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Mikkel B. Johnson

Publications and source records attributed to Mikkel B. Johnson.

At least 19 recordsLinked to original sources

Simple and Accurate Oscillation Probabilities for Three Coupled Neutrinos Propagating in Matter

Within a conventional Hamiltonian description, we find accurate closed-form expressions for the oscillation probabilities of three coupled neutrinos propagating in matter. Subtle cancelations that occur in coefficients of our formulation are avoided for all transitions $ν_a \to ν_b$ by transforming to a different set of coefficients presented in an appendix of this paper. The neutrino mass eigenvalues are easily obtained numerically as the solution of a cubic equation. Our methods are illustrated for flavor-changing transitions in the $(ν_e,ν_μ)$ sector. The resulting analytic expressions oscillation probabilities, which are particularly simple, are also accurate to a few percent over all regions of interest at present and the envisioned future neutrino facilities. While somewhat less accurate than numerical simulations, our approximate expressions are sufficiently accuracy to obviate the need for exact computer simulations in many circumstances.

hep-ph

Regions of Applicability of Approximate Formulations of Neutrino Oscillations in Matter

We examine the reliability of the theoretical methods presently used for analysis and prediction of neutrino oscillation phenomena. Of particular interest are the limitations imposed by branch points when expansions in one of the small parameters of the Standard Neutrino Model (SNM) are made to obtain tractable results. Our evaluation compares the approximate oscillation probabilities for flavor-changing transitions in the $(ν_e , ν_μ)$ sector to exact results obtained from of a recently-developed exact analytical representation of neutrino oscillations in matter within the SNM. From our numerical comparisons, we are able to identify regions where the existing approaches can be improved to take full advantage of the higher quality data expected at future neutrino facilities.

hep-ph

Analytical Theory of Neutrino Oscillations in Matter with CP violation

We develop an exact analytical formulation of neutrino oscillations in matter within the framework of the Standard Neutrino Model assuming 3 Dirac Neutrinos. Our Hamiltonian formulation, which includes CP violation, leads to expressions for the partial oscillation probabilities that are linear combinations of spherical Bessel functions in the eigenvalue differences. The coefficients of these Bessel functions are polynomials in the neutrino CKM matrix elements, the neutrino mass differences squared, the strength of the neutrino interaction with matter, and the neutrino mass eigenvalues in matter. We give exact closed-form expressions for all partial oscillation probabilities in terms of these basic quantities. Adopting the Standard Neutrino Model, we then examine how the exact expressions for the partial oscillation probabilities might simplify by expanding in one of the small parameters α and sinθ13 of this model. We show explicitly that for small α and sinθ13 there are branch points in the analytic structure of the eigenvalues that lead to singular behavior of expansions near the solar and atmospheric resonances. We present numerical calculations that indicate how to use the small-parameter expansions in practice.

hep-ph

Sterile Neutrinos and Pulsar Velocities Revisited,

We calculate the momentum given to a proto neutron star during the first 10 seconds after temperature equilibrium is reached, using recent evidence of sterile neutrinos and a measurement of the mixing angle. This is a continuation of an earlier estimate with a wide range of possible mixing angles. Using the new mixing angle we find that sterile neutrinos can account for the observed pulsar velocities.

astro-ph.HE

Erratum for Time Reversal in Neutrino Oscillations

We suggested a new experiment for the MINOS project, with baseline L=735 km, to employ another detector at baseline 2L, which could measure TRV, as with a 10% e-mu conversion at distance L. There would be a 1% increase of the original flavor at 2L, which could be detected.

