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Semi analytic calculation of cosmic microwave background anisotropies from wiggly and superconducting cosmic strings

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Figure

Figure 1. The constraint (74) on the square of the rms veloc-ity, v2, depending on the expansion rate n and the amount ofwiggles µ.
Figure 2. Evolution of the rms velocity υ, comoving characteristic length Lc and amount of wiggles µ as a function of redshiftz for wiggly cosmic string networks with different values of the parameter D, obtained by a modified version of the CMBactcode [43]
Figure 3. CMB anisotropy for wiggly cosmic string networks obtained by a modified version of the CMBact code [43]
Figure 4. Dependence of the scaling values of the rms velocity, v, and the comoving correlation length divided by conformaltime, ε, on the amount of wiggles µ for different expansion rates n.
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