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The purpose of this manual is to provide vocational educators with evaluation elements and tested models which can assist them in designing evaluation systems. Chapter 1 provides several sets of criteria for inclusion in any general program evaluation. The eleven general areas for which criteria are included are administrative procedures, curriculum design, staff development, articulation and coordination, liaison activities, student-related activities, recruitment and advising, placement and followup, expanded opportunities, facilities and equipment, and evaluation. Chapter 2 discusses some specific educational concepts and techniques which have implications for vocational evaluation, including achievement variables and taxonomies. Chapter 3 addresses the concept of evaluation models. These six models are presented and discussed: Accreditation, Tylerian, CIPP (context, input, process, and product., CSE (Center of the Study of Evalution), Formative and Summative, and Single Subject Design. Chapter 4 focuses on procedures to design a comprehensive evaluation system which includes data collection. Sample charts, tables, grids, and reporting forms are presented. Appendixes provide selected sample instrument formats representing the following categories of program evaluations: student assessment, teacher assessment follow-up, employee surveys, and the general category of evaluation. (YLB)

The main objective of the study is to test a motivational enhancement (ME) intervention to address barriers to engaging in mental health treatment for recently returned veterans of Operation Iraqi Freedom and Operation Enduring Freedom. The long term goal of the study is to increase veteran s participation in mental health treatment by using a Stages of Change model to reduce perceived stigma and barriers to treatment. The central hypothesis put forth is that veterans who receive motivational enhancement will demonstrate greater readiness to change and higher treatment program attendance than veterans who receive treatment as usual. During this year the pilot study for the project was completed. The purpose of the pilot study group was to inform us of any changes and/or enhance user ability of the project manuals. However, due to the lapse in coverage the data collected from the pilot group members could not be used. The veterans in the pilot study were notified of the lapse and were re-consented. During the year the team has continued to brainstorm resources and methods to recruit OIF/OEF veterans for the study. It is a logistical matter that continues to be challenging. More efforts are being made to reach agencies that may encounter OIF/OEF veterans that qualify for the study. Hiring of the veterans to help with recruitment was somewhat helpful in that we received additional inquires about the project, however, only a small number met the criteria for eligibility., The original document contains color images.

Established contract between Wayne State University (WSU) and the Detroit-Wayne County CMH Agency (Agency) to collaborate on implementation of the randomized controlled trial of the intervention as well as adapting the Motivational Enhancement intervention for use in a group modality. The contract with Southwest Counselling Solutions (SWCS) was also finalized which will now allow us to move forward with setting up training seminars for the clinical staff who will be responsible for provision of clinical services to participants in a manner that ensures model fidelity. WSU s IRB has approved the protocol for the study and has agreed to IRB of Record for both the Agency and SWCS. We are also in receipt of the approved FWAs. Efforts are continuing relative to FMU IRB reviewing the protocol for approval. The unplanned retirement of the original Principal Investigator (PI), Elaine Thomas, necessitated the assignment of new PI and request to USAMRMC for a modification/amendment to change the PI on the subject award

Recent advances in space-based heliospheric observations, laboratory experimentation, and plasma simulation codes are creating an exciting new cross-disciplinary opportunity for understanding fast energy release and transport mechanisms in heliophysics and laboratory plasma dynamics, which had not been previously accessible. This article provides an overview of some new observational, experimental, and computational assets, and discusses current and near-term activities towards exploitation of synergies involving those assets. This overview does not claim to be comprehensive, but instead covers mainly activities closely associated with the authors’ interests and reearch. Heliospheric observations reviewed include the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) on the National Aeronautics and Space Administration (NASA) Solar Terrestrial Relations Observatory (STEREO) mission, the first instrument to provide remote sensing imagery observations with spatial continuity extending from the Sun to the Earth, and the Extreme-ultraviolet Imaging Spectrometer (EIS) on the Japanese Hinode spacecraft that is measuring spectroscopically physical parameters of the solar atmosphere towards obtaining plasma temperatures, densities, and mass motions. The Solar Dynamics Observatory (SDO) and the upcoming Solar Orbiter with the Heliospheric Imager (SoloHI) on-board will also be discussed. Laboratory plasma experiments surveyed include the line-tied magnetic reconnection experiments at University of Wisconsin (relevant to coronal heating magnetic flux tube observations and simulations), and a dynamo facility under construction there; the Space Plasma Simulation Chamber at the Naval Research Laboratory that currently produces plasmas scalable to ionospheric and magnetospheric conditions and in the future also will be suited to study the physics of the solar corona; the Versatile Toroidal Facility at the Massachusetts Institute of Technology that provides direct, United States. Office of Naval Research, Naval Research Laboratory (U.S.)

