Observations of flux rope ? associated particle bursts with GEOTAIL in the distant tail

International audienceGeotail energetic particle, magnetic field data and plasma observations (EPIC, MGF and CPI experiments) have been examined for a number of energetic particle bursts in the distant tail (120ReGSM|By and/or Bz components, is consistent with the existence of closed field lines extending from Earth and wrapping around the core of the flux rope structure

Dzyaloshinskii--Moriya interaction: How to measure its sign in weak ferromagnetics?

Three experimental techniques sensitive to the sign of the Dzyaloshinskii--Moriya interaction are discussed: neutron diffraction, Moessbauer gamma-ray diffraction, and resonant x-ray scattering. Classical examples of hematite (alpha-Fe2O3) and MnCO3 crystals are considered in detailComment: 5 pages, 1 figure; to be published in JETP Letter

Identification of R gene genotypes in Japanese wheat cultivars

Dissertação de mestrado em Psicologia Clínica e da Saúde (Psicopatologia e Psicoterapias Dinâmicas), apresentada à Faculdade de Psicologia e de Ciências da Educação da Universidade de CoimbraA presente investigação visa explorar múltiplas variáveis (sociodemográficas, clínicas e satisfação com o suporte social) na relação com o bonding materno. O nosso principal objetivo foi perceber quais as diferenças entre as mães adultas e as mães adolescentes relativamente à forma como se vinculam (bonding) ao seu bebé, para isso procedemos às entrevistas de 57 mães, em que 29 são mães adultas e 28 são mães adolescentes. Consoante os nossos resultados, pudemos inferir que as mães adolescentes apresentam valores de bonding inferiores aos valores das mães adultas. Quando comparamos o bonding com o suporte social também verificamos que as mães adolescentes apresentam valores de perceção do suporte social inferiores aos valores das mães adultas. Deste modo, a relação mãe-bebé vai sendo fortalecida consoante aumenta a idade das mães e a perceção que as mesmas têm em relação ao suporte social.The present investigation pretends to explore multiple variables (sociodemographic, clinic, and satisfaction with social support) and its relation to maternal bonding. Our main goal was to understand which are the differences between adult mothers and teenage mothers as how they are bond to their baby. We interviewed 57 mothers, in which 29 are adult mothers and 28 are adolescent mothers. From our results, we infer that teenage mothers have lower values than adult mothers on bonding. When we compare bonding with social support we also found that teenage mothers have lower values of social support perception relatively to adult mothers. We also conclude that mother-baby relationship and social support perception will be strengthened as mothers grow older

Precision Fe Kalpha and Fe Kbeta Line Spectroscopy of the Seyfert 1.9 Galaxy NGC 2992 with Suzaku

We present detailed time-averaged X-ray spectroscopy in the 0.5--10 keV band of the Seyfert~1.9 galaxy NGC 2992 with the Suzaku X-ray Imaging Spectrometers (XIS). We model the complex continuum in detail. There is an Fe K line emission complex that we model with broad and narrow lines and we show that the intensities of the two components are decoupled at a confidence level >3sigma. The broad Fe K line has an EW of 118 (+32,-61) eV and could originate in an accretion disk (with inclination angle greater than ~30 degrees). The narrow Fe Kalpha line has an EW of 163 (+47,-26) eV and is unresolved FWHM <4090 km/s) and likely originates in distant matter. The absolute flux in the narrow line implies that the column density out of the line-of-sight could be much higher than measured in the line-of-sight, and that the mean (historically-averaged) continuum luminosity responsible for forming the line could be a factor of several higher than that measured from the data. We also detect the narrow Fe Kbeta line with a high signal-to-noise ratio and describe a new robust method to constrain the ionization state of Fe responsible for the Fe Kalpha and Fe Kbeta lines that does not require any knowledge of possible gravitational and Doppler energy shifts affecting the line energies. For the distant line-emitting matter (e.g. the putative obscuring torus) we deduce that the predominant ionization state is lower than Fe VIII (at 99% confidence), conservatively taking into account residual calibration uncertainties in the XIS energy scale and theoretical and experimental uncertainties in the Fe K fluorescent line energies. From the limits on a possible Compton-reflection continuum it is likely that the narrow Fe Kalpha and Fe Kbeta lines originate in a Compton-thin structure.Comment: Abstract is abridged. Accepted for publication in the Suzaku special issue of PASJ (November 2006). 18 pages, 6 figure

