On the spatial distribution of pre-main-sequence stars in Taurus

Gómez, Mercedes; Hartmann, L.; Kenyon, Scott J.; Hewett, R.

doi:10.1086/116567

Cited by 253 publications

(288 citation statements)

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“…Almost all the stars are born as members of various kinds of stellar groups, stellar associations being a very interesting one (Gomez et al 1993;Massey et al 1995). The variety of sizes of such stellar systems suggests a hierarchy in the formation of stellar structures as was earlier noted by McKibben Nail & Shapley (1953).…”

Section: Introductionmentioning

confidence: 78%

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

Gouliermis

Kontizas

et al. 2003

A&A

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Abstract. The method developed by Gouliermis et al. (2000, Paper I), for the detection and classification of stellar systems in the LMC, was used for the identification of stellar associations and open clusters in the central area of the LMC. This method was applied on the stellar catalog produced from a scanned 1.2 m UK Schmidt Telescope Plate in U with a field of view almost 6.• 5 × 6.• 5, centered on the Bar of this galaxy. The survey of the identified systems is presented here followed by the results of the investigation on their spatial distribution and their structural parameters, as were estimated according to our proposed methodology in Paper I. The detected open clusters and stellar associations show to form large filamentary structures, which are often connected with the loci of HI shells. The derived mean size of the stellar associations in this survey was found to agree with the average size found previously by other authors, for stellar associations in different galaxies. This common size of about 80 pc might represent a universal scale for the star formation process, whereas the parameter correlations of the detected loose systems support the distinction between open clusters and stellar associations.

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Section: Introductionmentioning

confidence: 78%

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

Gouliermis

Kontizas

et al. 2003

A&A

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“…[19,8,27]), but the notion has been questioned after Spitzer results hinted otherwise [1]. If there are indeed two modes, then we would expect to see a bi-or multi-modal profile in cumulative surface density distribution plots such as Figs.…”

Section: Resultsmentioning

confidence: 99%

Do All Stars in the Solar Neighbourhood Form in Clusters?

Bressert

Bastian

Gutermuth

2011

Star Clusters in the Era of Large Surveys

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We present a global study of low mass, young stellar object (YSO) surface densities (Σ ) in nearby (< 500 pc) star forming regions based on a comprehensive collection of Spitzer Space Telescope surveys. We show that the distribution of YSO surface densities is a smooth distribution, being adequately described by a lognormal function from a few to 10 3 YSOs per pc 2 , with a peak at ∼ 22 stars pc −2 . The observed lognormal Σ is consistent with predictions of hierarchically structured starformation at scales below 10 pc, arising from the molecular cloud structures. We do not find evidence for multiple discrete modes of star-formation (e.g. clustered and distributed). Comparing the observed Σ distribution to previous Σ threshold definitions of clusters show that they are arbitrary. We find that only a low fraction (< 26%) of stars are formed in dense environments where their formation/evolution (along with their circumstellar disks and/or planets) may be affected by the close proximity of their low-mass neighbours.

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“…The age of its population is ≈1 Myr. Six distinct clusters of stars in Taurus were detected by Gomez et al (1993) to have projected radii of 0.5−1 pc with ≈15 stars or binaries (with a mass of about 6 M for m ≈ 0.4) each and a median separation between the stellar centre-of-mass systems within each cluster of 0.3 pc. The individual clusters are separated by a few pc, thus do not interact dynamically.…”

Section: Taurusmentioning

confidence: 99%

Inverse dynamical population synthesis

Marks

Kroupa

2012

A&A

253

302

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Binary populations in young star clusters show multiplicity fractions both lower and up to twice as high as those observed in the Galactic field. We follow the evolution of a population of binary stars in dense and loose star clusters starting with an invariant initial binary population and a formal multiplicity fraction of unity, and demonstrate that these models can explain the observed binary properties in Taurus, ρ Ophiuchus, Chamaeleon, Orion, IC 348, Upper Scorpius A, Praesepe, and the Pleiades. The model needs to consider solely different birth densities for these regions. The evolved theoretical orbital-parameter distributions are highly probable parent distributions for the observed ones. We constrain the birth conditions (stellar mass, M ecl , and half-mass radius, r h ) for the derived progenitors of the star clusters and the overall present-day binary fractions allowed by the present model. The results compare very well with properties of molecular cloud clumps on the verge of star formation. Combining these with previously and independently obtained constraints on the birth densities of globular clusters, we identify a weak stellar mass -half-mass radius correlation for cluster-forming cloud clumps, r h /pc ∝ (M ecl /M ) 0.13 ± 0.04 . The ability of the model to reproduce the binary properties in all the investigated young objects, covering present-day densities from 1−10 stars pc −3 (Taurus) to 2 × 10 4 stars pc −3 (Orion), suggests that environment-dependent dynamical evolution plays an important role in shaping the present-day properties of binary populations in star clusters, and that the initial binary properties may not vary dramatically between different environments.

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On the spatial distribution of pre-main-sequence stars in Taurus

Cited by 253 publications

References 0 publications

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

Do All Stars in the Solar Neighbourhood Form in Clusters?

Inverse dynamical population synthesis

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