On the study of the mass ratio of spectroscopic binaries

Mazeh, T.; Goldberg, D.

doi:10.1086/171611

Cited by 57 publications

(50 citation statements)

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“…The values of the upper panel of Figure 3 were derived by Goldberg (2000) with the algorithm of Mazeh & Goldberg (1992). Because many of the 577 stars have masses smaller than the mass of the larger mass bin, Goldberg (2000) used for that bin only the binaries found within a subsample of 312 stars, of the original 577 stars, and scaled the value of that bin accordingly.…”

Section: Analysis and Resultsmentioning

confidence: 99%

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Derivation of the Mass Distribution of Extrasolar Planets with MAXLIMA, a Maximum Likelihood Algorithm

Zucker

Mazeh

2001

ApJ

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We construct a maximum likelihood algorithm, MAXLIMA, to derive the mass distribution of the extrasolar planets when only the minimum masses are observed. The algorithm derives the distribution by solving a numerically stable set of equations and does not need any iteration or smoothing. Based on 50 minimum masses, MAXLIMA yields a distribution that is approximately Ñat in log M. The frequency drops o † very sharply as masses go higher than 10 although we suspect there is still a higher mass M J , tail that extends up to probably 20We estimate that 5% of the G stars in the solar neighborhood M J . have planets in the range 1È10 with periods shorter than 1500 days. For comparison we present the M J mass distribution of stellar companions in the range 100È1000 which is also approximately Ñat in M J , log M. The two populations are separated by the "" brown dwarf desert,ÏÏ a fact that strongly supports the idea that these are two distinct populations. Accepting this deÐnite separation, we point out the conundrum concerning the similarities between the period, eccentricity, and even mass distribution of the two populations.

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Section: Analysis and Resultsmentioning

confidence: 99%

“…The e †ect of the unknown inclination of spectroscopic binaries was studied by numerous investigators (e.g., Mazeh & Goldberg 1992 ;Heacox 1995 ;Goldberg 2000), assuming random orientation in space. Heacox (1995) calculates Ðrst the minimum mass distribution and then uses its relation to the mass distribution to derive the latter.…”

Section: Introductionmentioning

confidence: 99%

Derivation of the Mass Distribution of Extrasolar Planets with MAXLIMA, a Maximum Likelihood Algorithm

Zucker

Mazeh

2001

ApJ

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“…Within the range 0.15 < q < 0.6, the obtained MRD is not very different from a uniform distribution. The deficiency of systems with q < 0.15 is due to a combination of observational bias and a bias of the inversion method (see, e.g., Mazeh & Goldberg 1992;Heacox 1995).…”

Section: Single-lined Binariesmentioning

confidence: 99%

“…Figure 8 shows that the real issue in obtaining the final MRD of the Am binaries is to establish the correct relative fraction of SB1 and SB2. Observational biases could influence this ratio, such as the Öpik or Branch effect (AL85), and it is not an easy task to disentangle those (Mazeh & Goldberg 1992). However, as the current sample is a collection of several samples, which seem to complement each other very well and which must all have been affected in different -hopefully opposite -ways, and as they were not magnitude limited, I think it is reasonable that the sample is well representative and the conclusions on the MRD should be secure.…”

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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“…1 we show the correlation between separation and mass ratio for the two samples of Fischer & Marcy (1992) (open triangles) and of Close et al (2003) (closed triangles), including only resolved binaries, for which the mass ratio can be reliably determined (see discussion in Mazeh & Goldberg 1992). In the Fischer & Marcy (1992) sample, a slight tendency of having lower q for wider systems can be seen, in agreement with the conclusion of Mazeh & Goldberg (1992) for higher mass primaries. On the other hand, the Close et al (2003) sample shows a shortage of systems with large separation, even if very few systems with separations larger than 10 au have also been found (Luhman 2004; Phan‐Bao et al 2005).…”

Section: Is 2m1207 a ‘Binary‐like’ Or A ‘Planet‐like’ System?mentioning

confidence: 99%

Constraints on the formation mechanism of the planetary mass companion of 2MASS 1207334-393254

Lodato

Delgado-Donate

Clarke

2005

Monthly Notices of the Royal Astronomical Society: Letters

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In this paper we discuss the nature and the possible formation scenarios of the companion of the brown dwarf 2MASS 1207334‐393254. We initially discuss the basic physical properties of this object and conclude that, although from its absolute mass (5MJup) it is a planetary object, in terms of its mass ratio q and of its separation a with respect to the primary brown dwarf, it is consistent with the statistical properties of binaries with higher primary mass. We then explore the possible formation mechanism for this object. We show that the standard planet formation mechanism of core accretion is far too slow to form this object within 10 Myr, the observed age of the system. On the other hand, the alternative mechanism of gravitational instability (proposed both in the context of planet and of binary formation) may, in principle, work and form a system with the observed properties.

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On the study of the mass ratio of spectroscopic binaries

Cited by 57 publications

References 0 publications

Derivation of the Mass Distribution of Extrasolar Planets with MAXLIMA, a Maximum Likelihood Algorithm

Derivation of the Mass Distribution of Extrasolar Planets with MAXLIMA, a Maximum Likelihood Algorithm

A Renaissance study of Am stars

Constraints on the formation mechanism of the planetary mass companion of 2MASS 1207334-393254

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