D. Maia

The authors present the preliminary results of a correlational study among the scales of Luria Nebraska Neuropsychological Battery (LNNB), the Mini Mental State Examination (MMSE) and clinical variables (disease onset and duration, type of crisis). The aim of this study is assessing the existence of a relationship between neuropsychological variables and clinical variables. 12 female patients with both nonepileptic and epileptic seizures with a mean age of 39,6 years (€12,3), followed at Psychiatric and Neurophysiology Services, were recruited. It were used the following instruments: socio demographic and a clinical interview, the LNNB and the MMSE. The results indicate that the emergence of nonepileptic seizures occurs on average 9 years after the onset of the epileptic disease; the duration of epilepsy is the clinical variable most correlated with the clinical scales of LNNB. The highest value (worst performance) was found on the scale that assesses the Intellectual Functions (30,...

A modeling framework for the prediction of the Martian radiation environment is presented. Features include input solar cycle modulated cosmic ray and solar particle event spectra, based both on CREME-96, the transport of this radiation in the Martian atmosphere and regolith, including creation of secondaries, using the Geant4 Monte Carlo toolkit. Details of the atmosphere are derived from the European

ABSTRACT In order to establish an individual plan of care for the patient for promote their psychosocial rehabilitation, was conducted a multidisciplinary assessment protocol. This protocol aims to characterize the patients admitted in DH, through the analysis of sociodemographic and clinical data at moment of clinical admission and discharge of the unit. Another objective is to assess the degree of satisfaction with the services provided, and also quality of life (QOL) (The Short Form Health Survey SF-36), psychopathological state (Brief Symptom Inventory - BSI) and functionality (Occupational Self Assessment - OSA).In a sample of 168 individuals, (assessment between January 2009 and June 2011) 48% were male (n=80). The average age of participants was 44.4 (SD=11.9), the average age of onset of 29.7 (SD=13.3). The most frequent diagnoses were the Group of Schizophrenia, Schizotypal and Delusional Disorders at 38.7%, followed by mood disorders with 30.4%.In regard to QOL, it was found out that patients scored significantly higher on some dimensions on discharge, corresponding to a better QOL. The BSI dimensions on exit are generally lower than the results of the entrance, which means that patients have less psychopathological symptoms. The results of OSA indicate that aspects of functionality, chosen by their patients for psychosocial rehabilitation are: self care and problem-solving ability.

Some results of the uvbybeta photometry of 237 F--G stars located in two fields situated near the South Galactic Pole, are presented here. These observations were carried out with the 0.5m Danish Telescope at ESO. We can conclude the following: 1) Stars with a large asymmetric drift show: a) No substantially different age distribution when compared to the thin disk. Thick disk candidates show an age range from 6--7 to 12--14 Gyr and a velocity dispersion of sigma_ {{W}}}=38 +/- 10 \km; b) However, some stars have solar-like metallicity. 2) The age distributions for thin disk candidates in different [Fe/H] bins are not identical, nevertheless, no well defined age--metallicity relation can be established.

The spatial distribution of stars towards the south galactic pole (SGP) has been studied using the sample by Rose & Agostinho (1991) in two fields covering about 55°, which is complete down to B = 12.5. Through the use of digitised objective prism spectra, their data yielded information on each star's magnitude, spectral type, luminosity class, an estimate of [Fe/H], radial velocity and proper motions. Maximum likelihood computations showed that the disk-like component(s) in the galactic z direction is best described by a two-exponential model with scale heights of 145±10 pc and 287±13 pc. The relative normalisations of these two components vary from nearly zero at F5 to about 3.6 for G0 - G3 stars. From uvbyß photometry of 250 late-F to early-G dwarf stars the authors conclude that the intermediate population (iP II) group shows a chemical distribution compatible with that of the thick disk, and its age shows a large variation with limits of 6 and 14 Gyr. There is a shift towar...

