Abstract
In this chapter we use the method of Smoothed Particle Hydrodynamics (SPH) to study the number and properties of accretion centres formed when a molecular gas cloud collapses, starting with initial conditions corresponding either to a turbulent or a rigidly rotating sphere. To do so we use a modified version of the SPH code GADGET-2, which is capable to detect when a gas particle becomes an accretion centre, inheriting the mass and momentum of all its closest neighbours. For both types of models (turbulent and uniformly rotating), we also study the effects of considering two different initial mass distributions: a uniform-density and a centrally condensed Plummer profile. We find that the turbulent models are more propense to fragment into a larger number of protostellar objects than the purely rotating clouds. However, in both types of models the average protostellar mass increases with increasing size of the kinetic energy content of the cloud.
This is a preview of subscription content, log in via an institution to check access.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
References
Arreaga-García G, Saucedo-Morales J, Carmona-Lemus J, Duarte-Pérez R (2008) Hydrodynamical simulations of the non-ideal gravitational collapse of a molecular gas cloud. Revista Mexicana de Astronomía y Astrofísica. 44:259–284
Arreaga-García G, Klapp-Escribano J, Gómez-Ramírez F (2009) The gravitational collapse of Plummer protostellar clouds. Astron Astrophys 509:A96
Arreaga-Garcia G, Saucedo-Morales J (2012) Physical effects of gas envelopes with different extension on the collapse of a gas core. Revista Mexicana de Astronomía y Astrofísica 48:61–84
Arreaga-García G, Klapp J, Sigalotti L. Di G (2007) Gravitational collapse and fragmentation of molecular cloud cores with GADGET-2. Astrophys J 666:290–308
Balsara DS (1995) von Neumann stability analysis of smooth particle hydrodynamics—suggestions for optimal algorithms. J Comput Phys 121:357–372
Bate MR, Bonnell IA, Price NM (1995) Modelling accretion in protobinary systems. Mon Not R Astron Soc 277:362–376
Bodenheimer P, Burkert A, Klein RI, Boss AP (2000) Multiple fragmentation of protostars. In: Mannings VG, Boss AP, Russell SS (eds) Protostars and planets IV. University of Arizona Press, Tucson, pp 675–701
Boss AP, Fisher RT, Klein RI, McKee CF (2000) The Jeans condition and collapsing molecular cloud cores: filaments or binaries? Astrophys J 528:325–335
Dobbs CL, Bonnell IA, Clark PC (2005) Centrally condensed turbulent cores: massive stars or fragmentation? Mon Not R Astron Soc 360:2–8
Dubinski J, Narayan R, Phillips TG (1995) Turbulence in molecular clouds. Astrophysical J 448:226–290
Federrath C, Banerjee R, Clark PC, Klessen RS (2010) Modeling collapse and accretion in turbulent gas clouds: implementation and comparison of sink particles in AMR and SPH. Astrophysical J 713:269–290
Gabbasov RF, Rodríguez-Meza MA, Klapp J, Cervantes-Cota JL (2006) The influence of numerical parameters on tidally triggered bar formation. Astron Astrophys 449:1043–1059
Goodwin SP, Whithworth AP, Ward-Thompson D (2004) Simulating star formation in molecular cloud cores. I. The influence of low levels of turbulence on fragmentation and multiplicity. Astron Astrophys 414:633–650
Monaghan JJ, Gingold RA (1983) Shock simulation by the particle method SPH. J Comput Phys 52:374–389
Offner SSR, Klein RI, McKee CF (2008) Driven and decaying turbulence simulations of low-mass star formation: from clumps to cores to protostars. Astrophysical J 686:1174–1194
Springel V (2005) The cosmological simulation code GADGET-2. Mon Not R Astron Soc 364:1105–1134
Tafalla M, Myers PC, Caselli P, Walmsley CM (2004) On the internal structure of starless cores. I. Physical conditions and the distribution of CO, CS, N\({_{2}}\)H\({^{+}}\), and NH\({_{3}}\) in L1498 and L1517B. Astron Astrophys 416:191–212
Whithworth AP, Ward-Thompson D (2001) An empirical model for protostellar collapse. Astrophys J 547:317–322
Acknowledgments
We would like to thank ACARUS-UNISON for the use of their computing facilities in the making of this chapter. This work was partially supported by the Consejo Nacional de Ciencia y Tecnología of Mexico (CONACyT) under the project Abacus CONACYT-EDOMEX-2011-C01-165873.
Author information
Authors and Affiliations
Corresponding author
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 2014 Springer International Publishing Switzerland
About this chapter
Cite this chapter
Arreaga-García, G., Klapp, J. (2014). Comparing Accretion Centres Between Rotating and Turbulent Cloud Cores. In: Sigalotti, L., Klapp, J., Sira, E. (eds) Computational and Experimental Fluid Mechanics with Applications to Physics, Engineering and the Environment. Environmental Science and Engineering(). Springer, Cham. https://doi.org/10.1007/978-3-319-00191-3_36
Download citation
DOI: https://doi.org/10.1007/978-3-319-00191-3_36
Published:
Publisher Name: Springer, Cham
Print ISBN: 978-3-319-00190-6
Online ISBN: 978-3-319-00191-3
eBook Packages: Earth and Environmental ScienceEarth and Environmental Science (R0)