scholarly journals The Mass Ratio Distribution in Main‐Sequence Spectroscopic Binaries Measured by Infrared Spectroscopy

2003 ◽  
Vol 599 (2) ◽  
pp. 1344-1356 ◽  
Author(s):  
T. Mazeh ◽  
M. Simon ◽  
L. Prato ◽  
B. Markus ◽  
S. Zucker
Keyword(s):  
Infrared Spectroscopy ◽  
Main Sequence ◽  
Spectroscopic Binaries ◽  
Mass Ratio ◽  
Ratio Distribution

scholarly journals Statistical Properties of an Unbiased Sample of F7-K Binaries: Towards The Long-Period Systems

2004 ◽  
Vol 191 ◽  
pp. 28-32 ◽  
Author(s):  
A. Eggenberger ◽  
J.-L. Halbwachs ◽  
S. Udry ◽  
M. Mayor
Keyword(s):  
Main Sequence ◽  
Equal Mass ◽  
Statistical Properties ◽  
Spectroscopic Binaries ◽  
Mass Ratio ◽  
Long Period ◽  
Period Distribution ◽  
Solar Type ◽  
Flat Distribution ◽  
Visual Binaries

AbstractWe have undertaken a new investigation of the statistical properties of main-sequence binaries, which is a revision and extension of the Duquennoy & Mayor survey of solar-type stars. The analysis has been divided into two parts: the spectroscopic binaries with periods shorter than 10 years, and the long-period systems including visual binaries and common proper motion pairs. In this contribution we present preliminary results regarding the intrinsic mass ratio and period distributions of visual binaries. Our results are strongly limited by small-number statistics, but when combined with the ones found for the spectroscopic binaries, the following results are obtained: (i) the excess of equal-mass binaries, if still present, is less important for long-period systems than for the binaries with P < 50 days; (ii) the period distribution is inconsistent with a flat distribution.

On the mass-ratio distribution of spectroscopic binaries with solar-type primaries

1992 ◽  
Vol 401 ◽  
pp. 265 ◽  
Author(s):  
Tsevi Mazeh ◽  
Dorit Goldberg ◽  
Antoine Duquennoy ◽  
Michel Mayor
Keyword(s):  
Spectroscopic Binaries ◽  
Mass Ratio ◽  
Ratio Distribution ◽  
Solar Type

On the Mass‐Ratio Distribution of Spectroscopic Binaries

2003 ◽  
Vol 591 (1) ◽  
pp. 397-405 ◽  
Author(s):  
Dorit Goldberg ◽  
Tsevi Mazeh ◽  
David W. Latham
Keyword(s):  
Spectroscopic Binaries ◽  
Mass Ratio ◽  
Ratio Distribution

The mass-ratio distribution of spectroscopic binaries along the main-sequence

2017 ◽  
Vol 12 (S330) ◽  
pp. 339-340
Author(s):  
Henri M. J. Boffin ◽  
Dimitri Pourbaix
Keyword(s):  
Spectral Type ◽  
Binary Systems ◽  
Large Fraction ◽  
Close Binary System ◽  
Spectroscopic Binaries ◽  
Close Binary ◽  
Mass Ratio ◽  
Primary Star ◽  
Ratio Distribution ◽  
One Step

AbstractBinarity is now a well-established quality affecting a large fraction of stars, and recent studies have shown that the fraction of binaries is a function of the spectral type of the primary star, with most massive stars being member of a close binary system. By cross-matching TGAS with SB9, we went one step further and derived the mass ratio distribution of binary systems as a function of the spectral type of the primary star. This, combined with the binary fraction, provides very strong constraints on star formation and critical input for stellar population models.

scholarly journals The Mass–Ratio Distribution of Short–Period Binaries

1992 ◽  
Vol 135 ◽  
pp. 119-126 ◽  
Author(s):  
T. Mazeh ◽  
D. Goldberg
Keyword(s):  
Numerical Simulations ◽  
Mass Distribution ◽  
Classical Method ◽  
Spectroscopic Binaries ◽  
Mass Ratio ◽  
Linear Mass ◽  
Ratio Distribution ◽  
Long Period ◽  
Short Period ◽  
True Mass

Abstract We present a new algorithm to derive the mass-ratio distribution of an observed sample of spectroscopic binaries. The algorithm replaces each binary of unknown inclination by an ensemble of virtual systems with a distribution of inclinations. We show that contrary to a widely held assumption the orientations of each virtual ensemble should not be distributed randomly in space. A few iterations are needed to find the true mass-ratio distribution. Numerical simulations clearly demonstrate the advantage of the new algorithm over the classical method. We have applied the new algorithm to the recent large sample of G-dwarf spectroscopic binaries, and got a uniform or perhaps a slightly rising linear mass-ratio distribution. This result suggests that the mass-ratio distributions of short-period and long-period binaries are substantially different. It also indicates that the mass distribution of the secondary stars is not the same as that of the single stars.

scholarly journals Arguments Indicating that Ap and Am Stars are Evolved Spectroscopic Binaries

1968 ◽  
Vol 1 ◽  
pp. 420-431
Author(s):  
E.P.J. van den Heuvel
Keyword(s):  
Spectroscopic Binaries ◽  
Mass Ratio ◽  
Helium Burning ◽  
Ratio Distribution ◽  
Hydrogen Burning ◽  
B Stars ◽  
Long Period ◽  
Galactic System ◽  
Roche Limit ◽  
Long Period Variables

Roughly three types of evolution of spectroscopic binaries may occur:Case (a): the primary fills its Roche limit already before the end of core hydrogen burning;Case (b): the primary fills its Roche limit after core hydrogen exhaustion but before the onset of helium burning, andCase (c): the primary does not fill its Roche limit before the end of core helium burning.Since long-period variables of Population I as well as Population II may reach radii of 10 AU, case (c) will occur in systems with periods up to 100 years. Since about 50% of the A and B stars are spectroscopic binaries, many evolved spectroscopic binaries are expected to occur in the galactic system. Computations show that, using the mass-ratio distribution of unevolved systems derived by Kuiper, the number of systems with one evolved component is expected to be at least as large as the number of unevolved systems, in the spectral regions A and B.

scholarly journals Tidal Circularization Among the Close Binaries in M67

1992 ◽  
Vol 151 ◽  
pp. 471-472
Author(s):  
David W. Latham ◽  
Robert D. Mathieu ◽  
Alejandra A. E. Milone ◽  
Robert J. Davis
Keyword(s):  
Main Sequence ◽  
Open Cluster ◽  
Radial Velocities ◽  
Spectroscopic Binaries ◽  
Close Binaries ◽  
To Come ◽  
Mirror Telescope

In 1971 Roger Griffin and Jim Gunn began monitoring the radial velocities of most of the members brighter than the main-sequence turnoff in the old open cluster M67, primarily using the 200-inch Hale Telescope. In 1982 the torch was passed to Dave Latham and Bob Mathieu, who began monitoring many of the same stars with the 1.5-meter Tillinghast Reflector and the Multiple-Mirror Telescope on Mt. Hopkins. We have successively combined these two sets of data, plus some additional CORAVEL velocities kindly provided by Michel Mayor, to obtain 20 years of time coverage (e.g. Mathieu et al. 1986). Among the stars brighter than magnitude V = 12.7 we have already published orbits for 22 spectroscopic binaries (Mathieu et al. 1990). At Mt. Hopkins an extension of this survey to many of the cluster members down to magnitude V = 15.5 has already yielded thirteen additional orbital solutions, with the promise of many more to come.

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