THE MASS-SIZE RELATION FROM CLOUDS TO CORES. II. SOLAR NEIGHBORHOOD CLOUDS

Kauffmann, J; Shetty, R; Goodman, A A; Pillai, T

doi:10.1088/0004-637X/716/1/433

Title: THE MASS-SIZE RELATION FROM CLOUDS TO CORES. II. SOLAR NEIGHBORHOOD CLOUDS

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Abstract

We measure the mass and size of cloud fragments in several molecular clouds continuously over a wide range of spatial scales (0.05 {approx}< r/pc {approx}< 3). Based on the recently developed 'dendrogram-technique', this characterizes dense cores as well as the enveloping clouds. 'Larson's Third Law' of constant column density, m(r) {proportional_to} r {sup 2}, is not well suited to describe the derived mass-size data. Solar neighborhood clouds not forming massive stars ({approx}<10 M {sub sun}; Pipe Nebula, Taurus, Perseus, and Ophiuchus) obey m(r) {<=} 870 M {sub sun}(r/pc){sup 1.33}. In contrast to this, clouds forming massive stars (Orion A, G10.15 - 0.34, G11.11 - 0.12) do exceed the aforementioned relation. Thus, this limiting mass-size relation may approximate a threshold for the formation of massive stars. Across all clouds, cluster-forming cloud fragments are found to be-at given radius-more massive than fragments devoid of clusters. The cluster-bearing fragments are found to roughly obey a mass-size law m {proportional_to} r {sup 1.27} (where the exponent is highly uncertain in any given cloud, but is certainly smaller than 1.5).

Authors:

Kauffmann, J; Shetty, R; Goodman, A A ^[1]; Pillai, T

Initiative in Innovative Computing (IIC), 60 Oxford Street, Cambridge, MA 02138 (United States)

Publication Date:: Thu Jun 10 00:00:00 EDT 2010

OSTI Identifier:: 21450845

Resource Type:: Journal Article

Journal Name:: Astrophysical Journal

Additional Journal Information:: Journal Volume: 716; Journal Issue: 1; Other Information: DOI: 10.1088/0004-637X/716/1/433; Journal ID: ISSN 0004-637X

Country of Publication:: United States

Language:: English

Subject:: 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; APPROXIMATIONS; DATA ANALYSIS; MASS; NEBULAE; STAR EVOLUTION; STARS; CALCULATION METHODS; EVOLUTION

Citation Formats


                    Kauffmann, J, Shetty, R, Goodman, A A, Pillai, T, and Myers, P. C., E-mail: jens.kauffmann@jpl.nasa.go. THE MASS-SIZE RELATION FROM CLOUDS TO CORES. II. SOLAR NEIGHBORHOOD CLOUDS.  United States: N. p., 2010. 
        Web.  doi:10.1088/0004-637X/716/1/433.

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                    Kauffmann, J, Shetty, R, Goodman, A A, Pillai, T, & Myers, P. C., E-mail: jens.kauffmann@jpl.nasa.go. THE MASS-SIZE RELATION FROM CLOUDS TO CORES. II. SOLAR NEIGHBORHOOD CLOUDS.  United States.  https://doi.org/10.1088/0004-637X/716/1/433

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                    Kauffmann, J, Shetty, R, Goodman, A A, Pillai, T, and Myers, P. C., E-mail: jens.kauffmann@jpl.nasa.go. 2010.  
        "THE MASS-SIZE RELATION FROM CLOUDS TO CORES. II. SOLAR NEIGHBORHOOD CLOUDS".  United States.  https://doi.org/10.1088/0004-637X/716/1/433.

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@article{osti_21450845,

  title        = {THE MASS-SIZE RELATION FROM CLOUDS TO CORES. II. SOLAR NEIGHBORHOOD CLOUDS},

  author       = {Kauffmann, J and Shetty, R and Goodman, A A and Pillai, T and Myers, P. C., E-mail: jens.kauffmann@jpl.nasa.go},

  abstractNote = {We measure the mass and size of cloud fragments in several molecular clouds continuously over a wide range of spatial scales (0.05 {approx}< r/pc {approx}< 3). Based on the recently developed 'dendrogram-technique', this characterizes dense cores as well as the enveloping clouds. 'Larson's Third Law' of constant column density, m(r) {proportional_to} r {sup 2}, is not well suited to describe the derived mass-size data. Solar neighborhood clouds not forming massive stars ({approx}<10 M {sub sun}; Pipe Nebula, Taurus, Perseus, and Ophiuchus) obey m(r) {<=} 870 M {sub sun}(r/pc){sup 1.33}. In contrast to this, clouds forming massive stars (Orion A, G10.15 - 0.34, G11.11 - 0.12) do exceed the aforementioned relation. Thus, this limiting mass-size relation may approximate a threshold for the formation of massive stars. Across all clouds, cluster-forming cloud fragments are found to be-at given radius-more massive than fragments devoid of clusters. The cluster-bearing fragments are found to roughly obey a mass-size law m {proportional_to} r {sup 1.27} (where the exponent is highly uncertain in any given cloud, but is certainly smaller than 1.5).},

  doi          = {10.1088/0004-637X/716/1/433},

  url          = {https://www.osti.gov/biblio/21450845},
  journal      = {Astrophysical Journal},

  issn         = {0004-637X},

  number       = 1,

  volume       = 716,

  place        = {United States},

  year         = {Thu Jun 10 00:00:00 EDT 2010},

  month        = {Thu Jun 10 00:00:00 EDT 2010}

}

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