The DOI matches its Crossref record; 133 of the 133 references it cites were found in a registry or an index.
MAPPING THE SHORES OF THE BROWN DWARF DESERT. II. MULTIPLE STAR FORMATION IN TAURUS-AURIGA
Open accessAbstract
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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“The multiplicity of class I young stellar objects (YSOs) in embedded clusters and pre-MS stars in young associations is high and ranges from 20% to 60% for the ∼10 1.5 -10 2.5 AU separation range and mass ratios of ∼0.1-1”
From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Kraus et al. 2011
Experimental — accuracy not yet measuredThe source backs part of the claim, not all of it — or backs it for a different population, condition or comparison.
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“The number of binaries is flat in log period or semi-major axis space (Halbwachs et al. 2003;Kraus et al. 2011), and young binaries are similar to field population in this respect (Duchêne et al. 2007).”
From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Kraus et al. 2011
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“However, this is difficult to formulate as binary identifications are not complete at mass ratios less than 0.1 (e.g., Kraus et al. 2011) and the number of secondaries hosting passive disks in the 10 7 year old age range is not well characterized.”
From PLANETARY CONSTRUCTION ZONES IN OCCULTATION: DISCOVERY OF AN EXTRASOLAR RING SYSTEM TRANSITING A YOUNG SUN-LIKE STAR AND FUTURE PROSPECTS FOR DETECTING ECLIPSES BY CIRCUMSECONDARY AND CIRCUMPLANETARY DISKS (2012) · cites this paper as Kraus et al. 2011
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Citations
Cites
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“If the disk accumulates material from the envelope more quickly than mass can accrete onto the star, then it could grow more massive and violate the Toomre stability criterion (Toomre 1964), fragmenting to form a bound companion.”
BackgroundA SURVEY OF STELLAR FAMILIES: MULTIPLICITY OF SOLAR-TYPE STARS
Raghavan, D., McAlister, H. A., Henry, T. J., Latham, D. W., Marcy, G. W., Mason, B. D., Gies, D. R., White, R. J., & ten Brummelaar, T. A. (2010) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/190/1/1 · Cited by 1,922
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Evolutionary Models for Very Low-Mass Stars and Brown Dwarfs with Dusty Atmospheres
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Cited by
Sorted by citations
Items 301–324 of 324
New Insights into the T Tauri Binary Separation Distribution
Eastlund, C., Moe, M., Kratter, K. M., & Kounkel, M. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adf6bc · Cited by 1
Ivanov, E. V. (2012) · Geomagnetism and Aeronomy · doi:10.1134/s0016793212080142 · Cited by 1
Wang, Y., Wu, Z. Y., Xu, T., Li, Q., Xu, M., Zhang, H., & Hou, Y. (2018) · SPIE Optical and Infrared Interferometry and Imaging · doi:10.1117/12.2311604 · Cited by 1
Strampelli, G., Pueyo, L. A., Aguilar, J., Aparicio, A., Duchêne, G., & Robberto, M. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac879e · Cited by 1
The SPHERE view of multiple star formation
Gratton, R., Desidera, S., Marzari, F., & Bonavita, M. (2022) · The European Physical Journal Plus · doi:10.1140/epjp/s13360-022-03377-0 · Cited by 1
Stellar multiplicity: an interdisciplinary nexusPreprint
Breivik, K., Price-Whelan, A. M., D’Orazio, D. J., Hogg, D. W., Johnson, L. C., Moe, M., Morton, T. D., & Tayar, J. (2019) · arXiv (Cornell University) · doi:10.48550/arxiv.1903.05094 · Cited by 1
“Adaptive-optics imaging of a handful of T Tauri stars reveals a similar binary excess across intermediate separations a ∼ 10 − 100 au [8, 9], which poses a significant challenge to models of binary formation and dynamical evolution [10].”
BackgroundSimon, M. (2019) · UA Campus Repository (The University of Arizona) · Cited by 1
Elliott, P., Huélamo, N., Bouy, H., Bayo, A., Melo, C., Torres, C. A. O., Sterzik, M., Quast, G. R., Chauvin, G., & Barrado, D. (2015) · arXiv (Cornell University) · doi:10.48550/arxiv.1505.07837
“Left: Red, green and gold shaded areas represent the 68% confidence intervals for the kernel density estimation (KDE) of multiple systems for SACY, Taurus (K11) and the field (R10), respectively.”
BackgroundResultInfluentialHigh Resolution Imaging and the Formation of Stars and Planets
Cheetham, A. C. (2015) · The Sydney eScholarship Repository (The University of Sydney)
Radio Interferometry Observations of the Hallmarks of Planet Formation
Andrews, S. M. (2013) · Proceedings of the International Astronomical Union · doi:10.1017/s1743921313007977
“…data are difficult to explain with either alternative disk evolution processes (see, e.g., Owen et al. 2011 and Birnstiel et al. 2012b regarding the issues with photoevaporation or particle growth, respectively) or more massive stellar/brown dwarf companions (Pott et al. 2010; Kraus et al. 2011).”
BackgroundSparse aperture masking at the VLT
Lacour, S., Tuthill, P., Amico, P., Ireland, M., Ehrenreich, D., Huélamo, N., & Lagrange, A. ‐. (2011) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201116712/pdf
Self-citationStone, J. M. (2015) · UA Campus Repository (The University of Arizona)
Dynamical Processing of Stars and Planets Through Star Clusters
Geller, A. M. (2016) · doi:10.22323/1.261.0006
“We now know that binary, and higher-order multiple stars are ubiquitous, and comprise a relatively large fraction of the stars in star forming regions [36, 51, 53, 7, 84], open clusters [66, 72, 67, 71, 35, 34, 43] and the Galactic field [83].”
BackgroundAbsolute parameters of young stars: PU Pup
Özkardeş, B., Sürgit, D., Erdem, A., Budding, E., & Banks, T. (2021) · Çanakkale Onsekiz Mart University AVESIS · doi:10.1088/1674-4527/21/10/256
Moderate-separation Binary Companions May Influence Young Stellar X-Ray Luminosity
Clark, M., Sullivan, K., & Soares-Furtado, M. (2024) · Research Notes of the AAS · doi:10.3847/2515-5172/ada14e
Using Rapid Rotators as Tracers of Multiplicity Statistics as a Function of Stellar Density
Cingirikonda, P., Kounkel, M., & Mullen, J. P. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae2acd
Looking for hot Jupiters around young stars
Yu, L. (2019) · theses.fr (ABES) · doi:10.70675/75d275cdz6db2z46a3zb4a3zafd03f4f4b0d
The Walkaway Star HP Tau/G2: Evidence for a Stellar Merger
Reipurth, B., Bally, J., Friberg, P., Faes, D. M., Briceño, C., Connelley, M. S., Flores, C., Cody, A. M., & Zinnecker, H. (2026) · The Astronomical Journal · doi:10.3847/1538-3881/ae4962
Barnes-Sánchez, F., & de Castro, A. I. G. (2026) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stag1789
Wang, R. L., Huber, D., Hey, D., Burns-Watson, N., Larsen, A., Kraus, A. L., Dupuy, T. J., Giacalone, S., & Crepp, J. R. (2026) · The Astronomical Journal · doi:10.3847/1538-3881/aea6d0
Self-citation
Metadata
- 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)
- 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
- 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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