Spacecraft observations in the inner heliosphere offer the first opportunity to measure 1-10 MeV solar neutrons. We discuss the physics of low-energy neutron production in solar flares and show that, even at interacting-particle energies of 2 MeV nucleon(-1), neutrons with energies >10 MeV are produced. On the other hand, a significant fraction of 1-10 MeV neutrons result from interactions of >10 MeV nucleon(-1) ions in typical flare spectra. We calculate the escaping neutron spectra for mono-energetic and power-law particle spectra at the Sun for the location and observation angle of MESSENGER at the time of its reported detection of low-energy neutrons associated with the 2007 December 31 solar flare. We detail concerns about this questionable observation of solar neutrons: 1. the inferred number of accelerated protons at the Sun for this modest M2-class flare was 10X larger than any flare observed to date, 2. the onset and duration of the 'solar' neutron count rate was similar to that of the solar energetic particles (SEPs), and 3. the authors' argument that the SEPs were dominated by electrons and so could not have produced the neutron counts locally in the spacecraft. In contrast we argue that solar energetic protons and particles, through local neutron production and accidental coincidences, were the source of most of the reported 'solar-neutron' counts., In press, Journal of Geophysical Research.

We detail observations of gamma rays produced by interactions of cosmic rays and solar-energetic particles on the Earth's atmosphere. The Solar Maximum Mission (SMM) spectrometer accumulated the quiescent atmospheric spectrum over its full 9-year lifetime and our analysis revealed 20 resolved line features. We compare this spectrum with one collected on October 20, 1989, when SMM observed gamma rays produced by shock-accelerated protons that impacted the atmosphere in the polar region following an intense solar flare and coronal mass ejection. Observed nuclear-line intensities increased by over a factor of 50 during this event. Because this event was on the horizon and subtended a limited solid angle as viewed from SMM, the local increase was several times higher. We compare the gamma ray line energies, widths, and intensities from the solar event and quiescent atmospheric spectra and discuss their identifications. From this comparison we confirm direct observations that the solar proton spectrum is considerably softer than the spectrum of cosmic rays. Extension of an existing code for calculating solar gamma ray lines will provide information on the spectra of the protons reaching the Earth's atmosphere and thus on their transport through the magnetosphere. Broad spectral features found in the spectra are likely to be caused by a multitude of unresolved lines excited by neutron capture in the instrument, spacecraft, and Earth's atmosphere., Published in JGR, v106 (Space Physics) nA1 p77-92, 2001. Sponsored in part by NASA.

We discuss how remote observations of gamma-ray lines and continua provide information on the population of electrons and ions that are accelerated in solar flares. The radi ation from these interactions also provides information on the composition of the flaring chromosphere. We focus our di scussion on recent RHESSI observations and archival observations made by SMM and Yohkoh.

We discuss how gamma-ray spectroscopy provides information about the acceleration and transport of electrons and ions in solar flares, and their interaction with the solar atmosphere. Temporal studies illuminate differences in the acceleration and transport of electrons and ions. Nuclear line studies reveal the elemental abundance, density, and temperature of the ambient solar atmosphere; and the spectrum, composition and directionality of the accelerated ions., Published in the ASP Conference Series, v219 p133-144, 2004. Sponsored in part by NASA.

