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Dark Matter Haloes and the Free Streaming Scale

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Dark Matter Haloes and the Free Streaming Scale Zurich Open Repository and Archive University of Zurich Main Library Strickhofstrasse 39 CH-8057 Zurich www.zora.uzh.ch Year: 2012 Dark matter structures and the free streaming scale Schneider, Aurel Posted at the Zurich Open Repository and Archive, University of Zurich ZORA URL: https://doi.org/10.5167/uzh-75587 Dissertation Published Version Originally published at: Schneider, Aurel. Dark matter structures and the free streaming scale. 2012, University of Zurich, Faculty of Science. Dark Matter Structures and the Free Streaming Scale Dissertation zur Erlangung der naturwissenschaftlichen Doktorw¨urde (Dr. sc. nat.) vorgelegt der Mathematisch-naturwissenschaftlichen Fakult¨at der Universit¨at Z¨urich von Aurel Schneider von D¨orflingen SH Promotionskomitee Prof. Dr. Ben Moore (Vorsitz) Prof. Dr. J¨urg Diemand Z¨urich, 2012 3 Aurel Schneider Institute for Theoretical Physics University of Zurich Winterthurerstrasse 190 CH-8057 Z¨urich Switzerland [email protected] c Aurel Schneider 2012 All rights reserved. No part of this document may be reproduced without the written permission of the publisher. 4 Contents Acknowledgments 7 Abstract 9 Zusammenfassung 10 1. Introduction 13 2. Theoretical background 17 2.1. Cosmichistory .............................. 17 2.2. DarkMatter................................ 19 2.2.1. Colddarkmatter(CDM) . 20 2.2.2. Warmdarkmatter(WDM) . 21 2.3. Linearstructureformation . 21 2.3.1. Particlemotion . 22 2.3.2. CollisionlessBoltzmannequation . 22 2.3.3. The Jeans criterion and the free streaming scale . ... 25 2.4. Statistical description of the density field . ....... 27 2.4.1. Basicconcepts. 27 2.4.2. Gaussianrandomfield . 28 2.5. Nonlinearstructureformation . 29 2.5.1. Numericalsimulations . 29 2.5.2. Approximative analytical approaches . 31 3. Paper I: CDM microhaloes 35 4. Paper II: WDM structure formation 43 5. Paper III: Stability of tidal streams 61 6. Prospects 71 6.1. Halo mass function around the free streaming scale . ..... 71 6.2. HaloconcentrationsinΛWDM . 72 6.3. Fragmentationincosmicfilaments. 72 Bibliography 75 6 Acknowledgments The Institute for Theoretical Physics at the University of Zurich is a wonderful place for doing a PhD, and I want to thank everyone contributing to this unique working atmosphere. I am especially grateful to my supervisor Ben Moore, who gave me the oppor- tunity to work on various different research projects and was always there when needed. His numerous advices have been crucial for accomplishing this thesis. I also want to thank Robert Smith for co-advising the thesis, for sharing his expertise, and for a very pleasant collaboration. I very much appreciated to collaborate with Doninno Anderhalden, Gianfranco Bertone, J¨urg Diemand, Lawrence Krauss, Andrea Macci`o, Doug Potter, Darren Reed, and Joachim Stadel, and I am grateful for many inspiring discussions. Special thanks go to Doug Potter for always being patient and for helping with various computational problems. Finally I want to thank my small new family for simply being here and for sharing the not always easy life of a researcher. 8 Abstract This thesis is about various aspects of dark matter structure formation under the influence of the velocity free streaming effect. Depending on the nature of dark matter, the free streaming can act on very different scales, going from the AU scale for a usual cold dark matter particle up to the scale of dwarf galaxies for a warm dark matter candidate. The effect of the free streaming may be observable and could give important hints on the nature of the dark matter particle. In a first part of the thesis we are looking at the disruption processes acting on the smallest earth-mass haloes in a 100 GeV neutralino dark matter scenario. The existence of such microhaloes in the solar neighborhood would be very interesting for direct and indirect dark matter detection experiments. We however show that tidal stripping as well as the disk passages destroy the major part of the microhalo, and that the effect on direct and indirect detection is negligible. In a second part we are considering a warm dark matter cosmology, studying nonlinear power spectrum, mass function, bias, and concentrations. We find a sur- prising behavior of the mass function and the concentration, and we interpret it as a consequence of a reversed hierarchy of structure formation. In the final part of the thesis we study the cylindrical collapse within tidal streams. In a cylindrical geometry the Jeans length is increased with respect to a homogeneous case, and structure formation is suppressed more efficiently. We find that tidal streams do not gravitationally fragment, since they are not cold enough to allow substantial growth of perturbations. 