Hostname: page-component-8448b6f56d-tj2md Total loading time: 0 Render date: 2024-04-19T14:17:08.451Z Has data issue: false hasContentIssue false
  • English
  • Français

Beyond single-stream with the Schrödinger method

Published online by Cambridge University Press:  12 October 2016

Cora Uhlemann  and
Michael Kopp
Cora Uhlemann
Affiliation:
Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Arnold Sommerfeld Center for Theoretical Physics, LMU, Theresienstr. 37, D-80333 Munich
Michael Kopp
Affiliation:
Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching, Arnold Sommerfeld Center for Theoretical Physics, LMU, Theresienstr. 37, D-80333 Munich
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We investigate large scale structure formation of collisionless dark matter in the phase space description based on the Vlasov-Poisson equation. We present the Schrödinger method, originally proposed by \cite{WK93} as numerical technique based on the Schrödinger Poisson equation, as an analytical tool which is superior to the common standard pressureless fluid model. Whereas the dust model fails and develops singularities at shell crossing the Schrödinger method encompasses multi-streaming and even virialization.

Keywords

large scale structurecold dark mattercosmic webhalo formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S308: The Zeldovich Universe: Genesis and Growth of the Cosmic Web , June 2014 , pp. 115 - 118
Copyright
Copyright © International Astronomical Union 2016 

References

Dominguez, , 2000, Phys.Rev., D62:103501.Google Scholar
Hahn, , Angulo, & Abel, , 2014, arXiv:1404.2280.Google Scholar
He, , 2012, MNRAS, 419:1667–1681, 1103.5730.CrossRefGoogle Scholar
Kopp, & Uhlemann, et al., 2014, in preparation.CrossRefGoogle Scholar
Lynden-Bell, , 1967, MNRAS, 136:101.Google Scholar
Melott, , Pellman, & Shandarin, , 1994, MNRAS, 269:626, arXiv:astro-ph/9312044.CrossRefGoogle Scholar
Navarro, , Frenk, & White, , ApJ, 490:493, arXiv:astro-ph/9611107.CrossRefGoogle Scholar
Pueblas, & Scoccimarro, , 2009, Phys.Rev., D80:043504, arXiv:0809.4606.Google Scholar
Takahashi, , 1989, Progress of Theoretical Physics Supplement, 98:109–156.Google Scholar
Uhlemann, & Kopp, , 2014, arXiv:1407.4810.Google Scholar
Uhlemann, , Kopp, & Haugg, , 2014, Phys.Rev., D90:023517, arXiv:1403.5567.Google Scholar
Widrow, & Kaiser, , 1993, Ap. Lett., 416:L71.Google Scholar
Zel'dovich, , 1970, A&A, 5:84–89.Google Scholar