Show simple item record

Gravity or turbulence? – II. Evolving column density probability distribution functions in molecular clouds

dc.contributor.authorBallesteros‐paredes, Javieren_US
dc.contributor.authorVázquez‐semadeni, Enriqueen_US
dc.contributor.authorGazol, Adrianaen_US
dc.contributor.authorHartmann, Lee W.en_US
dc.contributor.authorHeitsch, Fabianen_US
dc.contributor.authorColín, Pedroen_US
dc.date.accessioned2011-11-10T15:37:13Z
dc.date.available2012-11-02T18:56:47Zen_US
dc.date.issued2011-09-11en_US
dc.identifier.citationBallesteros‐paredes, Javier ; Vázquez‐semadeni, Enrique ; Gazol, Adriana; Hartmann, Lee W.; Heitsch, Fabian; Colín, Pedro (2011). "Gravity or turbulence? â II. Evolving column density probability distribution functions in molecular clouds." Monthly Notices of the Royal Astronomical Society 416(2). <http://hdl.handle.net/2027.42/87053>en_US
dc.identifier.issn0035-8711en_US
dc.identifier.issn1365-2966en_US
dc.identifier.urihttps://hdl.handle.net/2027.42/87053
dc.description.abstractIt has been recently shown that molecular clouds do not exhibit a unique shape for the column density probability distribution function ( N ‐PDF). Instead, clouds without star formation seem to possess a lognormal distribution, while clouds with active star formation develop a power‐law tail at high column densities. The lognormal behaviour of the N ‐PDF has been interpreted in terms of turbulent motions dominating the dynamics of the clouds, while the power‐law behaviour occurs when the cloud is dominated by gravity. In the present contribution, we use thermally bi‐stable numerical simulations of cloud formation and evolution to show that, indeed, these two regimes can be understood in terms of the formation and evolution of molecular clouds: a very narrow lognormal regime appears when the cloud is being assembled. However, as the global gravitational contraction occurs, the initial density fluctuations are enhanced, resulting, first, in a wider lognormal N ‐PDF, and later, in a power‐law N ‐PDF. We thus suggest that the observed N ‐PDF of molecular clouds are a manifestation of their global gravitationally contracting state. We also show that, contrary to recent suggestions, the exact value of the power‐law slope is not unique, as it depends on the projection in which the cloud is being observed.en_US
dc.publisherBlackwell Publishing Ltden_US
dc.publisherWiley Periodicals, Inc.en_US
dc.subject.otherTurbulenceen_US
dc.subject.otherStars: Formationen_US
dc.subject.otherISM: Cloudsen_US
dc.subject.otherISM: Generalen_US
dc.subject.otherISM: Kinematics and Dynamicsen_US
dc.titleGravity or turbulence? – II. Evolving column density probability distribution functions in molecular cloudsen_US
dc.typeArticleen_US
dc.rights.robotsIndexNoFollowen_US
dc.subject.hlbsecondlevelAstronomyen_US
dc.subject.hlbtoplevelScienceen_US
dc.description.peerreviewedPeer Revieweden_US
dc.contributor.affiliationumDepartment of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48105, USAen_US
dc.contributor.affiliationotherCentro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Apdo. Postal 72‐3 (Xangari), Morelia, Michocán 58089, Mexicoen_US
dc.contributor.affiliationotherDepartment of Physics and Astronomy, University of North Carolina Chapel Hill, CB 3255, Phillips Hall, Chapel Hill, NC 27599, USAen_US