The analysis of the November 6, 1997 event has taken advantage of the new capabilities of the OPorto Radiospectrograph and of the Nanccay Radioheliograph. The evolution of this event shows successive phases in time scales of a fraction of a second. It is shown that the CME observed by the LASCO/SOHO coronograph is the result of successive interactions of multiple

The spatial distribution of stars towards the south galactic pole (SGP) has been studied using the sample by Rose & Agostinho (1991) in two fields covering about 55°, which is complete down to B = 12.5. Through the use of digitised objective prism spectra, their data yielded information on each star's magnitude, spectral type, luminosity class, an estimate of [Fe/H], radial velocity and proper motions. Maximum likelihood computations showed that the disk-like component(s) in the galactic z direction is best described by a two-exponential model with scale heights of 145±10 pc and 287±13 pc. The relative normalisations of these two components vary from nearly zero at F5 to about 3.6 for G0 - G3 stars. From uvbyß photometry of 250 late-F to early-G dwarf stars the authors conclude that the intermediate population (iP II) group shows a chemical distribution compatible with that of the thick disk, and its age shows a large variation with limits of 6 and 14 Gyr. There is a shift towa...

We investigate the solar origin and propagation of a series of well-collimated energetic electron events on 1997 November 28, measured in situ by the Electron, Proton, and Alpha Monitor (EPAM) experiment on the Advanced Composition Explorer (ACE) spacecraft. EPAM measures electrons in the energy range from 40 to 300 keV over a wide range of look directions and with better than 1 minute time resolution. During the events in our study, the particles are strongly collimated along the magnetic field. As such, these near-relativistic (beta=0.4-0.7) particles tend to be scatter free; their observed arrival at ACE provides a good estimate of the release time back to the Sun. EPAM results are extended to 20 keV using energetic electron data from the Three-Dimensional Plasma Analyzer (3DP) experiment on the Wind spacecraft. We combine these observations with fast imaging of the solar corona in the meter wave domain, provided by the Nançay radioheliograph, and dynamic spectral information from the WAVES experiment on the Wind spacecraft. Together, this complement of observations of solar energetic particle events provides insight into the onset times and sites of particle acceleration in the low corona. The imaging observations at metric radio frequencies show three series of similar events off the west limb of the Sun that extend into interplanetary type III bursts. The third event corresponds only to a strong in situ particle event. During this time period, the coronagraphic observations from the Large Angle and Spectrometric Coronagraph experiment on the Solar and Heliospheric Observatory reveal a dimming and some morphological changes in the vicinity of the injection site, suggesting the opening of the magnetic field. We find that for the strongest event, the onset times for the energetic particles measured at the spacecraft reveal a dispersion in the inferred release times back at the Sun versus energy. The onset times measured for electrons with energies above 60 keV are not compatible with the release time back at the Sun inferred from particles of lower energies. This dispersion can be successfully explained by the radio data: the radio observations reveal two successive energetic electron injections separated by a few minutes. The observations thus show that there is a later release of the particles detected in situ at higher energies and that the origin of the phenomenon is in the low corona.

The Oporto radiospectrograph and the Nançay radioheliograph recorded a radio event on November 6, 1997, closely related in time with a flare on National Oceanic and Atmospheric Administration (NOAA) active region 8100. At the beginning of the event the radio sources are located on a rather small volume in the vicinity of the flare site. In a timescale of only

ABSTRACT We present our research on a fast and decelerating partial halo coronal mass ejection (CME) event detected in multi-wavelengths in the chromosphere and the corona on 14 October, 1999. The event involved a whole complex active area which spanned more than 40° of heliolongitude. It included a strong solar flare (XI/1N) and a complex eruptive filament within an active region of the entire complex. Especially, several radio sources were detected in the decimetric range prior to the CME by the Nançay Radioheliograph (NRH). A linear force-free field extrapolation of the Michelson Doppler Imager (MDI) magnetogram was performed to calculate the magnetic topology of the complex prior to the triggering of the event. The presence of a coronal null point combined with the occurrence of two distant and nearly simultaneous radio sources put strong arguments in favor of the generalized breakout model for the triggering of the eruption. The analysis of the subsequent development of the event suggests that large interconnecting loops were ejected together with the CME.

We present in this study a synthesis of results on the initiation and development of CMEs using coordinated observations from SOHO and ground-based instruments. The emphasis is placed on radio spectral and imaging data. One important goal of this study is the identification of radio signatures of CMEs providing information below one solar radius above the limb. CMEs can be