Towards a unified definition of solar limb during central eclipses and daily transits

The diameter of the Sun has been measured using Baily's beads during central eclipses, observed with portable telescopes. A blend of tiny emission lines produced in the first several hundred kilometers above the photosphere gives a light signal which prolonges the light curves of the beads. The simple criterion of light OFF/ON adopted in the previous approaches to define the timing of photosphere's disappearance/reappearance is modified. The technique of the limb darkening function reconstruction from the Baily's beads light curves is introduced here.Comment: 9 pages, 6 figures, Proc. of the 2nd Galileo-Xu Guangqi Meeting, Ventimiglia - Villa Hanbury, Italy, 11-16 July 201

Theoretical Problems in High Resolution Solar Physics, 2

The Science Working Group for the High Resolution Solar Observatory (HRSO) laid plans beginning in 1984 for a series of workshops designed to stimulate a broadbased input from the scientific community to the HRSO mission. These workshops have the dual objectives of encouraging an early start on the difficult theoretical problems in radiative transfer, magnetohydrodynamics, and plasma physics that will be posed by the HRSO data, and maintaining current discussions of results in high resolution solar studies. This workshop was the second in the series. The workshop format presented invited review papers during the formal sessions and contributed poster papers for discussions during open periods. Both are presented

A role for community health workers in pediatric ADHD treatment through the delivery of behavioral parent training

INTRODUCTION: Community health workers are a growing and developing portion of the healthcare workforce. They have proven successes in decreasing healthcare inequities for many common chronic medical conditions, such as asthma, and have secured support at the Department of Health and Human Services. One common medical condition for which community health workers have not yet been explored as a resource is pediatric Attention Deficit Hyperactivity Disorder. We sought to investigate what the literature showed on community health workers' involvement in ADHD treatments thus far, and to specifically investigate which ADHD behavioral parent training program could best be adapted to a pilot study where community health workers were the intervention delivery agents. METHODS: We performed a systematic review of the literature on evidence based behavioral parent training programs for children with ADHD. Parent training interventions were compared for ease of application to a community health worker home-visit model. Program ability to successfully reduce child behavior problems and improve parenting practices was analyzed. RESULTS: 8 full text articles were analyzed in depth and grouped by intervention type. 1 article was a sports-based intervention for fathers, 1 was meant to improve attendance rates, 1 was a combined child-targeted and parent-targeted Behavioral Parent Training (BPT) therapy, 2 were based on the "New Forest Parenting Package", and 3 were based on Barkley's 1997 manualized BPT. DISCUSSION: Evidence exists for the ability of community health workers to deliver a behavioral therapy to families of children with ADHD, specifically behavioral parent training. Barkley's manualized BPT had the best combination in our study of positive outcomes for families and ease of adaptability to in-home delivery. We recommend a pilot study be conducted using a modified version of Barkley's BPT and have community health workers as the delivery agents to begin to see what role community health workers can play in the treatment of pediatric ADHD

Investigation of mass flows in the transition region and corona in a three-dimensional numerical model approach

The origin of solar transition region redshifts is not completely understood. Current research is addressing this issue by investigating three-dimensional magneto-hydrodynamic models that extend from the photosphere to the corona. By studying the average properties of emission line profiles synthesized from the simulation runs and comparing them to observations with present-day instrumentation, we investigate the origin of mass flows in the solar transition region and corona. Doppler shifts were determined from the emission line profiles of various extreme-ultraviolet emission lines formed in the range of $T=10^4-10^6$ K. Plasma velocities and mass flows were investigated for their contribution to the observed Doppler shifts in the model. In particular, the temporal evolution of plasma flows along the magnetic field lines was analyzed. Comparing observed vs. modeled Doppler shifts shows a good correlation in the temperature range $\log(T$/[K])=4.5-5.7, which is the basis of our search for the origin of the line shifts. The vertical velocity obtained when weighting the velocity by the density squared is shown to be almost identical to the corresponding Doppler shift. Therefore, a direct comparison between Doppler shifts and the model parameters is allowed. A simple interpretation of Doppler shifts in terms of mass flux leads to overestimating the mass flux. Upflows in the model appear in the form of cool pockets of gas that heat up slowly as they rise. Their low temperature means that these pockets are not observed as blueshifts in the transition region and coronal lines. For a set of magnetic field lines, two different flow phases could be identified. The coronal part of the field line is intermittently connected to subjacent layers of either strong or weak heating, leading either to mass flows into the loop or to the draining of the loop.Comment: 7 pages, 7 figure

High-Frequency Oscillations in a Solar Active Region observed with the Rapid Dual Imager

High-cadence, synchronized, multiwavelength optical observations of a solar active region (NOAA 10794) are presented. The data were obtained with the Dunn Solar Telescope at the National Solar Observatory/Sacramento Peak using a newly developed camera system : the Rapid Dual Imager. Wavelet analysis is undertaken to search for intensity related oscillatory signatures, and periodicities ranging from 20 to 370 s are found with significance levels exceeding 95%. Observations in the H-alpha blue wing show more penumbral oscillatory phenomena when compared to simultaneous G-band observations. The H-alpha oscillations are interpreted as the signatures of plasma motions with a mean velocity of 20 km/s. The strong oscillatory power over H-alpha blue-wing and G-band penumbral bright grains is an indication of the Evershed flow with frequencies higher than previously reported.Comment: 9 pages, 9 figure