hep-ph

Neutrino Oscillation in Matter and Parameters $s_{13},δ_{CP}$

We estimate the dependence of $ν_μ$ to $ν_{e}$ conversion on parameters $θ_{13}$ and $δ_{CP}$ for several experimental facilities studying neutrino oscillations. We use the S-Matrix theory to estimate $\bar{ν_e}$ disappearance and compare estimates based on an older theory being used to extract $θ_{13}$ from the Double Chooz, Daya Bay, and RENO data, to assist in extracting an accurate value for $θ_{13}$ from these projects. We use values of $θ_{13}$ within known limits, and estimate the dependence of $ν_μ$ - $ν_{e}$ CP violation (CPV) probability on $δ_{CP}$ in order to suggest new experiments to measure CPV for neutrinos moving in matter.

hep-ph

Proposed TRV Measurement via L-nL Neutrino Oscillations

This is an extension of the L-2L experiment for measurement of time reversal violation (TRV) proposed in a recent publication. The main new aspects are taking into account the curvature of the earth's surface for long baseline neutrino beams, and recognizing that the matter effects disappear when the baseline is extended. A slight modification of the MINOS project, with a new detector at 2L, is proposed.

hep-ph

CP Violation in Neutrino Oscillations in Matter

We estimate CP violation for several experimental facilities studying neutrino oscillations. We also estimate the probability of $ν_μ$ to $ν_{e}$ conversion, using values of the parameter $θ_{13}$ within the known limits, in order to suggest new experiments to measure CP violation for neutrinos moving in matter.

hep-ph

Time Reversal in Neutrino Oscillations

We estimate the time reversal violations for neutrino oscillations in matter for typical experimental energies and baselines. We examine the present status of experiments on neutrino oscillations, propose experiments for TRV, and discuss the future.

hep-ph

Theory of Magnetic Seed-Field Theory of Magnetic Seed-Field Generation during the Cosmological First-Order Electroweak Phase Transition

We present a theory of the generation of magnetic seed fields in bubble collisions during a first-order electroweak phase transition (EWPT) possible for some choices of parameters in the minimal supersymmetric Standard Model. The theory extends earlier work and is formulated to assess the importance of surface dynamics in such collisions. We are led to linearized equations of motion with O(3) symmetry appropriate for examining collisions in which the Higgs field is relatively unperturbed from its mean value in the collision volume. Coherent evolution of the charged $W$ fields within the bubbles is the main source of the electromagnetic current for generating the seed fields, with fermions also contributing through the conductivity terms. We present numerical simulations within this formulation to quantify the role of the surface of the colliding bubbles, particularly the thickness of the surface, and to show how conclusions drawn from earlier work are modified. The main sensitivity arises such that the steeper the bubble surface the more enhanced the seed fields become. Consequently, the magnetic seed fields may be several times larger and smoother over the collision volume than found in earlier studies. Our work thus provides additional support to the supposition that magnetic fields produced during the EWPT in the early universe seed the galactic and extra-galactic magnetic fields observed today.

astro-ph.CO

EWPT Nucleation With MSSM and Electromagnetic Field Creation

Using EW-MSSM field theory, so the EWPT is first order, we derive the equations of motion for the gauge fields. With an isospin ansatz we derive e.o.m. for the electrically charged W fields uncoupled from all other fields. These and the lepton currents serve as the current for the Maxwell-like e.o.m. for the electromagnetic field. The electromagnetic field arising during EWPT bubble nucleation without leptons is found. We then calculate the electron current contribution, which is seen to be quite large. This provides the basis for determinining the magnetic field created by EWPT bubble collisions, which could seed galactic and extra-galactic magnetic fields.

astro-ph.CO

Magnetic Seed Field Generation from Electroweak Bubble Collisions, with Bubble Walls of Finite Thickness

Building on earlier work, we develop an equation-of-motion method for calculating magnetic seed fields generated from currents arising from charged W fields in bubble collisions during a first-order primordial electroweak phase transition allowed in some proposed extensions of the standard model. The novel feature of our work is that it takes into account, for the first time, the dynamics of the bubble walls in such collisions. We conclude that for bubbles with sufficiently thin surfaces the magnetic seed fields may be comparable to, or larger than, those found in earlier work. Thus, our results strengthen the conclusions of previous studies that cosmic magnetic fields observed today may originate from seeds created during the electroweak phase transition, and consequently that these fields may offer a clue relevant to extensions of the standard model.

