The Role of Multiplicity in Disk Evolution and Planet Formation

Kraus, Adam L.; Ireland, Michael; Hillenbrand, Lynne A.; Martinache, Frantz

doi:10.1088/0004-637x/745/1/19

Cited by 271 publications

(305 citation statements)

References 153 publications

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“…With the exception of Kraus et al (2012), these studies were not sensitive to the tight binary systems to which our study was especially sensitive. Kraus et al (2012) and Cheetham et al (2015), sensitive to similar binary separations to our study, find the disk fraction among close visual binaries (0.1-40 au) in Taurus-Auriga and Ophiuchus to be lower than for single stars. Their studies did not distinguish between circumbinary TDs and other disk types (e.g., debris disks).…”

Section: Sample Sensitivity To Companionsmentioning

confidence: 86%

“…However, several studies (Ghez et al 1997;White & Ghez 2001;Cieza et al 2009;Duchêne 2010;Kraus et al 2012) have found protoplanetary disk fractions are lower for young ( 5 Myr) binary systems with a<50 au than for single stars or wider binaries. With the exception of Kraus et al (2012), these studies were not sensitive to the tight binary systems to which our study was especially sensitive.…”

Section: Sample Sensitivity To Companionsmentioning

confidence: 99%

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Searching for Spectroscopic Binaries Within Transition Disk Objects*

Kohn

Shkolnik

Weinberger

et al. 2016

ApJ

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Transition disks (TDs) are intermediate stage circumstellar disks characterized by an inner gap within the disk structure. To test whether these gaps may have been formed by closely orbiting, previously undetected stellar companions, we collected high-resolution optical spectra of 31 TD objects to search for spectroscopic binaries (SBs). Twenty-four of these objects are in Ophiuchus and seven are within the Coronet, Corona Australis, and Chameleon I star-forming regions. We measured radial velocities for multiple epochs, obtaining a median precision of 400 ms −1 . We identified double-lined SB SSTc2d J163154.7-250324 in Ophiuchus, which we determined to be composed of a K7(±0.5) and a K9(±0.5) star, with orbital limits of a<0.6 au and P<150 days. This results in an SB fraction of -+ 0.04 0.03 0.12 in Ophiuchus, which is consistent with other spectroscopic surveys of non-TD objects in the region. This similarity suggests that TDs are not preferentially sculpted by the presence of close binaries and that planet formation around close binaries may take place over similar timescales to that around single stars.

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Section: Sample Sensitivity To Companionsmentioning

confidence: 86%

Section: Sample Sensitivity To Companionsmentioning

confidence: 99%

Searching for Spectroscopic Binaries Within Transition Disk Objects*

Kohn

Shkolnik

Weinberger

et al. 2016

ApJ

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“…Binaries with separations closer than ∼40 AU show a lower frequency of infrared excess compared with single or wide binary sources (e.g., Monin et al 2007;Cieza et al 2009;Kraus et al 2012). This suggests that these triples and quadruples should have a higher fraction of mixed pairs.…”

Section: Mixed Systemsmentioning

confidence: 99%

“…Because the close components should exhibit rapid disk clearing (Monin et 4 al. 2007;Cieza et al 2009;Kraus et al 2012), whether this parameter affects our discussion or not is explored in later sections. Binarity in these systems, especially those that are widely separated, has yet to be confirmed by multi-epoch astrometry; therefore, many of these systems are candidates of binaries.…”

Section: Sample and Archival Datamentioning

confidence: 99%

Study of infrared excess from circumstellar disks in binaries with Spitzer/IRAC

Itoh

Fukagawa

Shibai

et al. 2015

Publications of the Astronomical Society of Japan

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The presence of excess emission at 3.6-8.0 µm was investigated in a sample of 27 binary systems located in two nearby star-forming regions, Taurus and Ophiuchus, by using Spitzer/Infrared Array Camera (IRAC) archival data. Angular (Projected) separations for the binaries are greater than 2 ′′ (∼280 AU), which allowed us to perform spatially resolved photometry of individual primary and secondary sources. The measured occurrence of infrared excess suggests that binarity plays a role in the evolution of circumstellar disks, even at such wide binary separations. Most of the binaries have excess emission from both the circumprimary and circumsecondary disks, or show photospheric levels for both components at all four wavelengths of IRAC. On the other hand, four systems (17 +11 −8 %, designated by "mixed" systems) exhibit excess emission from a single binary component. This ratio is significantly smaller than that predicted by the random pairing of single stars, suggesting that circumprimary and circumsecondary disks are synchronously dispersed. In addition, the excess frequencies (EFs) of primary and secondary sources with a projected distance of a p ≃ 280-450 AU are 100 +0 −17 % and 91 +8 −18 %, respectively, and significantly higher than that of single stars (70 ± 5%). We made a simple model describing the EF distribution as a function of the disk outer radius, R out . Comparisons with observations using the Kolmogorov-Smirnov test show that the observational data are consistent with the model when the EF ≃ 1 region is found at R out ∼ 30-100 AU. This disk radius is smaller than that typically estimated for single stars. The high EF of circumstellar disks with these radii may indicate a prolonged lifetime of dust in binary systems possibly because smaller disks counteract mass loss by photoevaporation.