RHESSI has measured the positron-electron annihilation line and continuum in three solar flares: 2002 July 23, 2003 October 28, and 2003 November 2. The 511 keV line was broad (4-8 keV) in all three flares, consistent with annihilations in an ambient ionized medium at temperatures above 10(expn 5) K. The measured continuum from positronium and from Compton scattering was unobservable, with the exception of the first 4 minutes of the October 28 flare observation; this indicates that the density at which most annihilations occurred was greater than 10(expn 14) H cm(expn -3). The width of the line narrowed in 2 minutes to 1 keV late in the October 28 flare, consistent with annihilation in ionized H 10(expn 4) K and /= 10(expn 15) cm(expn -3). There is evidence for a similar decrease in line width late in the November 2 flare. These observations suggest a highly dynamic flaring atmosphere at chromospheric densities that can reach transition-region temperatures, then cool to less than 10(expn 4) K in minutes while remaining highly ionized. Although the energy contained in high-energy accelerated particles may have been enough to heat the plasma, the rate of deposition is not correlated with the temperature determined by the 511 keV line width, and this raises questions about the energy source., Published in the Astrophysical Journal, v615 pL169-L172, 10 Nov 2004. Prepared in collaboration with NASA Goddard Space Flight Center, Greenbelt, MD. Prepared in coopearion with the Department of Physics, and SCIPP, University of California, Santa Cruz, and the Space Sciences Laboratory and Department of Physics, University of California, Berkeley. Sponsored in part by NASA.

RHESSI has observed the 7Be and 7Li -ray lines from fusion of accelerated alpha particles with ambient helium produced during the 2002 July 23 solar are that erupted at a heliocentric angle of 73 deg. This is the first observation of the lines with a germanium spectrometer. We have fit the measured lines with calculated shapes for different energy and angular distributions for the interacting alpha particles. A particle distribution from saturated pitch-angle scattering in the corona provides the best fit, but isotropic, downward-isotropic, or fan-beam distributions also provide acceptable fits. We can rule out a downward-beamed distribution with 99.99% confidence. RHESSI measurements of other Doppler-shifted nuclear de--excitation lines are consistent with a forward isotropic distribution of interacting particles in a magnetic loop tilted by 40 deg from the normal to the solar surface toward Earth. Such a distribution is also consistent with the alpha-4He line shape with 15% confidence., Published in Ap. J. Letters, v595, 2003. Prepared in collaboration with the E.O. Hulburt Center for Space Research, Naval Research Laboratory, Washington, DC, and the Space Sciences Laboratory and Dept. of Physics, University of California, Berkeley, CA.

We report high spectral-resolution measurements of the 2.223 MeV neutron capture-line obtained with the Reuven Ramaty High Energy Spectroscopic Imager from the 2002 July 23 solar are. The time history of this line is affected by both the photospheric the abundance and the angular distribution of the interacting are-accelerated particles producing the neutrons. The measured time history is compared with predicted time histories calculated using a magnetic loop model with a magnetic eld perpendicular to the solar surface at the footpoints. The model includes energy losses due to Coulomb collisions, removal by nuclear reactions magnetic mirroring in the convergent ux tube, and MHD pitch-angle scattering in the corona. This is the first analysis of the neutron-capture line using such a physically-based model. The derived constraints on the interacting angular distribution require that the accelerated particles had to su er pitchangle scattering during their transport through the coronal portion of the loop. The derived photospheric 3He/H ratio was not well-constrained, primarily due to uncertainties associated with the measured nuclear deexcitation-line ux used to represent the neutron-production time pro le., Published in Ap .J. Letters, 595, L93 (2003).

The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) has observed the positron-electron annihilation line at 511 keV produced during the 2002 July 23 solar flare. The shape of the line is consistent with annihilation in two vastly different solar environments. It can be produced by formation of positronium by charge exchange in flight with hydrogen in a quiet solar atmosphere at a temperature of 6000 K. However, the measured upper limit to the 3g/2g ratio (ratio of annihilation photons in the positronium continuum to the number in the line) is only marginally consistent with what is calculated for this environment. The annihilation line can also be fitted by a thermal Gaussian having a width of 8.1 +/- 1.1 keV (FWHM), indicating temperatures of (4 7) x 10(expn 5) K. The measured 3g/2g ratio does not constrain the density when the annihilation takes place in such an ionized medium, although the density must be high enough to slow down the positrons. This would require the formation of a substantial mass of atmosphere at transition-region temperatures during the flare., Published in the Astrophysical Journal, v595 pL85-L88, 1 Oct 2003. Additional NASA grant DPR-W10049. Prepared in collaboration with the NASA Goddard Space Flight Center, Greenbelt, MD. Prepared in cooperation with the Space Sciences Laboratory and Department of Physics, University of California at Berkeley, and the School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel.