scholarly journals Statistics of Double and Multiple Stars in the Solar Neighborhood

1992 ◽  
Vol 135 ◽  
pp. 343-345
Author(s):  
Victor V. Orlov ◽  
Oleg A. Titov
Keyword(s):  
Physical Properties ◽  
Luminosity Function ◽  
Solar Neighborhood ◽  
Solar Neighbourhood ◽  
Stellar Systems ◽  
Additional Peak ◽  
Multiple Stars ◽  
Double And Multiple Stars ◽  
Absolute Magnitudes ◽  
Machine Readable

AbstractWe study the multiplicity function and physical properties of single, double, and multiple stellar systems in the solar neighbourhood (r < 10 pc), using a new preliminary machine–readable version of the Gliese & Jahreiss Catalogue (1991).The ratio of (n+l)-ple to n-ple systems is a constant fraction of about 1/4 for n =1, 2, 3, 4. The luminosity function f(M) for primaries in binaries has an additional peak at M є (6m,8m) that is absent in f(M) for single stars and secondary components. A significant correlation between the absolute magnitudes M1 and M2 of the components in binaries takes place.

scholarly journals Dynamic study of possible host stars for extrasolar planetary systems

2014 ◽  
Vol 9 (S310) ◽  
pp. 104-105 ◽  
Author(s):  
N. A. Shakht ◽  
L. G. Romanenko ◽  
D. L. Gorshanov ◽  
O. O. Vasilkova
Keyword(s):  
Planetary Systems ◽  
Dynamic Study ◽  
Stellar Systems ◽  
The Sun ◽  
Solar Mass ◽  
Double Stars ◽  
Multiple Stars ◽  
Double And Multiple Stars ◽  
Host Stars

AbstractWe present the stellar systems which consist of double and multiple stars with distances 3.5 ÷ 25 pc from the Sun, belonging to spectral classes F, G, K, M, having masses from 0.3 to 1.5 solar mass and can, in principle, possess planetary systems. On the basis of observations with Pulkovo 65 cm refractor the relative positions of double stars, the parameters of motion, the orbits and also the ephemeris for the nearest epochs have been computed.

scholarly journals On Utmost Multiplicity of Hierarchical Stellar Systems

2016 ◽  
Vol 25 (4) ◽  
Author(s):  
Y. M. Gebrehiwot ◽  
D. A. Kovaleva ◽  
A. Yu. Kniazev ◽  
O. Yu. Malkov ◽  
N. A. Skvortsov ◽  
...  
Keyword(s):  
High Multiplicity ◽  
Stellar Systems ◽  
Hierarchical Systems ◽  
Orbital Parameters ◽  
Multiple Stars ◽  
Component Systems ◽  
Double And Multiple Stars ◽  
Theoretical Considerations ◽  
Very High ◽  
Cross Match

AbstractAccording to theoretical considerations, multiplicity of hierarchical stellar systems can reach, depending on masses and orbital parameters, several hundred, while observational data confirm the existence of at most septuple (seven-component) systems. In this study, we cross-match the stellar systems of very high multiplicity (six and more components) in modern catalogues of visual double and multiple stars to find among them the candidates to hierarchical systems. After cross-matching the catalogues of closer binaries (eclipsing, spectroscopic, etc.), some of their components were found to be binary/multiple themselves, what increases the system's degree of multiplicity. Optical pairs, known from literature or filtered by the authors, were flagged and excluded from the statistics. We compiled a list of hierarchical systems with potentially very high multiplicity that contains ten objects. Their multiplicity does not exceed 12, and we discuss a number of ways to explain the lack of extremely high multiplicity systems.

scholarly journals Observed Relations Between Physical Properties and MK Classification as Functions of Metal Abundance for F5-K4 Stars

1976 ◽  
Vol 72 ◽  
pp. 75-78
Author(s):  
M. Grenon
Keyword(s):  
Physical Properties ◽  
Spectral Range ◽  
Spectral Type ◽  
Photometric System ◽  
Luminosity Class ◽  
Empirical Relations ◽  
Metal Abundance ◽  
Systematic Effects ◽  
The Absolute ◽  
Absolute Magnitudes

The Geneva photometric system has been calibrated in terms of [M/H], θeff, Mv in the spectral range F5 to K4. As the spectral type is a datum generally available, we derive empirical relations showing the coupling of θeff and [M/H] at given spectral type and luminosity class. Similar relations are offered for the absolute magnitudes and provide a more accurate means for deriving spectroscopic parallaxes. Systematic effects on the estimation of the luminosity class are also shown.

scholarly journals The Hipparcos Double and Multiple Star Solutions

1998 ◽  
Vol 11 (1) ◽  
pp. 539-541
Author(s):  
F. Mignard
Keyword(s):  
Detailed Data ◽  
Multiple Star ◽  
Multiple Systems ◽  
Multiple Stars ◽  
Different Types ◽  
Hipparcos Catalogue ◽  
Double And Multiple Stars

Abstract The Hipparcos Catalogue provides general astrometric and photometric information on double and multiple stars in specific fields of the main Catalogue and detailed data on the components in the various sections of a dedicated annex: the Double and Multiple Systems Annex (DMSA). Overall statistics of these solutions are presented for the 13211 entries of this annex and the different types of solutions are outlined.

scholarly journals Multicolour CCD measurements of visual double and multiple stars. III

2007 ◽  
Vol 464 (2) ◽  
pp. 641-645 ◽  
Author(s):  
P. Lampens ◽  
A. Strigachev ◽  
D. Duval
Keyword(s):  
Multiple Stars ◽  
Double And Multiple Stars

scholarly journals The Luminosity Function of White Dwarfs in the Local Disk and Halo

1989 ◽  
Vol 114 ◽  
pp. 15-23 ◽  
Author(s):  
James Liebert ◽  
Conard C. Dahn ◽  
David G. Monet
Keyword(s):  
White Dwarfs ◽  
Luminosity Function ◽  
Solar Neighborhood ◽  
Star Formation History ◽  
Empirical Estimates ◽  
Formation History ◽  
History Of ◽  
Cool White Dwarfs ◽  
Local Disk

The luminosity function (LF) and total space density of white dwarfs in the solar neighborhood contain important information about the star formation history of the stellar population, and provide an independent method of measuring its age. The first empirical estimates of the LF for degenerate stars were those of Weidemann (1967), Kovetz and Shaviv (1976) and Sion and Liebert (1977). The follow-up investigations made possible by the huge Luyten Palomar proper motion surveys, however, added many more faint white dwarfs to the known sample. While the number of known cool white dwarfs grew to nearly one hundred, these did not include any that were much fainter intrinsically than the coolest degenerates found from the early Luyten, van Biesbroeck and Eggen-Greenstein lists.

Double and Multiple Stars

1988 ◽  
pp. 253-256
Author(s):  
K. D. Rakos ◽  
H. A. McAlister ◽  
H. A. Abt ◽  
P. Couteau ◽  
J. Dommanget ◽  
...  
Keyword(s):  
Multiple Stars ◽  
Double And Multiple Stars
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