Towards multiple-star population synthesis

By P. Eggleton. 2009

318 citations recorded by the source corpus.

The multiplicities of stars, and some other properties, were collected recently by Eggleton & Tokovinin, for the set of 4559 stars with Hipparcos magnitude brighter than 6.0 (4558 excluding the Sun). In this paper I give a numerical recipe for constructing, by a Monte Carlo technique, a theoretical ensemble of multiple stars that resembles the observed sample. Only multiplicities up to eight are allowed; the observed set contains only multiplicities up to seven. In addition, recipes are suggested for dealing with the selection effects and observational uncertainties that attend the determination of multiplicity. These recipes imply, for example, that to achieve the observed average multiplicity of 1.53, it would be necessary to suppose that the real population has an average multiplicity slightly over 2.0. This numerical model may be useful for (i) comparison with the results of star and star cluster formation theory, (ii) population synthesis that does not ignore multiplicity above 2 and (iii) initial conditions for dynamical cluster simulations.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/f7bba63c1b874be28d2b2e2f4edae1c9c7982b9c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. D. Charbonneau
2. J. Winn
3. Timothy Morton
4. C. Dressing
5. D. Deming
6. T. Mazeh
7. A. Tokovinin
8. D. Fabrycky

In Instrumentation

1. D. Charbonneau
2. Timothy Morton
3. J. Winn
4. C. Dressing
5. A. Tokovinin
6. D. Fabrycky
7. D. Latham
8. D. Deming

In Statistical and Nonlinear Physics

1. D. Charbonneau
2. J. Winn
3. C. Dressing
4. D. Latham
5. Eric Mamajek
6. Timothy Morton
7. P. McCullough
8. D. Fabrycky

Citations in the corpus

• Stellar Multiplicity (2013, methodology): “This distribution resembles the geometric distribution seen for the field (Section 3.1.5; Eggleton & Tokovinin 2008).”
• New constraints on the multiplicity of massive young stars in Upper Scorpius (2015, unknown): “(1) MSC, Tokovinin (1997); (2) BSC, Eggleton & Tokovinin (2008); (3) Harmanec (1987); (4) North et al. (2007); (5) Kouwenhoven et al. (2007); (6) Levato et al. (1987); (7) Batten et al. (1989); (8) McAlister et al. (1990); (9) Andersen & Nordstrom (1983); (10) Lafrenière et al. (2014). planned for t”
• THE TRANSITING EXOPLANET SURVEY SATELLITE: SIMULATIONS OF PLANET DETECTIONS AND ASTROPHYSICAL FALSE POSITIVES (2015, methodology): “For the systems that are designated as triples, we assign the properties using the approach originally suggested by Eggleton (2009).”
• DISCOVERY OF A FAINT COMPANION TO ALCOR USING MMT/AO 5 μm IMAGING (2009, methodology): “In comparing the Mizar-Alcor sextuplet to the known multiple star population (Tokovinin 1997; Eggleton & Tokovinin 2008), it appears that that Mizar-Alcor (d ≃ 25 pc) is the 2nd known closest multiple system with 6 (or more) components after Castor (d ≃ 16 pc).”
• Unique sextuple system: 65 Ursae Majoris (2012, background): “Nevertheless, 65 UMa is a rather unusual system, we presently know of only 11 other sextuple systems (see Eggleton & Tokovinin 2008).”
• VERY WIDE BINARIES AND OTHER COMOVING STELLAR COMPANIONS: A BAYESIAN ANALYSIS OF THE HIPPARCOS CATALOGUE (2010, background): “The Astrophysical Journal Supplement Series, 192:2 (17pp), 2011 January Shaya & Olling of catalogs of field binaries are very seriously affected by selection effects (Hogeveen 1990; Olling 2005; Kouwenhoven 2006; Eggleton & Tokovinin 2008; Kouwenhoven et al. 2009).”
• FROM BINARIES TO MULTIPLES. II. HIERARCHICAL MULTIPLICITY OF F AND G DWARFS (2014, methodology): “In this second approach, adopted e.g. by Eggleton (2009), the model has to be elaborated by trial and error.”
• KEPLER-413B: A SLIGHTLY MISALIGNED, NEPTUNE-SIZE TRANSITING CIRCUMBINARY PLANET (2014, background): “Eggleton and Tokovinin (2008) find that ∼ 25% of all multiple systems with a solar-type star are triples and higher order.”
• SURVEYING THE BRIGHT STARS BY OPTICAL INTERFEROMETRY. I. A SEARCH FOR MULTIPLICITY AMONG STARS OF SPECTRAL TYPES F-K (2016, background): “Eggleton & Tokovinin (2008) presented a catalog of bright, multiple (two or more components) star systems and discussed the implications of multiplicity for several topics in astrophysics.”