astro-ph.CO

Large Mixing Angle Sterile Neutrinos and Pulsar Velocities

We investigate the momentum given to a protoneutron star, the pulsar kick, during the first 10 seconds after temperature equilibrium is reached. Using a model with two sterile neutrinos obtained by fits to the MiniBoone and LSND experiments there is a large mixing angle, and the effective volume for emission is calculated. Using formulations with neutrinos created by URCA processes in a strong magnetic field, so the lowest Landau level has a sizable probability, we find that with known paramenters the asymmetric sterile neutrino emissivity might account for large pulsar kicks.

astro-ph.CO

Pulsar Kicks With Sterile Neutrinos and Landau Levels

We use a model with two sterile neutrinos obtained by fits to the MiniBoone and LSND experiments. Using formulations with neutrinos created by URCA Processes in a strong magnetic field, so the lowest Landau level has a sizable probability, we find that with known paramenters the assymetric sterile neutrino emissivity might account for large pulsar kicks.

astro-ph

Electromagnetic Field Creation During EWPT Nucleation With MSSM

We derive the equations of motion for electroweak MSSM with a right-handed Stop, from which we derive the equations for the electromagnetic field that arises from bubble nucleation and collisions during the first order electroweak phase transition that can occur in this MSSM. Introducing an isospin ansatz we derive e.o.m. for the electrically charged W fields uncoupled from all other fields. These serve as the current for the Maxwell-like e.o.m. for the em field. The resulting electromagnetic field arising during EWPT bubble nucleation is found. This electromagnetic structure, along with that arising from bubble collisions, could seed galactic and extra-galactic magnetic fields.

hep-ph

Pulsar Kicks With Modified URCA and Electrons in Landau Levels

We derive the energy asymmetry given the proto-neutron star during the time when the neutrino sphere is near the surface of the proto-neutron star, using the modified URCA process. The electrons produced with the anti-neutrinos are in Landau levels due to the strong magnetic field, and this leads to asymmetry in the neutrino momentum, and a pulsar kick. The magnetic field must be strong enough for a large fraction of the eletrons to be in the lowest Landau level, however, there is no direct dependence of our pulsar velocity on the strength of the magnetic field. Our main prediction is that the large pulsar kicks start at about 10 s and last for about 10 s, with the corresponding neutrinos correlated in the direction of the magnetic field. We predict a pulsar velocity of 1.03 $\times 10^{-4} (T/10^{10}K)^7$ km/s, which reaches 1000 km/s if T $\simeq 9.96 \times 10^{10}$ K.

astro-ph

Role of Charged Gauge Fields in Generating Magnetic Seed Fields in Bubble Collisions during the Cosmological Electroweak Phase Transition

We calculate the magnetic field generated during bubble collisions in a first-order electroweak phase transition that may occur for some choices of parameters in the minimal supersymmetric Standard Model. We show that for sufficiently gentle collisions, where the Higgs field is relatively unperturbed in the bubble overlap region, the equations of motion can be linearized so that in the absence of fermions the charged W fields are the source of the electromagnetic current for generating the seed fields. Solutions of the equations of motion for the charged gauge fields and Maxwell's equations for the magnetic field in O(1,2) space-time symmetry are expressed in closed form by applying boundary conditions at the time of collision. Our results indicate that the magnetic fields generated by charged $W^{\pm}$ fields in the collision are comparable to those found in previous work. The magnetic fields so produced could seed galactic and extra-galactic magnetic fields observed today.

astro-ph

Electromagnetic Field Creation During EWPT Nucleation With Lepton Currents

We include the electromagnetic currents from fermion degrees of freedom in the equations of motion for electroweak MSSM with a right-handed Stop that we have recently investigated. It is found that near the surface of the bubble walls there are important effects on the electromagnetic fields produced during bubble nucleation.

hep-ph