dc.description.bitstreamurlhttp://deepblue.lib.umich.edu/bitstream/2027.42/87053/1/j.1365-2966.2011.19141.x.pdf
dc.identifier.doi10.1111/j.1365-2966.2011.19141.xen_US
dc.identifier.sourceMonthly Notices of the Royal Astronomical Societyen_US
dc.identifier.citedreferenceBallesteros‐Paredes J. J., 2006, MNRAS, 372, 443en_US
dc.identifier.citedreferenceBallesteros‐Paredes J., Hartmann L., Vázquez‐Semadeni E., 1999a, ApJ, 527, 285en_US
dc.identifier.citedreferenceBallesteros‐Paredes J., Vázquez‐Semadeni E., Scalo J., 1999b, ApJ, 515, 286en_US
dc.identifier.citedreferenceBallesteros‐Paredes J., Klessen R. S., Mac Low M.‐M., Vázquez‐Semadeni E., 2006, in Reipurth B., Jewitt D., Keil K., eds, Protostars and Planets V. Univ. of Arizona Press, Tucson, p. 63en_US
dc.identifier.citedreferenceBallesteros‐Paredes J., Hartmann L. W., Vázquez‐Semadeni E., Heitsch F., Zamora‐Avilés M. A., 2011, MNRAS, 411, 65en_US
dc.identifier.citedreferenceBergin E. A., Hartmann L. W., Raymond J. C., Ballesteros‐Paredes J., 2004, ApJ, 612, 921en_US
dc.identifier.citedreferenceCaselli P., Myers P. C., 1995, ApJ, 446, 665en_US
dc.identifier.citedreferenceDib S., Burkert A., 2005, ApJ, 630, 238en_US
dc.identifier.citedreferenceFranco J., Cox D. P., 1986, PASP, 98, 1076en_US
dc.identifier.citedreferenceFroebrich D., Murphy G. C., Smith M. D., Walsh J., Del Burgo C., 2007. MNRAS, 378, 1447en_US
dc.identifier.citedreferenceFroebrich D., Rowles J., 2010, MNRAS, 406, 1350en_US
dc.identifier.citedreferenceGibson D., Plume R., Bergin E., Ragan S., Evans N., 2009, ApJ, 705, 123en_US
dc.identifier.citedreferenceGoldreich P., Kwan J., 1974, ApJ, 189, 441en_US
dc.identifier.citedreferenceGoodman A. A., Pineda J. E., Schnee S. L., 2009, ApJ, 692, 91en_US
dc.identifier.citedreferenceHartmann L., Ballesteros‐Paredes J., Bergin E. A., 2001, ApJ, 562, 852en_US
dc.identifier.citedreferenceHeitsch F., Hartmann L., 2008, ApJ, 689, 290en_US
dc.identifier.citedreferenceHeitsch F., Burkert A., Hartmann L. W., Slyz A. D., Devriendt J. E. G., 2005, ApJ, 633, L113en_US
dc.identifier.citedreferenceHeitsch F., Slyz A. D., Devriendt J. E. G., Hartmann L. W., Burkert A., 2006, ApJ, 648, 1052en_US
dc.identifier.citedreferenceHeitsch F., Ballesteros‐Paredes J., Hartmann L., 2009, ApJ, 704, 1735en_US
dc.identifier.citedreferenceHennebelle P., Pérault M., 1999, A&A, 351, 309en_US
dc.identifier.citedreferenceHeyer M., Krawczyk C., Duval J., Jackson J. M., 2009, ApJ, 699, 1092en_US
dc.identifier.citedreferenceKainulainen J., Beuther H., Henning T., Plume R., 2009, A&A, 508, L35en_US
dc.identifier.citedreferenceKainulainen J., Beuther H., Banerjee R., Federrath C., Henning T., 2011, A&A, 530, A64en_US
dc.identifier.citedreferenceKlessen R. S., 2000, ApJ, 535, 869en_US
dc.identifier.citedreferenceKoyama H., Inutsuka S. I., 2002, ApJ, 564, L97en_US
dc.identifier.citedreferenceKravtsov A. V., Klypin A. A., Khokhlov A. M., 1997, ApJS, 111, 73en_US
dc.identifier.citedreferenceKritsuk A. G., Norman M. L., Wagner R., 2011, ApJ, 727, L20en_US
dc.identifier.citedreferenceLarson R. B., 1981, MNRAS, 194, 809en_US
dc.identifier.citedreferenceMac Low M.‐M., Klessen R. S., 2004, Rev. Modern Phys., 76, 125en_US
dc.identifier.citedreferenceMac Low M.‐M., Klessen R. S., Burkert A., Smith M. D., 1998, Phys. Rev. Lett., 80, 275en_US
