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On a dense energy grid reaching up to 75 meV electron collision energy the fragmentation angle and the kinetic energy release of neutral dissociative recombination fragments have been studied in a twin merged beam experiment. The anisotropy described by Legendre polynomials and the extracted rotational state contributions were found to vary on a likewise narrow energy scale as the rotationally averaged rate coefficient. For the first time angular dependences higher than 2$^{nd}$ order could be deduced. Moreover, a slight anisotropy at zero collision energy was observed which is caused by the flattened velocity distribution of the electron beam., Comment: 8 pages, 4 figures; The Article will be published in the proceedings of DR 2007, a symposium on Dissociative Recombination held in Ameland, The Netherlands (18.-23. July 2008); Reference 19 has been published meanwhile in S. Novotny, PRL 100, 193201 (2008)

This paper looks at a class of closed orientable 3-manifolds constructed from a gluing of three handlebodies, such that the inclusion of each handlebody is $\pi_1$-injective. This construction is the generalisation to handlebodies of the condition for gluing three solid tori to produce non-Haken Seifert fibered 3-manifolds with infinite fundamental group. It is shown that there is an efficient algorithm to decide if a gluing of handlebodies meets the disk-condition. Also an outline for the construction of the characteristic variety (JSJ decomposition) in such manifolds is given. Some non-Haken and atoroidal examples are given., Comment: 36 pages, 24 figures. Mainly gramatical changes and two figures added

This review concerns the origin and the possible effects of magnetic fields in the early Universe. We start by providing to the reader with a short overview of the current state of art of observations of cosmic magnetic fields. We then illustrate the arguments in favour of a primordial origin of magnetic fields in the galaxies and in the clusters of galaxies. We argue that the most promising way to test this hypothesis is to look for possible imprints of magnetic fields on the temperature and polarization anisotropies of the cosmic microwave background radiation (CMBR). With this purpose in mind, we provide a review of the most relevant effects of magnetic fields on the CMBR. A long chapter of this review is dedicated to particle physics inspired models which predict the generation of magnetic fields during the early Universe evolution. Although it is still unclear if any of these models can really explain the origin of galactic and intergalactic magnetic fields, we show that interesting effects may arise anyhow. Among these effects, we discuss the consequences of strong magnetic fields on the big-bang nucleosynthesis, on the masses and couplings of the matter constituents, on the electroweak phase transition, and on the baryon and lepton number violating sphaleron processes. Several intriguing common aspects, and possible interplay, of magnetogenesis and baryogenesis are also dicussed., Comment: 152 LaTeX pages, 6 figures., final version to appear in Phys. Rep

We put bounds on the variation of the value of the fine structure constant $\alpha$, at the time of Big Bang nucleosynthesis. We study carefully all light elements up to $^7$Li. We correct a previous upper limit on $|\Delta \alpha / \alpha|$ estimated from $^4$He primordial abundance and we find interesting new potential limits (depending on the value of the baryon-to-photon ratio) from $^7$Li, whose production is governed to a large extent by Coulomb barriers. The presently unclear observational situation concerning the primordial abundances preclude a better limit than $|\Delta \alpha/\alpha| \lsim 2\cdot 10^{-2}$, two orders of magnitude less restrictive than previous bounds. In fact, each of the (mutually exclusive) scenarios of standard Big Bang nucleosynthesis proposed, one based on a high value of the measured deuterium primordial abundance and one based on a low value, may describe some aspects of data better if a change in $\alpha$ of this magnitude is assumed., Comment: 21 pages, eps figures embedded using epsfig macro

We investigate, through Monte-Carlo simulations, the nature of the second order point in a $Z_2$ (Bosonic) + $Z_2$ gauge theory in four dimensions. Detailed analysis of the critical exponents point to the Ising universality class. Relevancy to extended models and possible Non-Gaussian behavior is discussed., Comment: 4 pages, 6 figures, LaTex

The recent observations of 50 TeV gamma radiation by HEGRA have the potential of determining the extragalactic flux of infrared radiation. The fact that radiation is observed in the range between 30 and 100 TeV sets an upper limit on the infrared flux, while a cutoff at $E_{\gamma} \approx 50$ TeV fixes this flux with a good accuracy. If the intrinsic radiation is produced due to interaction of high energy protons with gas or low-energy target photons, then an accompaning high-energy neutrino flux is unavoidable. We calculate this flux and underground muon flux produced by it. The muon flux is dominated by muons with energies about 1 TeV and can be marginally detected by a 1 km$^2$ detector like an expanded AMANDA., Comment: 9 pages, latex2e, 3 eps figures

