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dc.contributor.authorTREMBLIN, Pascal
dc.contributor.authorAUDIT, E.
dc.contributor.authorMINIER, V.
hal.structure.identifierFinnish Meteorological Institute [FMI]
dc.contributor.authorSCHMIDT, W.
hal.structure.identifierFORMATION STELLAIRE 2015
dc.contributor.authorSCHNEIDER, N.
dc.date.issued2015
dc.date.conference2012-08-20
dc.description.abstractEnWe present a new model for the formation of dense clumps and pillars around HII regions based on shocks curvature at the interface between a HII region and a molecular cloud. UV radiation leads to the formation of an ionization front and of a shock ahead. The gas is compressed between them forming a dense shell at the interface. This shell may be curved due to initial interface or density modulation caused by the turbulence of the molecular cloud. Low curvature leads to instabilities in the shell that form dense clumps while sufficiently curved shells collapse on itself to form pillars. When turbulence is high compared to the ionized-gas pressure, bubbles of cold gas have sufficient kinetic energy to penetrate into the HII region and detach themselves from the parent cloud, forming cometary globules.Using computational simulations, we show that these new models are extremely efficient to form dense clumps and stable and growing elongated structures, pillars, in which star formation might occur (see Tremblin et al. 2012a). The inclusion of turbulence in the model shows its importance in the formation of cometary globules (see Tremblin et al. 2012b). Globally, the density enhancement in the simulations is of one or two orders of magnitude higher than the density enhancement of the classical ``collect and collapse`` scenario. The code used for the simulation is the HERACLES code, that comprises hydrodynamics with various equation of state, radiative transfer, gravity, cooling and heating.Our recent observations with Herschel (see Schneider et al. 2012a) and SOFIA (see Schneider et al. 2012b) and additional Spitzer data archives revealed many more of these structures in regions where OB stars have already formed such as the Rosette Nebula, Cygnus X, M16 and Vela, suggesting that the UV radiation from massive stars plays an important role in their formation. We present a first comparison between the simulations described above and recent observations of these regions.
dc.language.isoen
dc.subject.enmethods: numerical
dc.subject.enmethods: data analysis
dc.subject.enISM: globules
dc.subject.enISM: HII regions
dc.subject.enISM: kinematics and dynamics
dc.title.enFormation of structures around HII regions: ionization feedback from massive stars
dc.typeCommunication dans un congrès
dc.identifier.doi10.1017/S1743921314012307
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
bordeaux.pagepp. 590
bordeaux.volume16
bordeaux.countryCN
bordeaux.conference.cityBeijing
bordeaux.peerReviewedoui
hal.identifierhal-01137386
hal.version1
hal.invitednon
hal.proceedingsoui
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01137386v1
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