X-Ray Spectral Variability of the Seyfert Galaxy NGC 4051 Observed with Suzaku

We report results from a Suzaku observation of the narrow-line Seyfert 1 NGC 4051. During our observation, large amplitude rapid variability is seen and the averaged 2--10 keV flux is 8.1x10^-12 erg s^-1 cm^-2, which is several times lower than the historical average. The X-ray spectrum hardens when the source flux becomes lower, confirming the trend of spectral variability known for many Seyfert 1 galaxies. The broad-band averaged spectrum and spectra in high and low flux intervals are analyzed. The spectra are first fitted with a model consisting of a power-law component, a reflection continuum originating in cold matter, a blackbody component, two zones of ionized absorber, and several Gaussian emission lines. The amount of reflection is rather large (R ~ 7, where R=1 corresponds to reflection by an infinite slab), while the equivalent width of the Fe-K line at 6.4 keV is modest (140 eV) for the averaged spectrum. We then model the overall spectra by introducing partial covering for the power-law component and reflection continuum independently. The column density for the former is 1x10^23 cm^-2, while it is fixed at 1x10^24 cm-2 for the latter. By comparing the spectra in different flux states, we identify the causes of spectral variability. (abridged)Comment: 19 pages, 18 figures, accepted for publication in PASJ (Suzaku 3rd special issue

Análise de deslocamentos em partidas de basquetebol e de futebol de campo: estudo exploratório através da análise de séries temporais

Durações e intensidades de períodos de esforço e de pausa são importantes determinantes da demanda fisiológica no exercício. As técnicas de análise dos deslocamentos em esportes com bola, apesar de serem objeto de muitas investigações, não tem conseguido refletir apropriadamente o padrão de intermitência da atividade. Neste estudo, a velocidade de deslocamentos de uma equipe de basquetebol e outra de futebol de campo foi analisada através de séries de Fourier. As velocidades instantâneas de deslocamentos (Vt) em cada segundo (t) da partida foram determinadas através de videografia e análise em computador. Foram calculadas, dentre outras variáveis, o desvio padrão e a média móvel em 60 s (VMt) da Vt , a correlação de Pearson entre a VMt e t. Foi também calculado o periodograma da Vt através da transformada rápida de Fourier normalizado para o número de observações em partida (amplitude da velocidade na késima frequência: AVk). O desvio padrão da Vt foi maior no basquetebol, o r foi negativo e significativamente menor no futebol. A análise da VMt indicou um padrão periódico em ambas partidas. O exame da AVk mostrou que no basquetebol havia periodicidade nos deslocamentos em ciclos de 12, 26 e 96 s e no futebol de 140, 209 e 1037s. Conjuntamente esses resultados indicam que: a) o basquetebol apresenta maior intermitência do que o futebol com durações de esforços mais curtos; b) no futebol há tendência à diminuição da velocidade de deslocamento na partida; c) os deslocamentos nos dois tipos de partida apresentam flutuações não periódicas compatíveis com a característica da modalidade e d) a técnica de análise de séries temporais pode ser uma ferramenta útil para a descrições de deslocamentos em partida

Suzaku Observation of Two Ultraluminous X-Ray Sources in NGC 1313

Two ultraluminous X-ray sources (ULXs) in the nearby Sb galaxy NGC 1313, named X-1 and X-2, were observed with Suzaku on 2005 September 15. During the observation for a net exposure of 28~ks (but over a gross time span of 90~ks), both objects varied in intensity by about 50~%. The 0.4--10 keV X-ray luminosity of X-1 and X-2 was measured as $2.5 \times 10^{40}~{\rm erg~s^{-1}}$ and $5.8 \times 10^{39}~{\rm erg~s^{-1}}$, respectively, with the former the highest ever reported for this ULX. The spectrum of X-1 can be explained by a sum of a strong and variable power-law component with a high energy cutoff, and a stable multicolor blackbody with an innermost disk temperature of $\sim 0.2$ keV. These results suggest that X-1 was in a ``very high'' state, where the disk emission is strongly Comptonized. The absorber within NGC 1313 toward X-1 is suggested to have a subsolar oxygen abundance. The spectrum of X-2 is best represented, in its fainter phase, by a multicolor blackbody model with the innermost disk temperature of 1.2--1.3 keV, and becomes flatter as the source becomes brighter. Hence X-2 is interpreted to be in a slim-disk state. These results suggest that the two ULXs have black hole masses of a few tens to a few hundreds solar masses.Comment: accepted for publication in PAS

Suzaku Observations of Ejecta-Dominated Galactic Supernova Remnant G346.6-0.2

We present here the results of the X-ray analysis of Galactic supernova remnant G346.6-0.2 observed with {\it Suzaku}. K-shell emission lines of Mg, Si, S, Ca and Fe are detected clearly for the first time. Strong emission lines of Si and S imply that X-ray emission nature of G346.6-0.2 is ejecta-dominated. The ejecta-dominated emission is well fitted with a combined model consisting of thermal plasma in non-equilibrium ionization and a non-thermal component, which can be regarded as synchrotron emission with a photon index of $\Gamma$ $\sim 0.6$. Absorbing column density of $N_{\rm H}\sim2.1\times10^{22}$ ${\rm cm^{-2}}$ is obtained from the best-fitting implying a high-density medium, high electron temperature of $kT_{\rm e}\sim1.2$ keV, and ionization timescale of $n_{\rm e}t\sim2.9\times10^{11}$ ${\rm cm^{-3}s}$ indicating that this remnant may be far from full ionization equilibrium. The relative abundances from the ejecta show that the remnant originates from a Type Ia supernova explosion.Comment: 7 pages, 4 figur