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“…In addition, the single star fraction -a crucial statistic for giant planet formation (e.g. Kraus et al 2012) -decreases from ∼60-70% for M-dwarfs (Fischer & Marcy 1992;Bergfors et al 2010) to ∼54% for solar-type stars (Duquennoy & Mayor 1991;Raghavan et al 2010) to near 0% for the most massive stars (Preibisch et al 1999), further separating M-dwarfs from AFGK stars as the most numerous potential planet hosts of all the stellar classes (Lada 2006). About 25% of all Doppler-confirmed planets with M sin i < 30 M ⊕ are orbiting M-dwarfs.…”

mentioning

confidence: 99%

VVV high proper motion stars – I. The catalogue of brightK_S≤ 13.5 stars

Kurtev

Gromadzki

Beamín

et al. 2016

Mon. Not. R. Astron. Soc.

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Knowledge of the stellar content near the Sun is important for a broad range of topics ranging from the search for planets to the study of Milky Way structure. The most powerful method for identifying potentially nearby stars is proper motion (PM) surveys. All old optical surveys avoid, or are at least substantially incomplete, near the Galactic plane. The depth and breadth of the "Vista Variables in Vía Láctea" (VVV) near-IR survey significantly improves this situation. Taking advantage of the VVV survey database, we have measured PMs in the densest regions of the MW bulge and southern plane in order to complete the census of nearby objects. We have developed a custom PM pipeline based on VVV catalogues from the Cambridge Astronomy Survey Unit (CASU), by comparing the first epoch of JHK S with the multi-epoch K Sbands acquired later. Taking advantage of the large time baseline between the 2MASS and the VVV observations, we also obtained 2MASS-VVV PMs. We present a near-IR proper motion catalogue for the whole area of the VVV survey, which includes 3003 moving stellar sources. All of these have been visually inspected and are real PM objects. Our catalogue is in very good agreement with the proper motion data supplied in IR catalogues outside the densest zone of the MW. The majority of the PM objects in our catalogue are nearby M-dwarfs, as expected. This new database allow us to identify 57 common proper motion binary candidates, among which are two new systems within 30 pc of the Sun.Key words: catalogues -proper motions -binaries: general -stars: kinematics and dynamics -stars: low-mass. INTRODUCTIONA complete census of stars within the solar neighbourhood out to a specified distance will inform us about the stellar mass function, star formation, and the kinematics of the Galaxy and of young, nearby clusters and moving groups. The main difficulty in constructing a volume-limited sample is identification of nearby, low-mass objects because of their ⋆ Email: radostin.kurtev@uv.cl low luminosity. Also, accurate distance measurements for these stars are not easy to obtain.The most powerful method for identifying potential nearby stars comes from PM surveys. PM surveys continually improve, as longer time baselines increase the accuracy of the measurement. A uniform census of nearby stars allows characterisation of the relative occurrence rates of different types of stars, and allows relationships between intrinsic properties of those stars, including absolute magnitude and colour, to be examined.The first attempts at large surveys for high proper-

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The Role of Multiplicity in Disk Evolution and Planet Formation

Cited by 271 publications

References 153 publications

Searching for Spectroscopic Binaries Within Transition Disk Objects*

Searching for Spectroscopic Binaries Within Transition Disk Objects*

Study of infrared excess from circumstellar disks in binaries with Spitzer/IRAC

VVV high proper motion stars – I. The catalogue of brightK_S≤ 13.5 stars

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The Role of Multiplicity in Disk Evolution and Planet Formation

Cited by 271 publications

References 153 publications

Searching for Spectroscopic Binaries Within Transition Disk Objects*

Searching for Spectroscopic Binaries Within Transition Disk Objects*

Study of infrared excess from circumstellar disks in binaries with Spitzer/IRAC

VVV high proper motion stars – I. The catalogue of brightKS≤ 13.5 stars

Contact Info

Product

Resources

About

VVV high proper motion stars – I. The catalogue of brightK_S≤ 13.5 stars