A preferred vision for administering elementary schools : a reflective essay

I believe in being a proactive administrator. I do not want to be recognized simply as the authority figure in the school that is rarely seen. My door will always be open, and I will be seen in the classrooms as well as throughout the school. I want to be active in the teaching process. My first year as a principal will be a time for me to become familiar with the school environment. I will not make any major changes the first year unless I am forced to do so. I believe that this time should be spent becoming competent in performing administrative duties and evaluating existing procedures, structures and goals. Also, it will be a time to develop relationships with staff, students, and parents so that I may gain their trust and confidence. This is important so that the staff and parents will be more open to change in the future

A Comparative Analysis of School Reorganization of Bear Lake County Idaho

Education, always important, is today more essential than ever if we are to perpetuate and improve our democratic way of life . The recognition of the importance of education in our society has resulted in planning at the national , state and local levels

A Statistical Analysis of the SOT-Hinode Observations of Solar Spicules and their Wave-like Behavior

We consider a first important parameter of spicules as observed above the solar visible limb: their apparent diameter as a function of the height above the limb which determines their aspect ratio and leads to the discussion of their magnetic origin using the flux tube approximation. We found that indeed spicules show a whole range of diameters, including unresolved "interacting spicules" (I-S), depending of the definition chosen to characterize this ubiquitous dynamical phenomenon occurring into a low coronal surrounding. 1-D Fourier amplitude spectra (AS) made at different heights above the limb are shown for the first time. A definite signature in the 0.18 to 0.25 Mm range exists, corresponding to the occurrence of the newly discovered type II spicules and, even more impressively, large Fourier amplitudes are observed in the 0.3 to the 1.2 Mm range of diameters and spacing, in rough agreement with what historical works were reporting. Additionally, some statistically significant behavior, based on AS computed for different heights above the limb, is discussed. "Time slice or x-t diagrams" revealing the dynamical behavior of spicules are also analyzed. They show that most of spicules have multiple structures (similarly to the doublet spicules) and they show impressive transverse periodic fluctuations which were interpreted as upward kink or Alfven waves. Evidence of the helical motion in spicules is now well evidenced, the typical periods of the apparent oscillation being around 120 sec. A fine analysis of the time-slice diagram as a function of the effective heights shows an interesting new feature near the 2 Mm height. We speculate on the interpretation of this feature as being a result of the dynamical specificities of the spicule helical motion as seen in these unprecedented high resolution HCaII line emission time series.Comment: 21 pages, 8 figurs, 1 tabl

The quiet Sun average Doppler shift of coronal lines up to 2 MK

The average Doppler shift shown by spectral lines formed from the chromosphere to the corona reveals important information on the mass and energy balance of the solar atmosphere, providing an important observational constraint to any models of the solar corona. Previous spectroscopic observations of vacuum ultra-violet (VUV) lines have revealed a persistent average wavelength shift of lines formed at temperatures up to 1 MK. At higher temperatures, the behaviour is still essentially unknown. Here we analyse combined SUMER/SoHO and EIS/Hinode observations of the quiet Sun around disk centre to determine, for the first time, the average Doppler shift of several spectral lines formed between 1 and 2 MK, where the largest part of the quiet coronal emission is formed. The measurements are based on a novel technique applied to EIS spectra to measure the difference in Doppler shift between lines formed at different temperatures. Simultaneous wavelength-calibrated SUMER spectra allow establishing the absolute value at the reference temperature of 1 MK. The average line shifts at 1 MK < T < 1.8 MK are modestly, but clearly bluer than those observed at 1 MK. By accepting an average blue shift of about (-1.8+/-0.6) km/s at 1 MK (as provided by SUMER measurements), this translates into a maximum Doppler shift of (-4.4+/-2.2) km/s around 1.8 MK. The measured value appears to decrease to about (-1.3+/-2.6) km/s at the Fe XV formation temperature of 2.1 MK. The measured average Doppler shift between 0.01 and 2.1 MK, for which we provide a parametrisation, appears to be qualitatively and roughly quantitatively consistent with what foreseen by 3-D coronal models where heating is produced by dissipation of currents induced by photospheric motions and by reconnection with emerging magnetic flux.Comment: 9 pages, 10 figures. Astronomy and Astrophysics (in press

Measurement Properties of the Motivation for Youth Treatment Scale with a Residential Group Home Population

A client’s motivation to receive services has long been identified as a highly relevant component of mental health treatment. In fact, ample evidence demonstrates that client motivation is significantly related to seeking services, remaining in services, and improved client outcomes (e.g., Broome, Joe, & Simpson, 2001; Ryan, Plant, & O’Malley, 1995; Schroder, Sellman, Frampton, & Deering, 2009). Additionally, it has been recognized that motivation is a “dynamic” characteristic that changes throughout treatment (Melnick, De Leon, Hawke, Jainchill, & Kressel, 1997; Schroder et al., 2009). In this way, motivation is an important client factor to assess and monitor throughout the treatment process. The broad construct of motivation is comprised of two separate, but related components conceptualized as motivation to change and motivation for treatment. As defined by DiClamente, Schlundt, and Gemmell (2004), motivation to change refers to a willingness to recognize problematic behavior and take steps toward change, whereas motivation for treatment refers to a willingness to seek help and remain compliant with an intervention program. In other words, a motivated person not only perceives the importance of changing, but also has confidence that they are able to be successful at making the change (Burke, Arkowitz, & Menchola, 2003)