Thermophysical and sonochemical behaviour of binary mixtures of decan-1-ol with halohydrocarbons at (T=293.15 and 313.15)K

Bhatia, Subhash C.; Bhatia, Rachna; Dubey, Gyan Prakash

doi:10.1016/j.jct.2009.07.020

Cited by 19 publications

(13 citation statements)

References 56 publications

(114 reference statements)

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“…This is in contrast with the Large Magellanic Cloud (LMC), where about 10% of the known open clusters seem to belong to pairs and probably more than 50% of them are true binary clusters (Dieball & Grebel 2000;Dieball et al 2002). Following Bhatia (1990), the lifetimes of binary clusters depend on their mutual separation but also on the tidal force of the parental galaxy and on encounters with giant molecular clouds. The models of Bhatia (1990) indicate binary cluster lifetimes ranging from a few 10 6 yr to 4 × 10 7 yr.…”

Section: Introductionmentioning

confidence: 92%

“…Following Bhatia (1990), the lifetimes of binary clusters depend on their mutual separation but also on the tidal force of the parental galaxy and on encounters with giant molecular clouds. The models of Bhatia (1990) indicate binary cluster lifetimes ranging from a few 10 6 yr to 4 × 10 7 yr. Besides pairs originating from the same star forming event (which we call "true binary/double clusters"), gravitational capture can also create cluster pairs.…”

Section: Introductionmentioning

confidence: 99%

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Open clusters in the Third Galactic Quadrant III. Alleged binary clusters

Vazquez

Moitinho

Carraro³

et al. 2010

A&A

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Aims. We aim to determine accurate distances and ages of eight open clusters in order to: (1) assess their possible binarity (2) provide probes to trace the structure of the Third Galactic Quadrant. Methods. Cluster reddenings, distances, ages and metallicities are derived from ZAMS and isochrone fits in UBVRI photometric diagrams. Field contamination is reduced by restricting analysis to stars within the cluster limits derived from star counts. Further membership control is done by requiring that stars have consistent positions in several diagrams and by using published spectral types. Results. The derived distances, ages and metallicities have shown that none of the analysed clusters compose binary/double systems. Of the four candidate pairs, only NGC 2383/NGC 2384 are close to each other, but have different metallicities and ages. Ruprecht 72 and Ruprecht 158 are not clusters but fluctuations of the field stellar density. Haffner 18 is found to be the superposition of two stellar groups at different distances: Haffner 18(1) at 4.5 kpc and Haffner 18(2) between 9.5 and 11.4 kpc from the Sun. The derived distances and ages have been used to situate the clusters in the Galactic context. In particular, young stellar groups trace spiral structure at large Galactocentric radii. At least two clusters formed during the last few 10 8 yr in an interstellar medium with less than solar abundances. Conclusions. In contrast with the LMC, double clusters are apparently rare, or even non existent, in the undisturbed environment of the Third Galactic Quadrant. This leaves open the question of whether binary clusters form more easily toward denser and more violent regions of the Milky Way such as the inner Galaxy.

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Section: Introductionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Open clusters in the Third Galactic Quadrant III. Alleged binary clusters

Vazquez

Moitinho

Carraro³

et al. 2010

A&A

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“…Thus, binary star clusters are believed to be short-lived, with lifetimes of 10-100 Myr (Bhatia 1990;de la Fuente Marcos & de la Fuente Marcos 2010;Priyatikanto et al 2016). Within the Magellanic Clouds, between ∼10%-20% of clusters are potentially part of a binary/multiple system (see Dieball et al 2002and references therein).…”

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confidence: 99%

The Hierarchical Distribution of the Young Stellar Clusters in Six Local Star-forming Galaxies

Grasha

Calzetti

Adamo

et al. 2017

ApJ

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We present a study of the hierarchical clustering of the young stellar clusters in six local (3-15 Mpc) star-forming galaxies using Hubble Space Telescope broad band WFC3/UVIS UV and optical images from the Treasury Program LEGUS (Legacy ExtraGalactic UV Survey). We have identified 3685 likely clusters and associations, each visually classified by their morphology, and we use the angular two-point correlation function to study the clustering of these stellar systems. We find that the spatial distribution of the young clusters and associations are clustered with respect to each other, forming large, unbound hierarchical star-forming complexes that are in general very young. The strength of the clustering decreases with increasing age of the star clusters and stellar associations, becoming more homogeneously distributed after ∼40-60 Myr and on scales larger than a few hundred parsecs. In all galaxies, the associations exhibit a global behavior that is distinct and more strongly correlated from compact clusters. Thus, populations of clusters are more evolved than associations in terms of their spatial distribution, traveling significantly from their birth site within a few tens of Myr whereas associations show evidence of disruption occurring very quickly after their formation. The clustering of the stellar systems resembles that of a turbulent interstellar medium that drives the star formation process, correlating the components in unbound star-forming complexes in a hierarchical manner, dispersing shortly after formation, suggestive of a single, continuous mode of star formation across all galaxies.

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“…Models for less massive clusters in the LMC tidal field predict a few ×10 7 yr for the pair lifetime, with separations varying from ∼ 6 pc for cluster masses of 10 3 M and ∼ 14 pc for 10 4 M (Bhatia 1990). According to these models, after this timescale either the cluster pair merges due to mutual gravitational interaction or is disrupted by the galactic tidal field and, less probably, by passing giant molecular clouds.…”

Section: Discussionmentioning

confidence: 99%

Astrophysical properties of binary star clusters in the Small Magellanic Cloud

2009

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Abstract.To study the evolution of binary star clusters, we have imaged seven systems in the Small Magellanic Cloud with the SOAR 4m telescope using B and V filters. The sample contains pairs with well-separated components (d < 30 pc) as well as systems that apparently have merged, as evidenced by their unusual structures. By employing isochrone fitting to their color-magnitude diagrams, we have determined reddening values, ages and metallicities, and by fitting King models to their radial stellar-density profiles we estimated core radii. Disturbances of the density profiles are interpreted as evidence of interactions. Properties such as the distances between their components and their age differences are addressed in terms of the timescales involved, to assess the physical connection of the system. In two cases, the age difference is more than 50 Myr, which suggests a chance alignment, capture or sequential star formation.

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Thermophysical and sonochemical behaviour of binary mixtures of decan-1-ol with halohydrocarbons at (T=293.15 and 313.15)K

Cited by 19 publications

References 56 publications

Open clusters in the Third Galactic Quadrant III. Alleged binary clusters

Open clusters in the Third Galactic Quadrant III. Alleged binary clusters

The Hierarchical Distribution of the Young Stellar Clusters in Six Local Star-forming Galaxies

Astrophysical properties of binary star clusters in the Small Magellanic Cloud

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