Stellar Multiplicity

By G. Duchêne, A. Berkeley, Institut de Plan'etologie et d'Astrophysique de Grenoble, Harvard-Smithsonian Cfa. 2013

978 citations recorded by the source corpus.

Stellar multiplicity is an ubiquitous outcome of the star formation process. Characterizing the frequency and main characteristics of multiple systems and their dependencies on primary mass and environment is therefore a powerful tool to probe this process. While early attempts were fraught with selection biases and limited completeness, instrumentation breakthroughs in the last two decades now enable robust analyses. In this review, we summarize our current empirical knowledge of stellar multiplicity for Main Sequence stars and brown dwarfs, as well as among populations of Pre-Main Sequence stars and embedded protostars. Clear trends as a function of both primary mass and stellar evolutionary stage are identified that will serve as a comparison basis for numerical and analytical models of star formation.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2897c9ac98785289b19220e4aa634f90850d2421

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In Astronomy and Astrophysics

1. Timothy Morton
2. D. Charbonneau
3. Michela Mapelli
4. Jon Fortney
5. A. Mann
6. E. Gaidos
7. A. Kraus
8. F. Antonini

Citations in the corpus

• SURVEYING THE BRIGHT STARS BY OPTICAL INTERFEROMETRY. I. A SEARCH FOR MULTIPLICITY AMONG STARS OF SPECTRAL TYPES F-K (2016, background): “Since it is known that almost all binaries with periods this short have circular orbits as a result of tidal dissipation (Raghavan et al. 2010; Duchêne & Kraus 2013), it is likely that they would have been detectable unless viewed at inclinations i60°.”
• The Solar Neighborhood. XLV. The Stellar Multiplicity Rate of M Dwarfs Within 25 pc (2019, background): “The dot-dash line indicates a peak at 4 AU for the 10 pc sub-sample, which is very close to the peaks reported above in Janson et al. (2014a); Duchêne & Kraus (2013).”
• Greatly Enhanced Merger Rates of Compact-object Binaries in Non-spherical Nuclear Star Clusters (2017, result): “This choice is consistent with the observed mass ratios of massive binary stars (Duchêne & Kraus 2013; Sana et al. 2012; Kobulnicky et al. 2014).”
• Lidov–Kozai Cycles with Gravitational Radiation: Merging Black Holes in Isolated Triple Systems (2016, result): “This distribution is roughly consistent with the curve shown in Figure 3 of the review by Duchêne & Kraus (2013), showing results from the literature for the eccentricities of massive stellar binaries.”
• TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26 (2021, background): “At the same time, there are many open questions that remain; for example, what mechanism (or combination of mechanisms) drives multiplicity rates (Duchêne & Kraus 2013), what determines the distribution of mass ratios (Wells & Prša 2021), how does (close) binarity affect stellar evolution of stars…”
• Unresolved stellar companions with Gaia DR2 astrometry (2020, background): “It is now established that O and B stars are much more likely to reside in a pair compared to stars further down the main sequence (MS; see Garmany, Conti & Massey 1980; Raghavan et al. 2010; Sana et al. 2012; Duchêne & Kraus 2013; Moe & Di Stefano 2017).”
• OBSERVATIONS OF HIERARCHICAL SOLAR-TYPE MULTIPLE STAR SYSTEMS (2015, background): “The latest results on binary statistics are reviewed by Duchêne & Kraus (2013).”
• Searching for faint companions with VLTI/PIONIER - II. 92 main sequence stars from the Exozodi survey (2014, background): “Historically, many dedicated studies have been carried out to quantify the number of binaries in the solar neighbourhood, showing higher multiplicity rates around more massive stars (see Duchêne & Kraus 2013, for a recent review).”
