Clusters ◽  
Radial Velocities ◽  
Proper Motions ◽  
The Mean

The determination of secular parallaxes of stars is usually based on meridian observations of proper motions of bright stars, this introducing known systematic errors. The mean parallaxes of stars can be obtained by means of radial velocities which are known for the bright stars. The more perspective method, the reference of stars to galaxies, is not applicable at low galactic latitudes.

A determination of the apex and velocity of the solar motion from radial velocities of stars of spectral type B

1924 ◽  
Vol 222 (8) ◽  
pp. 113-122
Author(s):  
B. Fessenkoff ◽  
C. Ogrodnikoff
Keyword(s):  
Spectral Type ◽  
Radial Velocities ◽  
Type B ◽  
Solar Motion

scholarly journals The rapid determination of radial velocities by a new projection method.

1946 ◽  
Vol 52 ◽  
pp. 48
Author(s):  
R. M. Petrie
Keyword(s):  
Projection Method ◽  
Rapid Determination ◽  
Radial Velocities

scholarly journals Periodical Variations in the Spectrum of X Persei. Discovery of a 22-Hr Period in the Variations of the Radial Velocities of Hα.

1980 ◽  
Vol 88 ◽  
pp. 367-373
Author(s):  
T. S. Galkina
Keyword(s):  
Emission Line ◽  
Variable Star ◽  
Radial Velocities ◽  
X Ray

The bright BOe star X Persei has been observed for over 50 years as an emission-line object and as a variable star. Throughout this time, the star displayed typical behavior for such an object. The discovery that it lies very close to the position of a weak X-ray source renewed interest in the star, which is now under close scrutiny. The probable association of X Persei with 3U 0352+30 has been subject to several discussions (Hutchings, Crampton and Redman, 1975; Margon, Bowyer, and Penegor, 1976; Hutchings and Walker 1976; Persi, Viotti and Ferrari-Toniolo 1977, 1978).

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