Flat cosmology with collisionless cold dark matter (CDM) and cosmological constant (ΛCDM cosmology) may have some problems on small scales, even though it has been very successful on large scales. We study the effect of Self-Interacting Dark Matter (SIDM) hypothesis on the density profiles of halos. Collisionless CDM predicts cuspy density profiles toward the center, while observations of low mass galaxies prefer cored profiles. SIDM was proposed by Spergel & Steinhardt  as a possible solution to this cuspy profile problem on low-mass scales. On the other hand, observations and collisionless CDM agree on mass scales of galaxy clusters. It is also known that the SIDM hypothesis would contradict with X-ray and gravitational lensing observations of cluster of galaxies, if the cross section were too large. Our final goal is to find the range of SIDM scattering cross section models that are consistent with those astrophysical observations in two different mass scales.
There are two theoretical approaches to compute the effect of self-interacting scattering – Gravitational N-body simulation with Monte Carlo scattering and conducting fluid model; those two approaches, however, had not been confirmed to agree with each other. We first show that two methods are in reasonable agreement with each other for both isolated halos and for halos with realistic mass assembly history in an expanding ΛCDM universe; the value of cross section necessary to have a maximally relaxed low-density core in ΛCDM is in mutual agreement.
We then develop a semianalytic model that predicts the time evolution of SIDM halo. Our semianalytic relaxation model enables us to understand how a SIDM halo would relax to a cored profile, and obtain an ensemble of SIDM halos from collisionless simulations with reasonable computational resources. We apply the semianalytic relaxation model to CDM halos, and compare the resulting statistical distribution of SIDM halos with astrophysical observations. We show that there exists a range of scattering cross sections that simultaneously solve the cuspy core problem on low-mass scales and satisfy the galaxy cluster observations.
We also present that other potential conflicts between ΛCDM and observations could be resolved in Part II and III.
|Advisor:||Shapiro, Paul R.|
|Commitee:||Dicus, Duane A., Komatsu, Eiichiro, Matzner, Richard A., Weinberg, Steven|
|School:||The University of Texas at Austin|
|School Location:||United States -- Texas|
|Source:||DAI-B 71/08, Dissertation Abstracts International|
|Keywords:||Boltzmann-Newton system, Halo formation, Large-scale structure, Self-interacting dark matter|
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