In view of several conflicting results, we reanalyze the effects of magnetic fields on the primordial nucleosynthesis. In the case the magnetic field is homogeneous over a horizon volume, we show that the main effects of the magnetic field are given by the contribution of its energy density to the Universe expansion rate and the effect of the field on the electrons quantum statistics. Although, in order to get an upper limit on the field strength, the weight of the former effect is numerically larger, the latter cannot be neglected. Including both effects in the PN code we get the upper limit $B \le 1\times 10^{11}$ Gauss at the temperature $T = 10^9~^oK$. We generalize the considerations to cases when instead the magnetic is inhomogeneous on the horizon length. We show that in these cases only the effect of the magnetic field on the electrons statistics is relevant. If the coherence length of the magnetic field at the end of the PN is in the range $10 \ll L_0 \ll 10^{11}$ cm our upper limit is $B \le 1\times 10^{12}$ Gauss., Comment: 12 pages LaTex file with two included ps figs

We study the variation of the hadron masses in the presence of external magnetic fields of strength of the order of the masses themselves. We identify the main factors affecting the lattice simulation results: - the boundary discontinuities for $eB << 2\pi / L^2 a^2$. - the SU(6) choice of the hadron wave-function. We confirm qualitatively the earlier theoretical ansatz on the linear behaviour of the masses with the magnetic field and, as a by-product, we improve the lattice measurements of the nucleon magnetic moments. However our systematic and statistical errors preclude us from measuring the theoretically predicted field strength at which the proton becomes heavier than the neutron., Comment: 18 pages, compressed uuencoded postscript file

We compute the variation of the masses of the proton and the neutron induced by the presence of a strong external magnetic field. We discuss the choice of the wave function and different techniques how to apply the magnetic field. The results obtained from a 24 16^2 8 and a 16^2 8^2 lattice are compared with a phenomenological approach., Comment: 3 pages, PostScipt, compressed, uuencoded, contribution to Lattice 94

Expected atmospheric ${\bar \nu_e}$ fluxes will result in a significant number of resonantly produced low mass hadronic vector states, as the $\rho$, in large volume neutrino telescopes. The existence of sources of higher energy neutrinos will result in the production of higher mass states, as the $D_s^*$ and the $({\bar t}b)_{J=1}$. We calculate the rates of production of these states and discuss their signals. Independent of theoretical flux determinations, the detection of these states will be a tool for experimentally determining these fluxes., Comment: pages, UCI-TR 94-10

Superconducting cosmic strings may be viewed as wires of thickness $1/\Lambda$ with $\Lambda=10^{16}$ TeV. We show that the weak interactions will spread out the current to distances $r= (1/M_Z)\ln (I/M_Z)$, where $I$ is the magnitude of the current in the string. Consequences for the scattering of light by these strings is presented., Comment: 7pages, UCI TR 93-28, LaTex with Revtex III macros

The GRANAT group (R. Sunyaev {\it et al.\/}, Central Bureau of Astronomical Telegrams, International Astronomical Union, Circular No.~5481) recently reported the observation of a $(545 \pm 11)$ keV line in the spectrum of the Crab Nebula. It is tempting to associate this with the positron-electron annihilation line at 511 keV. If this line originates from some transition at the surface of the neutron star in the Crab, we expect a red shift of around 10\% rather then the observed blue shift of $\sim 35$ keV; in fact, this gravitational red shift implies that the natural frequency of the observed line is also 10\% higher, or around 600 keV. In this article we shall present a mechanism for generating such a split from 511 keV. For this mechanism to be successful we require: (a) surface magnetic fields, in the annihilation region, to be $(3-8)\times 10^{12}$~G and to point in our direction, (b) surface densities of $(10^5-10^6)$ g/cc. Both of these assumptions are consistent with pulsar models., Comment: pages (set in Revtex II)

A delicate interplay between the anomalous magnetic moments of the proton and neutron makes, in magnetic fields $B\ge 2\times 10^{14}$ T, the neutron stable and for fields $B\ge 5\times 10^{14}$ T the proton becomes unstable to a decay into a neutron via $\beta$ emission. Limits on the field strengths for which these arguments hold are presented and are related to questions of vacuum stability in the presence of such fields. Possible astrophysical consequences are discussed., Comment: 12 pages