dc.contributor.author | Klessen, RS | |
dc.contributor.author | Ballesteros‐Paredes, J | |
dc.contributor.author | Vazquez‐Semadeni, E | |
dc.contributor.author | Duran‐Rojas, C | |
dc.date.accessioned | 2019-02-04T13:15:47Z | |
dc.date.issued | 2005-02-20 | |
dc.description.abstract | We investigate the velocity structure of protostellar cores that result from nonmagnetic numerical models of the
gravoturbulent fragmentation of molecular cloud material. A large fraction of the cores analyzed are ‘‘quiescent’’;
i.e., they have nonthermal line widths smaller or equal to the thermal line width. Specifically, about 23% of the
cores have subsonic turbulent line-of-sight velocity dispersions turb cs. A total of 46% are ‘‘transonic,’’ with
cs < turb 2cs. More than half of our sample cores are identified as ‘‘coherent,’’ i.e., with turb roughly independent of column density. Of these, about 40% are quiescent, 40% are transonic, and 20% are supersonic. The fact
that dynamically evolving cores in highly supersonic turbulent flows can be quiescent may be understood because
cores lie at the stagnation points of convergent turbulent flows, where compression is at a maximum and relative
velocity differences are at a minimum. The apparent coherence may be due, at least in part, to an observational effect
related to the length and concentration of the material contributing to the line. In our simulated cores, turb often has
its local maximum at small but finite offsets from the column density maximum, suggesting that the core is the dense
region behind a shock. Such a configuration is often found in observations of nearby molecular cloud cores and
argues in favor of the gravoturbulent scenario of stellar birth as it is not expected in star formation models based on
magnetic mediation. A comparison between the virial estimate Mvir for the mass of a core based on turb and its
actual value M shows that cores with collapsed objects tend to be near equipartition between their gravitational and
kinetic energies, while cores without collapsed objects tend to be gravitationally unbound, suggesting that gravitational collapse occurs immediately after gravity becomes dominant. Finally, cores in simulations driven at large
scales are more frequently quiescent and coherent and have more realistic ratios of Mvir=M, supporting the notion
that molecular cloud turbulence is driven at large scales. | en_GB |
dc.description.sponsorship | Emmy Noether Program of the Deutsche Forschungsgemeinschaft | en_GB |
dc.description.sponsorship | CONACYT | en_GB |
dc.description.sponsorship | CONACYT | en_GB |
dc.identifier.citation | Vol. 620, pp. 786 - 794 | en_GB |
dc.identifier.doi | 10.1086/427255 | |
dc.identifier.grantnumber | KL1358/1 | en_GB |
dc.identifier.grantnumber | 27752-E | en_GB |
dc.identifier.grantnumber | 36571-E | en_GB |
dc.identifier.uri | http://hdl.handle.net/10871/35717 | |
dc.language.iso | en | en_GB |
dc.publisher | American Astronomical Society | en_GB |
dc.rights | © 2005. The American Astronomical Society. | en_GB |
dc.subject | ISM: kinematics and dynamics | en_GB |
dc.subject | stars: formation | en_GB |
dc.subject | turbulence | en_GB |
dc.subject | ISM: clouds | en_GB |
dc.title | Quiescent and Coherent Cores from Gravoturbulent Fragmentation | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2019-02-04T13:15:47Z | |
dc.identifier.issn | 0004-637X | |
dc.description | This is the final published version. Available from the American Astronomical Society via the DOI in this record. | en_GB |
dc.identifier.journal | The Astrophysical Journal | en_GB |
dc.rights.uri | http://www.rioxx.net/licenses/all-rights-reserved | en_GB |
dcterms.dateAccepted | 2004-11-03 | |
rioxxterms.version | VoR | en_GB |
rioxxterms.licenseref.startdate | 2005-02-20 | |
rioxxterms.type | Journal Article/Review | en_GB |
refterms.dateFCD | 2019-02-04T13:09:50Z | |
refterms.versionFCD | VoR | |
refterms.dateFOA | 2019-02-04T13:15:49Z | |
refterms.panel | B | en_GB |