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

Mazeh, T.; Simon, M.; Prato, L.; Markus, B.; Zucker, S.

doi:10.1086/379346

Cited by 78 publications

(111 citation statements)

References 29 publications

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“…The narrow peak at q = 1 is reduced as compared with Söderhjelm (2000), because it is not seen by e.g. Mazeh et al (2003), or as a much broader feature by Halbwachs et al (2003). Its total contribution to the above f (q) is only about 6%, and it is relatively unimportant in the present study.…”

Section: Population Synthesis For Binariesmentioning

confidence: 49%

Eclipsing binary statistics – Theory and observation

Söderhjelm

Dischler

2005

A&A

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The expected distributions of eclipse-depth versus period for eclipsing binaries of different luminosities are derived from large-scale population synthesis experiments. Using the rapid Hurley et al. BSE binary evolution code, we have evolved several hundred million binaries, starting from various simple input distributions of masses and orbit-sizes. Eclipse probabilities and predicted distributions over period and eclipsedepth (P/∆m) are given in a number of main-sequence intervals, from O-stars to brown dwarfs. The comparison between theory and Hipparcos observations shows that a standard (Duquennoy & Mayor) input distribution of orbit-sizes (a) gives reasonable numbers and P/∆m-distributions, as long as the mass-ratio distribution is also close to the observed flat ones. A random pairing model, where the primary and secondary are drawn independently from the same IMF, gives more than an order of magnitude too few eclipsing binaries on the upper main sequence. For a set of eclipsing OB-systems in the LMC, the observed period-distribution is different from the theoretical one, and the input orbit distributions and/or the evolutionary environment in LMC has to be different compared with the Galaxy. A natural application of these methods are estimates of the numbers and properties of eclipsing binaries observed by large-scale surveys like Gaia.

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Section: Population Synthesis For Binariesmentioning

confidence: 49%

Eclipsing binary statistics – Theory and observation

Söderhjelm

Dischler

2005

A&A

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“…The brightest one is, in its turn, a double-lined spectroscopic binary discovered by Latham et al (1988) and confirmed by Goldberg et al (2002); the low-mass spectroscopic companion is labelled "E". Mazeh et al (2003) Carney et al (1994), which is inconsistent with the F8V spectral type and several effective temperature determinations of components A and E (e.g. Goldberg et al 2002).…”

Section: Wds 20599+4016 (Hd 200077 Ae-d and G 210-44 Ab)mentioning

confidence: 62%

Reaching the boundary between stellar kinematic groups and very wide binaries

Caballero¹

2009

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Aims. I look for and characterise very wide binaries and multiple systems with projected physical separations larger than s = 0.1 pc, which is generally believed to be a sharp upper limit to the distribution of wide binary semimajor axes. Methods. I investigated in detail 30 Washington double stars with angular separations of ρ > 1000 arcsec. I discarded 23 of them as probably unbound systems based on discordant astrometry, photometry, spectral types, and radial velocities. The remaining seven systems were subject to a comprehensive data compilation and derivation (multi-wavelength photometry, heliocentric distance, multiplicity, age, mass, metallicity, membership in a young kinematic group). Results. Of the seven very wide systems, six have projected physical separations greater than the hypothetical cutoff at s = 0.1 pc and four have separations s > 0.2 pc. Although there are two systems in young kinematic groups (namely HD 136654 and BD+32 2572 in the Hyades Supercluster, and AU Mic and AT Mic AB in the β Pictoris moving group), there is no clear prevalence of young systems (τ < 1 Ga) among these very wide binaries. Finally, I compare the binding energies of the seven systems with those of other weakly bound systems in the field.

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“…Their MRD also depends on the orbital period, since short period binaries (P < 50 days) include more systems with mass ratios of 0.8 or more. Mazeh et al (2003) reported infrared spectroscopic observations of a large well-defined sample of main-sequence, singlelined spectroscopic binaries to detect the secondaries and derive the mass ratio distribution of short-period binaries. Their sample consists of 51 Galactic disc spectroscopic binaries, with primary masses in the range 0.6-0.85 M .…”

Section: The Mrd Of Am Starsmentioning

confidence: 99%

A Renaissance study of Am stars

Boffin

2010

A&A

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Aims. Triggered by the study of Carquillat & Prieur (2007, MNRAS, 380, 1064 of Am binaries, I reanalyse their sample of 60 orbits to derive the mass ratio distribution (MRD), assuming as they did a priori functional forms, i.e. a power law or a Gaussian. The sample is then extended using orbits published by several groups and a full analysis of the MRD is made, without any assumption on the functional form. Methods. I derive the MRD using a Richardson-Lucy inversion method, assuming a fixed mass of the Am primary and randomly distributed orbital inclinations. Using the large sub-sample of double-lined spectroscopic binaries, I show that this methodology is indeed perfectly adequate. Results. I first derive new parameters of the functional form for the Carquillat & Prieur sample. Using the inversion method, applied to my extended sample of 162 systems, I find that the final MRD can be approximated by a uniform distribution.

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

Cited by 78 publications

References 29 publications

Eclipsing binary statistics – Theory and observation

Eclipsing binary statistics – Theory and observation

Reaching the boundary between stellar kinematic groups and very wide binaries

A Renaissance study of Am stars

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