• THE GALACTIC O-STAR SPECTROSCOPIC SURVEY (GOSSS). II. BRIGHT SOUTHERN STARS (2013, background): “To our knowledge, the second value is the highest binary fraction ever measured for a large sample of massive stars20 Compared to the results reviewed by Duchêne & Kraus (2013), the SB multiplicity frequency for high-mass stars is on the low side of their value (70 ± 9”
• Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, background): “The initial mass of the primary star is taken from a broken power law IMF: ∝M−1.3 for 0.08 ≤ M < 0.5 M , ∝M−2.2 for 0.5 ≤ M < 1.0 M , and ∝M−2.3 for 1.0 ≤ M ≤ 150 M (Kroupa 2001; Bastian et al. 2010; Duchêne & Kraus 2013).”
• DOUBLE COMPACT OBJECTS. III. GRAVITATIONAL-WAVE DETECTION RATES (2015, neutral): “In field populations about 10%–30% of binaries are, in fact, triples (or higher multiples; e.g., Kiminki & Kobulnicky 2012; Kiminki et al. 2012; Duchêne & Kraus 2013) and Kozai–Lidov effects or dynamical instabilities (Perets & Kratter 2012) may lead to the merger of wide BH– BH binaries.”
• The Close Binary Fraction of Solar-type Stars Is Strongly Anticorrelated with Metallicity (2018, background): “…how the close binary fraction varies with primary mass, metallicity, age, and environment provides significant insight into the processes of protobinary fragmentation, accretion, and orbital migration (Kratter et al. 2008, 2010a; Duchêne & Kraus 2013; Moe & Di Stefano 2017; Moe & Kratter 2018).”
• Prospects for detection of detached double white dwarf binaries with Gaia, LSST and LISA (2017, methodology): “For intermediate-mass stars, the value of b ranges between 0 and −1 (Duchêne & Kraus 2013).”
• RADIATION MAGNETOHYDRODYNAMIC SIMULATIONS OF PROTOSTELLAR COLLAPSE: NONIDEAL MAGNETOHYDRODYNAMIC EFFECTS AND EARLY FORMATION OF CIRCUMSTELLAR DISKS (2015, background): “Obviously, this problem cannot be real because many protoplanetary disks and extrasolar planets have been observed, and because the fraction of binaries or multiples is known to be high (e.g., Raghavan et al. 2010; Duchêne & Kraus 2013).”
• Imaging Extrasolar Giant Planets (2016, background): “Roughly 20% of brown dwarfs are close binaries with separation distributions peaking near 4.5 AU and mass ratios approaching unity (e.g., Burgasser et al. 2007; Kraus & Hillenbrand 2012; Duchêne & Kraus 2013).”
• Binary Companions of Evolved Stars in APOGEE DR14: Search Method and Catalog of ∼5000 Companions (2018, background): “…star systems are of great interest in astrophysics: the population of stars and their companions encodes information about star formation processes, stellar parameters and evolution, and the dynamics of multi-body systems (for recent reviews, see Duchêne & Kraus 2013; Moe & Di Stefano 2017).”
• Binary Black Hole Mergers from Field Triples: Properties, Rates, and the Impact of Stellar Evolution (2017, result): “This choice is consistent with observations of massive binary stars which indicate a nearly flat distribution of the mass ratio (e.g., Sana et al. 2012; Duchêne & Kraus 2013; Kobulnicky et al. 2014).”
• Abundance Estimates for 16 Elements in 6 Million Stars from LAMOST DR5 Low-Resolution Spectra (2019, background): “Binary and multiple star systems About half of the stars are expected to be in binary or multiple systems (see e.g., Duchêne & Kraus 2013; Gao et al. 2014; Yuan et al. 2015b).”
• THE VLA NASCENT DISK AND MULTIPLICITY SURVEY OF PERSEUS PROTOSTARS (VANDAM). II. MULTIPLICITY OF PROTOSTARS IN THE PERSEUS MOLECULAR CLOUD (2016, methodology): “Duchêne & Kraus (2013) presented a combined analysis of Connelley et al. (2009) and Duchêne et al. (2007) to derive a CSF of 0.35±0.05 for Class I sources with separations between 50 and 2000 au.”