Hostname: page-component-cd9895bd7-dk4vv Total loading time: 0 Render date: 2024-12-23T11:10:39.799Z Has data issue: false hasContentIssue false
  • English
  • Français

Higher-order Lagrangian perturbative theory for the Cosmic Web

Published online by Cambridge University Press:  12 October 2016

Takayuki Tatekawa  and
Shuntaro Mizuno
Takayuki Tatekawa
Affiliation:
Center for Infromation Initiative, University of Fukui, 3-9-1 Bunkyo, Fukui, Fukui, 910-8507, Japan email: [email protected] Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo, 169-8555, Japan
Shuntaro Mizuno
Affiliation:
Waseda Institute for Advanced Study, Waseda University, 1-6-1 Nishi-Waseda, Shinjuku, Tokyo, 169-8050, Japan
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.

Zel'dovich proposed Lagrangian perturbation theory (LPT) for structure formation in the Universe. After this, higher-order perturbative equations have been derived. Recently fourth-order LPT (4LPT) have been derived by two group. We have shown fifth-order LPT (5LPT) In this conference, we notice fourth- and more higher-order perturbative equations. In fourth-order perturbation, because of the difference in handling of spatial derivative, there are two groups of equations. Then we consider the initial conditions for cosmological N-body simulations. Crocce, Pueblas, and Scoccimarro (2007) noticed that second-order perturbation theory (2LPT) is required for accuracy of several percents. We verify the effect of 3LPT initial condition for the simulations. Finally we discuss the way of further improving approach and future applications of LPTs.

Keywords

large-scale structure of universemethods: analytical
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. 119 - 120
Copyright
Copyright © International Astronomical Union 2016 

References

Buchert, T. 1992, Mon. Not. R. Astron. Soc., 254, 729 Google Scholar
Barrow, J. D. & Saich, P. 1993, Class. Quantum Grav., 10, 79 Google Scholar
Bouchet, F. R., Juszkiewicz, R., Colombi, S., & Pellat, R. 1992, Astrophys. J., 394, L5 Google Scholar
Buchert, T. & Ehlers, J. 1993, Mon. Not. R. Astron. Soc., 264, 375 Google Scholar
Buchert, T. 1994, Mon. Not. R. Astron. Soc., 267, 811 Google Scholar
Bouchet, F. R., Colombi, S., Hivon, E., & Juszkiewicz, R. 1995 Astron. Astrophys., 296, 575 Google Scholar
Catelan, P. 1995, Mon. Not. R. Astron. Soc., 276, 115 Google Scholar
Crocce, M., Pueblas, S., & Scoccimarro, R. 2006 Mon. Not. R. Astron. Soc., 373, 369 Google Scholar
Ma, C.-P. & Bertschinger, E. 1995 Astrophys. J., 455, 7 Google Scholar
Peebles, P. J. E. 1984, Astrophys. J., 284, 439 Google Scholar
Rampf, C. & Buchert, T. 2012, J. Cosmol. Astropart. Phys., 06, 021 CrossRefGoogle Scholar
Rampf, C. 2012, J. Cosmol. Astropart. Phys., 12, 004 Google Scholar
Sasaki, M. & Kasai, M. 1998 Prog. Theor. Phys., 99, 585 CrossRefGoogle Scholar
Tatekawa, T. & Mizuno, S. 2007, J. Cosmol. Astropart. Phys. 12 014 Google Scholar
Tatekawa, T. 2013, Prog. Theor. Exp. Phys., 013E03Google Scholar
Tatekawa, T. 2014, J. Cosmol. Astropart. Phys., 04, 025 CrossRefGoogle Scholar
Zel'dovich, Ya. B. 1970, Astron. Astrophys., 5, 84 Google Scholar