dc.identifier.citedreferenceOstriker E. C., Stone J. M., Gammie C. F., 2001, ApJ, 546, 980en_US
dc.identifier.citedreferencePadoan P., Nordlund Å., 1999, ApJ, 526, 279en_US
dc.identifier.citedreferencePassot T., Vázquez‐Semadeni E., 1998, Phys. Rev. E, 58, 4501en_US
dc.identifier.citedreferencePlume R., Jaffe D. T., Evans N. J., II, Martin‐Pintado J., Gomez‐Gonzalez J., 1997, ApJ, 476, 730en_US
dc.identifier.citedreferenceRidge N. A. et al., 2006, AJ, 131, 2921en_US
dc.identifier.citedreferenceRosas‐Guevara Y., Vázquez‐Semadeni E., Gómez G. C., Jappsen A.‐K., 2010, MNRAS, 406, 1875en_US
dc.identifier.citedreferenceShirley Y. L., Evans N. J.,, II, Young K. E., Knez C., Jaffe D. T., 2003, ApJS, 149, 375en_US
dc.identifier.citedreferenceShu F. H., 1977, ApJ, 214, 488en_US
dc.identifier.citedreferenceStone J. M., Ostriker E. C., Gammie C. F., 1998, ApJ, 508, L99en_US
dc.identifier.citedreferenceTassis K., Christie D. A., Urban A., Pineda J. L., Mouschovias T. C., Yorke H. W., Martel H., 2010, MNRAS, 408, 1089en_US
dc.identifier.citedreferenceVázquez‐Semadeni E., 1994, ApJ, 423, 681en_US
dc.identifier.citedreferenceVázquez‐Semadeni E., 2010, in Alves J., Elmegreen B., Trimble V., eds, Proc. IAU Symp. 270, Computational Star Formation. Cambridge Univ. Press, Cambridge, p. 275en_US
dc.identifier.citedreferenceVázquez‐Semadeni E., 2011, in Kothes R., Landecker T. L., Willis A. G., eds, ASP Conf. Ser. Vol. 438, The Dynamic Interstellar Medium. A Celebration of the Canadian Galactic Plane Survey. Astron. Soc. Pac., San Francisco, p. 83en_US
dc.identifier.citedreferenceVázquez‐Semadeni E., García N., 2001. ApJ, 557, 727en_US
dc.identifier.citedreferenceVázquez‐Semadeni E., Ryu D., Passot T., González R. F., Gazol A., 2006, ApJ, 643, 245en_US
dc.identifier.citedreferenceVázquez‐Semadeni E., Gómez G. C., Jappsen A. K., Ballesteros‐Paredes J., González R. F., Klessen R. S., 2007, ApJ, 657, 870en_US
dc.identifier.citedreferenceVázquez‐Semadeni E., González R. F., Ballesteros‐Paredes J., Gazol A., Kim J., 2008, MNRAS, 390, 769en_US
dc.identifier.citedreferenceVázquez‐Semadeni E., Gómez G. C., Jappsen A.‐K., Ballesteros‐Paredes J., Klessen R. S., 2009, ApJ, 707, 1023en_US
dc.identifier.citedreferenceVázquez‐Semadeni E., Colín P., Gómez G. C., Ballesteros‐Paredes J., Watson A. W., 2010, ApJ, 715, 1302en_US
dc.identifier.citedreferenceWilson R. W., Jefferts K. B., Penzias A. A., 1970, ApJ, 161, L43en_US
dc.identifier.citedreferenceWu J., Evans N. J., Shirley Y. L., Knez C., 2010, ApJS, 188, 313en_US
dc.identifier.citedreferenceZuckerman B., Evans N. J.,, II, 1974, ApJ, 192, L149en_US
dc.owningcollnameInterdisciplinary and Peer-Reviewed


Files in this item

Show simple item record

Remediation of Harmful Language

The University of Michigan Library aims to describe library materials in a way that respects the people and communities who create, use, and are represented in our collections. Report harmful or offensive language in catalog records, finding aids, or elsewhere in our collections anonymously through our metadata feedback form. More information at Remediation of Harmful Language.

Accessibility

If you are unable to use this file in its current format, please select the Contact Us link and we can modify it to make it more accessible to you.