By Markus Kuster, Georg Raffelt, Berta Beltrán
Axions are extraordinary hypothetical debris which can either clear up the CP challenge of quantum chromodynamics and even as account for the darkish subject of the universe. in keeping with a chain of lectures by means of global specialists during this box held at CERN (Geneva), this quantity presents a pedagogical advent to the speculation, cosmology and astrophysics of those interesting debris and provides an up to date account of the prestige and prospect of ongoing and deliberate experimental searches. inexperienced persons and practitioners of astroparticle physics will locate during this publication either a concise creation and a present reference paintings to a show off subject that connects the “inner area” of the uncomplicated particle global with the “outer house” of the universe at large.
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Extra resources for Axions: Theory, Cosmology, and Experimental Searches
Phys. B 311, 253 (1988) 40 41. : Phase-space structure of cold dark matter halos. Phys. Lett. B 291, 288 (1992) 41 42. : Robustness of discrete flows and caustics in cold dark matter cosmology. Phys. Rev. D 72, 083513 (2005) [astro-ph/0508049] and references therein 41 2 Axion Cosmology 49 43. : Axion miniclusters. Phys. Lett. B 205, 228 (1988) 42, 43 44. : Axion miniclusters and Bose stars. Phys. Rev. Lett. 71, 3051 (1993) [hep-ph/9303313] 42 45. : Femtolensing and picolensing by axion miniclusters.
II axions do homogenize and hence the axion energy density has a smooth component at teq . However, pop. II axions may get gravitationally bound to miniclusters later on. It seems rather diﬃcult to model this process reliably. A discussion is given in . It is concluded there that the accretion of pop. II axions results in miniclusters that have an inner core of pop. I axions with density of order 10−18 g cm−3 and a fluﬀy envelope of pop. II axions with density of order 10−25 g cm−3 . When a minicluster falls onto a galaxy, tidal forces are apt to destroy it.
2 String Decay The evolution of axion strings between the PQ and QCD phase-transitions was discussed in Sect. 3. The number density of axions emitted in string 38 P. 70) in terms of the quantities ξ, r¯, and χ that we introduced to parameterize our ignorance of various aspects of string evolution and decay. Because their spectrum dna /dk ∝ k −2 in the range t−1 k (tPQ t)−1/2 , the bulk of axions emitted in string-decay have momenta of order t−1 at 1 time t1 and become non-relativistic soon after they acquire mass.