2006MNRAS.369..143M

Query : 2006MNRAS.369..143M

2006MNRAS.369..143M - Mon. Not. R. Astron. Soc., 369, 143-155 (2006/June-2)

Triggered star formation in bright-rimmed clouds: the Eagle nebula revisited.

MIAO J., WHITE G.J., NELSON R., THOMPSON M. and MORGAN L.

Abstract (from CDS):

A three-dimensional smoothed particle hydrodynamics model has been extended to study the radiation-driven implosion effect of massive stars on the dynamical evolution of surrounding molecular clouds. The new elements in the upgraded code are the inclusion of Lyman continuum in the incident radiation flux and the treatment of hydrogen ionization process; the introduction of ionization heating and recombination cooling effects; and the addition of a proper description of the magnetic and turbulent pressures to the internal pressure of the molecular cloud. This extended code not only provides a realistic model to trace the dynamical evolution of a molecular cloud, but also can be used to model the kinematics of the ionization and shock fronts and the photoevaporating gas surrounding the molecular cloud, which the previous code is unable to handle.

The application of this newly developed model to the structure of the middle Eagle nebula finger suggests that the shock induced by the ionizing radiation at the front side of the head precedes an ionization front moving towards the centre of the core, and that the core at the fingertip is at a transition stage evolving toward a state of induced star formation. The dynamical evolution of the velocity field of the simulated cloud structure is discussed to illustrate the role of the self-gravity and the different cloud morphologies which appear at different stages in the evolutionary process of the cloud. The motion of the ionization front and the evaporating gas are also investigated. The modelled gas evaporation rate is consistent with that of other current models and the density, temperature and chemical profiles are in agreement with the observed values.

The relative lifetimes of different simulated cloud morphologies suggest a possible answer to the question of why more bright-rimmed clouds are observed to possess a flat-core than an elongated-core morphology.


Abstract Copyright: 2006 The Authors. Journal compilation © 2006 RAS

Journal keyword(s): radiative transfer - stars: formation - ISM: evolution - Hii regions - ISM: kinematics and dynamics

Simbad objects: 1

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Number of rows : 1
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 M 16 OpC 18 18 45.1 -13 47 31           ~ 1084 1

Query : 2006MNRAS.369..143M

Basic data :
M 16 -- Open Cluster
Other object types: otypes_help 		OpC (2013A&A,OCISM,...), Cl* (2020A&A,C,...), Rad (CTB,GRS,...), Cl? (2013A&A), HII (LBN)
ICRS coord. (ep=J2000) : 		18 18 45.1 -13 47 31 (Optical) [ ] E 2021A&A...647A..19T
FK4 coord. (ep=B1950 eq=1950) : 		18 15 55.0 -13 48 47 [ ]
Gal coord. (ep=J2000) : 		016.9615 +00.8106 [ ]
Proper motions mas/yr : 		0.178 -1.576 [0.014 0.018 90] C 2020A&A...633A..99C
Radial velocity / Redshift / cz : 		V(km/s) 18.00 [0.58] / z(~) 0.000060 [0.000002] / cz 18.00 [0.58]
   (Opt) A 2017AstBu..72..257L
Parallaxes (mas): 		0.566 [0.006] C 2020A&A...633A..99C
Angular size (arcmin): 		80.0 80.0 0 (~) C 2022A&A...664A..66M
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Hierarchy : number of linked objects
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: 2287 		Display criteria :

Identifiers (18) :
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M 16 LBN 016.96+00.78 NAME Star Queen Villafranca O-019
C 1816-138 LBN 67 NGC 6611 [KPR2004b] 441
CTB 51 LMH 22 NRL 14 [KPS2012] MWSC 2886
GRS G017.00 +00.30 MM 21 OCISM 10
IC 4703 NAME Eagle Nebula OCl 54

References (1084 between 1850 and 2026) (Total 1084)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).
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Velocities : 6    Distance : 7    Fe/H : 1    Plx : 7    PM : 9   

   

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Herschel : 16    ISO : 52    IUE : 3   

   

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Data at NED - NASA/IPAC Extragalactic Database : M 16

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NGC 6611

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