Conscientious objectors during Britain's last popular war

Due to the character of the original source materials and the nature of batch digitization, quality control issues may be present in this document. Please report any quality issues you encounter to [email protected], referencing the URI of the item.Includes bibliographical references (leaves 22).This paper contains the results of my research on the conscientious objectors of World War II in Great Britain. After a brief overview of the events of the 1920's and 1930's which led to the formation of pacifist sentiments in Britain, I discuss my findings regarding who the conscientious objectors were, what the differences were between the objectors in the second world war and the first world war, and how the objectors in the second war were treated by their government and society. I also present information regarding the various experiences of the objectors during the war and the legal aspects of conscientious objection

A Teachable Unit on Soft Corals with Instructional Method Variances

The soft coral Sinularia flexibilis contains an aqueous alcohol extract that has shown antineoplastic activity against lymphocytic leukemia (Weinheimer and Matson, 1977). It also has other biological properties that work as antimicrobials, anti-inflammatory agents, and cytotoxicity activities (Kamel and Slattery, 2005). There is much research on the effects of flow rate on growth and morphology (Khalesi, Beeftink, & Wijffels, 2007) and the effects of light-dependency on growth rate (Khalesi, Beeftink, & Wijffels, 2009). The purpose of this student project was to further research on S. flexibilis, as well as incorporate that research into evaluating the effects of lecture-based teaching methods versus 5E-based teaching methods. The results showed nearly a two-point difference in the averages of the quizzes given in the two lectures, with the lecture-based lecture having the higher average. The qualitative feedback from the students attending both lessons also showed a significant preference for the lecture over the 5E lesson

A two-component transport model for solar wind fluctuations: Waves plus quasi-2D turbulence

We present a model for the transport of solar wind fluctuations, based on the assumption that they can be well-represented using two distinct components: a quasi-2D turbulence piece and a wave-like piece. For each component, coupled transport equations for its energy, cross helicity, and characteristic lengthscale(s) are derived, along with an equation for the proton temperature. This energy-containing “two-component” model includes the effects of solar wind expansion and advection, driving by stream shear and pickup ions, and nonlinear cascades. Nonlinear effects are modeled using a recently developed one-point phenomenology for such a two-component model of homogeneous MHD turbulence [1]. Heating due to these nonlinear effects is included in the temperature equation. Numerical solutions are discussed and compared with observation

Empirical Constraints on Proton and Electron Heating in the Fast Solar Wind

We analyze measured proton and electron temperatures in the high-speed solar wind in order to calculate the separate rates of heat deposition for protons and electrons. When comparing with other regions of the heliosphere, the fast solar wind has the lowest density and the least frequent Coulomb collisions. This makes the fast wind an optimal testing ground for studies of collisionless kinetic processes associated with the dissipation of plasma turbulence. Data from the Helios and Ulysses plasma instruments were collected to determine mean radial trends in the temperatures and the electron heat conduction flux between 0.29 and 5.4 AU. The derived heating rates apply specifically for these mean plasma properties and not for the full range of measured values around the mean. We found that the protons receive about 60% of the total plasma heating in the inner heliosphere, and that this fraction increases to approximately 80% by the orbit of Jupiter. A major factor affecting the uncertainty in this fraction is the uncertainty in the measured radial gradient of the electron heat conduction flux. The empirically derived partitioning of heat between protons and electrons is in rough agreement with theoretical predictions from a model of linear Vlasov wave damping. For a modeled power spectrum consisting only of Alfvenic fluctuations, the best agreement was found for a distribution of wavenumber vectors that evolves toward isotropy as distance increases.Comment: 11 pages (emulateapj style), 5 figures, ApJ, in pres

Transport of cross helicity and radial evolution of alfvenicity in the solar wind

A transport theory including cross helicity, magnetohydrodynamic(MHD) turbulence, and driving by shear and pickup ions, is applied to the radial evolution of the solar wind. The radial decrease of cross helicity observed in the solar wind can be accounted for when sufficient driving is included to overcome the inherent tendency for MHD turbulence to produce Alfvenic states

Radial evolution of cross helicity at low and high latitudes in the solar wind

We employ a turbulence transport theory to the radial evolution of the solar wind at both low and high latitudes. The theory includes cross helicity, magnetohydrodynamic (MHD) turbulence, and driving by shear and pickup ions. The radial decrease of cross helicity, observed in both low and high latitudes, can be accounted for by including sufficient shear driving to overcome the tendency of MHD turbulence to produce Alfvénic states. The shear driving is weaker at high latitudes leading to a slower evolution. Model results are compared with observations from Ulysses and Voyager

Electron and proton heating by solar wind turbulence

Previous formulations of heating and transport associated with strong magnetohydrodynamic (MHD) turbulence are generalized to incorporate separate internal energy equations for electrons and protons. Electron heat conduction is included. Energy is supplied by turbulent heating that affects both electrons and protons, and is exchanged between them via collisions. Comparison to available Ulysses data shows that a reasonable accounting for the data is provided when (i) the energy exchange timescale is very long and (ii) the deposition of heat due to turbulence is divided, with 60% going to proton heating and 40% into electron heating. Heat conduction, determined here by an empirical fit, plays a major role in describing the electron data

Radial evolution of cross helicity in high-latitude solar wind

We employ a turbulence transport theory to explain the high-latitude radial evolution of cross helicity, or Alfvénicity, observed by the Ulysses spacecraft. Evolution is slower than at low latitudes due to weakened shear driving