Note on the Determination of Radial Velocities of Nebulae

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

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

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 The Status of Absolute Proper Motions and the Kinematics of Globular Clusters

1995 ◽  
Vol 164 ◽  
pp. 406-406 ◽  
Author(s):  
M. Geffert ◽  
B. Dauphole ◽  
J. Colin ◽  
M. Odenkirchen ◽  
H.-J. Tucholke ◽  
...  
Keyword(s):  
Globular Clusters ◽  
Radial Velocities ◽  
Proper Motions ◽  
Preliminary Results ◽  
Space Motion ◽  
The Status ◽  
Galactic Potentials ◽  
Total Energies

We have studied a sample of 26 globular clusters for which so far absolute proper motions exist in the literature. The proper motions were combined with distances and radial velocities for a determination of the space motion of the clusters. Using different galactic potentials (see Dauphole & Colin 1994 and references therein) we calculated the orbits of the globular clusters and their time averaged eccentricities, total energies, and apo- and perigalactic distances. The relation of the orbital quantities to the metallicities of the globular clusters has been studied. Preliminary results of this study were presented in Geffert et al. (1993).

scholarly journals Determination of the double galaxies masses by the “timing argument” method

2018 ◽  
pp. 6-10
Author(s):  
Yu. Kudrya
Keyword(s):  
Dark Matter ◽  
Milky Way ◽  
Radial Velocities ◽  
Local Volume ◽  
Rotational Moment ◽  
Wide Pairs ◽  
Wide Range ◽  
The Masses ◽  
Stellar Masses

The possibilities of application of the “timing argument” (ТА) method to the physical pairs of galaxies that differ from the pair M31 – Milky Way are considered. We confine ourselves to pairs in the Local volume, imposing the additional isolation conditions on candidates for inclusion in the sample. The method was supplemented by the manner of taking into account the nonparallel- ism of the radial velocities of galaxies of close (wide) pairs. For the fourteen physical galaxy pairs (see a list in Tables) of the Local volume galaxies their ТА masses, including masses of dark matter, were estimated. The ratio χ of the mass of pairs to the sum of stellar masses was obtained in wide range from 0.5 to 4000. In some cases (KPG-40, KM-94, J0742+16, J1303-17, J1315+47) the masses estimated by TA are in agreement with popular estimates of χ. For whole sample, taking into account such variance of χ values it is difficult to make certain conclusions regarding its physical causes. Most likely, the TA model in the majority of the cases considered can not be used, pairs of general considerations can have a relative rotational moment.

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