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Magnetic monopole flux limits in primary cosmic radiation derived from muon-poor shower data and inverse Compton scattering
We relate the anomaly in the noise color of spin ice to the emergent nature of its magnetic monopoles and their random walk. Monopoles are quasi-particles, and the spin vacuum in which they wander is not structureless. Rather, the underlying spin ensemble filters the thermal white noise, leading to non-trivial coevolution. Thus, monopoles can be considered as "dressed" random walkers, activated by a non-trivial stochastic noise that subsumes mutual interactions and the coevolution of their spin vacuum. From this, we suggest that recent experimental results are interpretable in terms of monopole subdiffusion. Furthermore, we then conjecture relations between the color of the noise and other observables, such as relaxation time, monopole density, the dynamic exponent, and the order of the annihilation reaction, which suggests to us the introduction of spin-ice-specific critical exponents in a neighborhood of the ice manifold criticality.
In the analyses, published in Ref. [1], the exclusion limits are calculated in dependence of the mean free path of the magnetic monopole - nucleon catalysis interaction.
Schwinger quantization relation for magnetic charges derived by group theoretic method combining rotational and gauge invariances
No indication of slowly moving penetrating particles in cosmic radiation underground was found during two years observation. Particle velocity and pulse shape are main criteria for search. Probability of the imitation of slow particles (Beta 0.1) by atmospheric muons is negligible. Our upper limit on superheavy magnetic monopole flux is now 1.86 x 10 to the minus 15th power cm(-2) sr(-1) s(-1) (90% c.l.) for velocity range 2 x 0.0001 beta 0.1.
The survival of the Galactic magnetic field almost certainly sets an astrophysical upper bound of approx. 10 to the minus 15th power cm(-2) sr(-1) s(-1) on the flux of monopoles. To improve significantly upon this Parker limit with direct, real time searches would require a detector area of approx. 10,000 square meters and a collection time of years. Several such searches are being contemplated. A novel alternative scheme using large mica crystals capable of recording and storing tracks of slow monopoles over a time scale of approx. 10 to the 9th power years was proposed.
For several months in early 1965 the sun appeared to have large scale magnetic field directed outwards at nearly all latitudes and longitudes. Several independent observations that lead to this puzzling situation are discussed.
For three or four consecutive months in 1965 observations of the sun's magnetic field showed that it was predominantly directed out of the sun at all solar latitudes. This interval in the first part of 1965 is near the minimum of the sunspot cycle. Solar activity has been strongly associated with large-scale solar regions with field directed predominantly into the sun, while the observations noted seem to show that just near solar maximum there is almost no field observed to be directed into the sun. An attempt is made to describe and develop these interesting circumstances.
It is shown that galactic-disk monopoles could yield air showers which are stochastically aligned with the local Orion-arm magnetic field and which are above the energies of similarly aligned galactic heavy nuclei. In the absence of a cosmic-ray anisotropy, this method sets limits on the flux of galactic monopoles and their production cross sections. Limits based on the cosmic-ray anisotropy at 10 to the 19th power eV are presented. The possibility of stochastic alignment of inverse Compton photons from monopoles and 2.7 K black-body photons is considered. The resulting monopole-flux limits, based on the same data as those calculated by Osborne (1970), differ significantly from Osborne's limits, where the mechanisms of spiral-arm alignment and galactic containment are ignored.
The interactions of superheavy monopoles with stars of mass 0.6-25 solar masses are studied. It is shown that captured monopoles cluster near the stellar center, and that their contribution to the total stellar luminosity and their effects on the structure of stars will be unobservable as long as the flux is significantly below the Parker (1970, 1971) bound. It is suggested that all but the strongly magnetic stars will retain a substantial fraction of the monopoles they capture.
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