CMB Anisotropy Induced by a Moving Straight Cosmic String

TL;DR

This paper analyzes the CMB anisotropy caused by a moving straight cosmic string, proposing that combined optical and gravitational lensing methods improve detection, with specific anisotropy amplitudes and angular deficit parameters.

Contribution

It provides a detailed model of CMB anisotropy from straight cosmic strings and suggests combined detection methods for better identification.

Findings

CMB anisotropy amplitude ranges from 15-30 μK for certain string parameters.

Optical detection covers only 20% of cosmic strings, requiring combined methods.

Deficit angles for detection range from 0.1 to 6 arcseconds.

Abstract

We showed that the part of strings could be detected by optical method is only 20% from the total available amount of such objects, therefore the gravitational lensing method has to be "completed" by CMB one. We found the general structure of the CMB anisotropy generated by a cosmic string for simple model of straight string moving with constant velocity. For strings with deficit angle 1-2 arcsec the amplitude of generated anisotropy has to be 15-30 muK (the corresponding string linear density is (G mu) ~ 10^{-7} and energy is GUT one, 10^{15} GeV). To use both radio and optical methods the deficit angle has to be from 0.1 arcsec to 5-6 arcsec. If cosmic string can be detected by optical method, the length of corresponding brightness spot of anisotropy has to be no less than 100 degrees.