Cited by 325Astrophysics and Star Formation StudiesStellar, planetary, and galactic studiesGalaxies: Formation, Evolution, Phenomena

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MAPPING THE SHORES OF THE BROWN DWARF DESERT. II. MULTIPLE STAR FORMATION IN TAURUS-AURIGA

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Kraus, Adam L., Ireland, Michael J., Martinache, Frantz, Hillenbrand, Lynne A.·2011·The Astrophysical Journal

DOI 10.1088/0004-637x/731/1/8

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Abstract

We have conducted a high-resolution imaging study of the Taurus–Auriga star-forming region in order to characterize the primordial outcome of multiple star formation and the extent of the brown dwarf desert. Our survey identified 16 new binary companions to primary stars with masses of 0.25–2.5 M ☉ , raising the total number of binary pairs (including components of high-order multiples) with separations of 3–5000 AU to 90. We find that ∼2/3–3/4 of all Taurus members are multiple systems of two or more stars, while the other ∼1/4–1/3 appear to have formed as single stars; the distribution of high-order multiplicity suggests that fragmentation into a wide binary has no impact on the subsequent probability that either component will fragment again. The separation distribution for solar-type stars (0.7–2.5 M ☉ ) is nearly log-flat over separations of 3–5000 AU, but lower-mass stars (0.25–0.7 M ☉ ) show a paucity of binary companions with separations of ≳200 AU. Across this full mass range, companion masses are well described with a linear-flat function; all system mass ratios ( q = M B / M A ) are equally probable, apparently including substellar companions. Our results are broadly consistent with the two expected modes of binary formation (free-fall fragmentation on large scales and disk fragmentation on small scales), but the distributions provide some clues as to the epochs at which the companions are likely to form.

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Sorted by citations

Stellar Multiplicity
Duchêne, G., & Kraus, A. L. (2013) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081710-102602 · Cited by 1,353
“The latter conclusion also matches the results of Kouwenhoven et al. (2007b) for intermediate-mass multiple systems in Upper Scorpius.”
BackgroundMethodInfluentialSelf-citation
Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars
Moe, M., & Stefano, R. D. (2017) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aa6fb6 · Cited by 1,292
“…have also concluded that the statistics of solar-type binaries in open clusters are indistinguishable from those in the field for a broad range of cluster densities and ages τ ≈ 3 Myr - 7 Gyr (Bouvier et al. 1997; Köhler et al. 2006; Kraus et al. 2011; Geller & Mathieu 2012; King et al. 2012).”
BackgroundMethodInfluential
THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS
Andrews, S., Rosenfeld, K., Kraus, A., & Wilner, D. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/771/2/129 · Cited by 400
“The infrared-selected Luhman et al. catalog of Tau-Aur Class II sources is used as the basis of our sample: it includes 179 young stellar “systems” composed of 227 (known) individual stars with spectral types from B8 to M9 (e.g., Luhman 2000, 2004; Kraus et al. 2011).”
MethodSelf-citation
Gravitational Instabilities in Circumstellar Disks
Kratter, K. M., & Lodato, G. (2016) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081915-023307 · Cited by 528
“On the contrary, Kraus et al. (2011) find that for young stars in Taurus, the lower mass objects M∗ < 0.7M typically have companions with smaller separations consistent with disk fragmentation (< 100AU ,) whereas stars with 0.7M < M∗ < 2.5M have more companions at larger separations.”
Background
Stellar, brown dwarf and multiple star properties from a radiation hydrodynamical simulation of star cluster formation
Bate, M. R. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19955.x · Cited by 535

See all 325

Authors: Kraus, A. L., Ireland, M. J., Martinache, F., & Hillenbrand, L. A.
Affiliations: University of Hawaiʻi at Mānoa (US)
The University of Sydney (AU)
National Astronomical Observatory of Japan (JP)
California Institute of Technology (US)
ORCID: Ireland, Michael J.
Martinache, Frantz
Venue: The Astrophysical Journal
Publisher: American Astronomical Society
Published: 2011-03-17
Volume: 731
Issue: 1
Pages: 8
ISSN: 0004-637X (ISSN-L)
1538-4357
DOI: 10.1088/0004-637x/731/1/8
OpenAlex: W1996452021
Semantic Scholar: d9092295d91fdf71df1f34481bdbff65a7fb02f1
Cited by: 325
References: 133
Citations by year: 2026: 4 · 2025: 7 · 2024: 16 · 2023: 12 · 2022: 17 · 2021: 16 · 2020: 22 · 2019: 37 · 2018: 19 · 2017: 24 · 2016: 28 · 2015: 28 · 2014: 21 · 2013: 33 · 2012: 25
FWCI: 16.14
Type: journal article
Language: en
Open access: bronze
doi.org
Locations: The Astrophysical Journal (publishedVersion)
arXiv (Cornell University) (submittedVersion)
CaltechAUTHORS (California Institute of Technology) (submittedVersion)
ANU Open Research (Australian National University) (submittedVersion)
arXiv (Cornell University)
Funders: National Science Foundation (NAS 5-26555)
National Aeronautics and Space Administration (NAS 526555, 526555)
California Institute of Technology
Space Telescope Science Institute (NAS5- 26555, 5-26555, 26555)
U.S. Naval Observatory (NAS 5-26555)
Topics: Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Keywords: brown dwarf desert, multiple star formation, Taurus-Auriga star-forming region, binary companion, binary separation distribution, disk fragmentation, substellar companions

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MAPPING THE SHORES OF THE BROWN DWARF DESERT. II. MULTIPLE STAR FORMATION IN TAURUS-AURIGA

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