Accretion Centers Induced in a Molecular Cloud Core After a Penetrating Collision

  • G. Arreaga-GarcíaEmail author
  • J. Klapp
Conference paper
Part of the Environmental Science and Engineering book series (ESE)


The aim of this paper is to present a set of numerical simulations of a penetrating collision, in which a small gas core (the bullet) penetrates a larger gas core (the target). In the target core, the gravitational collapse is supposed to be ongoing before the collision. Each colliding core has a uniform density profile and rigid body rotation; besides the mass and size of the target core have been chosen to represent the observed molecular cloud core L1544. We modified the Lagrangian code \(\textit{Gagdet}2\) to identify when a gas particle can become an accretion center, and to inherit the mass and momentum of all the very close neighboring particles. Three collision models are here considered for pre-collision velocities \(v/c_0=\) \(2.5\), \(5.0\), and \(10\) Mach. The outcome of these collision models are presented only for two different values of the bullet’s radius, that is for \(R_0/4\), and \(R_0/2\) where \(R_0\) is the radius of the target core. Such collision models reveal how accretion centers are formed, with a spatial distribution that strongly depends on the pre-collision velocity. We thus show hereby that penetrating collisions may have a major and favorable influence in the star formation process.


Gravitational Collapse Rigid Body Rotation Collision Model Collision System Target Core 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.



We would like to thank ACARUS-UNISON for the use of their computing facilities. This work has been partially supported by the Consejo Nacional de Ciencia y Tecnología of Mexico (CONACyT) under the project CONACyT-EDOMEX-2011-C01-165873.


  1. Anathpindika S (2009) Supersonic cloud collision. Astron Astrophys 504:437–450CrossRefGoogle Scholar
  2. Anathpindika S (2010) Collision between dissimilar clouds: stability of the bow-shock, and the formation of prestellar cores. Mon Not Roy Astron Soc 405:1431–1443Google Scholar
  3. Arreaga-Garcia G, Klapp J, Saucedo-Morales J (2014) Simulations of colliding uniform density H2 clouds. Int J Astron Astrophys 4:192–220CrossRefGoogle Scholar
  4. Balsara DS (1995) von Neumann stability analysis of smooth particle hydrodynamics: suggestions for optimal algorithms. J Comput Phys 121:357–372CrossRefGoogle Scholar
  5. Boss AP, Fisher RT, Klein R, McKee CF (2000) The Jeans condition and collapsing molecular cloud cores: filament or binaries? Astrophys J 528:325–335CrossRefGoogle Scholar
  6. Higuchi AE, Chibueze-Asao JO, Tasker EJ, Ken-Takahira K, Takano S (2014) ALMA view of GO.25+0.016: can cloud-cloud collision form the cloud? Astrophys J 147(6):7Google Scholar
  7. Monaghan JJ, Gingold RA (1983) On the fragmentation of differentially rotating clouds. Mon Not Roy Astron Soc 204:715–733CrossRefGoogle Scholar
  8. Springel V (2005) The cosmological simulation code Gadget-2. Mon Not Roy Astron Soc 364:1105–1134CrossRefGoogle Scholar
  9. Whitworth AP, Ward-Thompson D (2001) An empirical model for protostellar collapse. Astrophys J 547:317–322CrossRefGoogle Scholar

Copyright information

© Springer International Publishing Switzerland 2015

Authors and Affiliations

  1. 1.Departamento de Investigación En Física de la Universidad de SonoraHermosilloMexico
  2. 2.Instituto Nacional de Investigaciones Nucleares, ININMexicoMexico
  3. 3.Departamento de MatemáticasCinvestav Del I.P.N.MexicoMexico

Personalised recommendations