10 Zusammenfassung Diese Thesis handelt von unterschiedlichen Aspekten der kosmischen Strukturfor- mation, welche dominiert wird von dunkler Materie. Zentraler Bestandteil ist dabei der sogenannte “free-streaming” Effekt, der ein Ausdruck f¨ur die Geschwindigkeits- dispersion eines kollisionsfreien Fluides ist und zu einer Unterdr¨ukung der Struktur- bildung auf kleinen Skalen f¨uhrt. Wie klein diese kritische free-streaming Skala ist, h¨angt ab von der Art des hypothetischen dunklen Materie-Teilchens und liegt im Bereich zwischen der Gr¨osse des inneren Sonnensystemes f¨ur “kalte” dunkle Materie (CDM) und der Gr¨osse von Zwerggalaxien f¨ur “warme” dunkle Materien (WDM). Der free-streaming Effekt, k¨onnte unter Umst¨anden beobachtbar sein und w¨urde dann Aufschluss geben, ¨uber die Art des hypothetischen dunkle Materie-Teilchens. In einem ersten Teil der Thesis betrachten wir den zerst¨orerischen Einfluss des galaktischen Halos auf die kleinsten Strukturen in einem CDM Szenario mit einem 100 GeV Neutralino. Diese Strukturen werden “Mikrohalos” genannt und sind nur etwa eine Erdmasse schwer. F¨ur direkte und indirekte Detektionsexperimente von dunkler Materie w¨are die Existenz von Mikrohalos im oder um das Sonnensystems von grosser Bedeutung. Wir zeigen jedoch, dass Gezeitenkr¨afte und Gravitation- swechselwirkung mit Sternen einen Grossteil der Mikrohalos zerst¨ort, oder so stark komprimiert, dass sie keinen Einfluss mehr auf Detektionsexperimente haben. In einem zweiten Teil betrachten wir eine WDM Kosmologie, wobei wir die nicht- lineare spektrale Leistungsdichte, die Massenfunktion und die Konzentration der Halos, sowie den “bias” untersuchen. Die Massenfunktion und die Konzentration zeigen ein ¨uberraschendes Verhalten, welches als Zeichen einer Umkehrung der hi- erarchischen Strukturbildung interpretiert werden kann. In dem dritten und letzten Teil der Thesis betrachten wir den Gravitations- Kollaps innerhalb eines Zylinders und wenden dieses Modell an auf Gezeitenstr¨ome (tidal streams) von Substrukturen in einem galaktischen Halo. Wir zeigen, dass “tidal streams” auf Grund ihrer grossen Geschwindigkeitsdispersion stabil sind und nicht fragmentieren. 12 1 INTRODUCTION This thesis is a summary of my research activities of the last three to four years. It is not a self consistent work nor does it contain one single research hypothesis, but it is a patchwork of different research projects I have worked on during the time of my PhD. There are however common points relating the different projects, which are the dark matter structure formation and, more specifically, the velocity free streaming effect. The thesis consists of a general introduction into the research field followed by three published papers and ending with an outlook to future work. I will now give a short overview of the research done in these papers, and discuss how the different subjects are related to the thesis as a whole. The first paper is about the local dark matter distribution within a ΛCDM cosmology. This is of great interest for the search of the dark matter particle, since the interpretation of detection experiments depends on the local dark matter den- sity. Because of the very nonlinear behavior of small scale structure formation and the finite resolution of N-body simulations, it is however impossible to determine the precise distribution at the local scale of our solar system. We perform analytical approximations and toy model simulations to estimate the local dark matter dis- tribution. We thereby assume a hierarchical structure formation, which means that the smallest structures, called microhaloes, form very early, have high concentra- tions and are therefore the most susceptible to survive the disrupting forces within the Milky way halo. The mass of the microhaloes is determined by the primordial CDM free streaming scale which depends on the nature and mass of the dark matter particle candidate. Assuming a 100 GeV neutralino the microhalo mass is extremely −6 small, comparable to the one of the earth, i.e. 10 M⊙. In order to determine the influence of microhaloes on the dark matter distribution, we estimate their number density in the Milky Way halo as well as their resistance to disruption effects, such as tidal streaming and interactions with stars in the galactic disk. We find that only the very centers of the microhaloes survive and more than 95% of the initial mass is Chapter 1: Introduction stripped away. The boosting effect of this remnants on direct and indirect detection stays negligibly small. We also explore the local velocity distribution which could show signatures from the initially very cold tidal streams of disrupted microhaloes. The streams are however heated up by stars in the disk, and spikes in phase space are completely washed out, leading to a quasi Maxwellian velocity distribution.
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