Young stellar clusters

Jan 17, 2011
An image of the young star forming region in Perseus, as seen by the infrared cameras onboard the Spitzer Space Telescope. Young stars are seen as pinkish dots. Although the stellar population here differs from that seen in more massive clusters, new research indicates that the processes at work in these modest groups (and the consequent properties of the stars) are one end of a range of normal situations that includes both massive and smaller clusters. Credit: NASA and Spitzer

(PhysOrg.com) -- Most stars are thought to form in clusters rather than in isolation, as the gas and dust in a molecular cloud coalesces under the influence of gravity until clumps develop that are dense enough to become stars. Most massive stars are also found in such groupings, rather than in isolation.

There are some nearby star-forming regions, however, that for some reason deviate from this norm: their low mass stars are found in isolation, and they have no . It is not understood whether the differences arise because there are two distinct contexts for making stars, or because normal clustering occurs across a large continuum of cloud properties with a consequent range of group characteristics.

CfA astronomers Helen Kirk and Phil Myers analyzed the mass and spatial distributions of fourteen nearby, intermediate size young stellar groups looking for evidence of a sharp distinction between clustered and isolated modes of . The groups were chosen because they are young (their stars have not moved very far away from their birthplaces), yet old enough that the mass of each young star can be accurately determined from its spectrum. In addition, the stars are spatially distinct, and the stellar population of each group has been well determined.

The astronomers conclude that, at least for the groups they examined, the properties are scaled-down versions of large cluster characteristics. The groups' masses span a wide range that is statistically consistent with the normal distribution seen, and moreover there is a correlation between the mass of the most massive star in each group and that of the whole group.

Finally, they find that the most massive member tends to be found near the center of the cluster, just as it does in more massive examples. The results, besides quantifying the cluster properties of these nearby regions, support the conclusion that there is only one mode of star formation at work in both regimes of isolated and clustered star formation.

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eachus
not rated yet Jan 17, 2011
Speaking as a statistician, this result looks unthinking and almost stupid. It is pretty well established that the lifetimes of these star nurseries are determined by the size of the largest star formed. (When it becomes a supernova or for Wolf-Rayet stars, almost as soon as they are created.)

This means that smaller clusters have much longer lifetimes and should be vastly overrepresented in the cluster population. (I'm ignoring globular clusters, as those seem to be remnants of small galaxies stripped of their outer stars by larger galaxies (or galaxies with larger black holes.)

There is a counter bias in favor of discovering larger star forming regions, but if we try to count all clusters within say 500 parsecs we will find that large clusters are significantly overrepresented, considering their short star-forming lifetimes.

So what gives? My guess is that smaller clusters have their gas blown out by supernovas in nearby large clusters.

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