Particle Physics

Dark Matter in Astrophysics and Particle Physics 1998: by L Baudis, H. V. Klapdor-Kleingrothaus

By L Baudis, H. V. Klapdor-Kleingrothaus

One of many significant open questions in excessive strength physics and cosmology is the character and foundation of darkish subject. darkish topic in Astrophysics and Particle Physics 1998 offers a accomplished review of the present prestige of study during this topical box. The e-book brings jointly top researchers from worldwide to check fresh growth and destiny instructions for learn within the diverse ways to the darkish subject challenge. It collects effects from cosmology, large-scale constitution, and accelerator and nonaccelerator physics. The e-book additionally reports the correlations among and the virtues of every of the fields for the decision of abundance, nature, and foundation of darkish subject.

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Additional resources for Dark Matter in Astrophysics and Particle Physics 1998: Proceedings of the Second International Conference on Dark Matter in Astro and Particle Physics, held in Heidelberg, Germany, 20-25 July 1998

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1, we mentioned the caveat that we have assumed that the contribution to the spectra from sub-horizon modes should be negligible. This is probably the case in the 52 53 most commonly studied defect based theories, cosmic strings and textures, but it is important to realize that the many other, more complicated defect models could possibly exist. It has been suggested [56] that it might be possible to form a network of strings connected by monopoles, which act like beads on cosmic necklaces. In this case, the correlation length of the string network may be much smaller and consequently the rms velocity of the network  which should be of order the correlation length relative to the horizon  will also be small, that is, in the language of the model for strings already discussed ξ ~ v << 1.

This can be seen very clearly when compared to the spectrum of just the inflationary contribution. It has been reported recently that such a feature might exist in the observed power spectrum [55], although it is unclear whether an accurate comparisons can be made since the length scales that we are considering are in the non-linear regime. It will be interesting to compare these models with the observations of the forthcoming galaxy surveys. An interesting by-product of this increase in the power on small scales will be a proportionate increase in the number objects forming at high redshifts.

It should be noted that once b100 is fixed, then removing any unwanted power on small scales can be achieved by the modifications to cosmological parameters. We should finally comment that the 'b100 problem' is not a no go theorem, being more phenomenologically based. There are, for example, source models which can almost mimic the predictions of adiabatic models [37, 38], although none of these models appears to have any kind of physical relevance for any realistic defect-based model. We should note that we have also assumed that super-horizon modes dominate the structure formation process.

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