On the structure and evolution of a polar crown prominence/filament system

Polar crown prominences are made of chromospheric plasma partially circling the Suns poles between 60 and 70 degree latitude. We aim to diagnose the 3D dynamics of a polar crown prominence using high cadence EUV images from the Solar Dynamics Observatory (SDO)/AIA at 304 and 171A and the Ahead spacecraft of the Solar Terrestrial Relations Observatory (STEREO-A)/EUVI at 195A. Using time series across specific structures we compare flows across the disk in 195A with the prominence dynamics seen on the limb. The densest prominence material forms vertical columns which are separated by many tens of Mm and connected by dynamic bridges of plasma that are clearly visible in 304/171A two-color images. We also observe intermittent but repetitious flows with velocity 15 km/s in the prominence that appear to be associated with EUV bright points on the solar disk. The boundary between the prominence and the overlying cavity appears as a sharp edge. We discuss the structure of the coronal cavity seen both above and around the prominence. SDO/HMI and GONG magnetograms are used to infer the underlying magnetic topology. The evolution and structure of the prominence with respect to the magnetic field seems to agree with the filament linkage model.Comment: 24 pages, 14 figures, Accepted for publication in Solar Physics Journal, Movies can be found at http://www2.mps.mpg.de/data/outgoing/panesar

Physics of Solar Prominences: I - Spectral Diagnostics and Non-LTE Modelling

This review paper outlines background information and covers recent advances made via the analysis of spectra and images of prominence plasma and the increased sophistication of non-LTE (ie when there is a departure from Local Thermodynamic Equilibrium) radiative transfer models. We first describe the spectral inversion techniques that have been used to infer the plasma parameters important for the general properties of the prominence plasma in both its cool core and the hotter prominence-corona transition region. We also review studies devoted to the observation of bulk motions of the prominence plasma and to the determination of prominence mass. However, a simple inversion of spectroscopic data usually fails when the lines become optically thick at certain wavelengths. Therefore, complex non-LTE models become necessary. We thus present the basics of non-LTE radiative transfer theory and the associated multi-level radiative transfer problems. The main results of one- and two-dimensional models of the prominences and their fine-structures are presented. We then discuss the energy balance in various prominence models. Finally, we outline the outstanding observational and theoretical questions, and the directions for future progress in our understanding of solar prominences.Comment: 96 pages, 37 figures, Space Science Reviews. Some figures may have a better resolution in the published version. New version reflects minor changes brought after proof editin

Formation of a White-Light Jet within a Quadrupolar Magnetic Configuration

We analyze multi-wavelength and multi-viewpoint observations of a large-scale event viewed on 7 April 2011 originating from an active region complex. The activity leads to a white-light jet being formed in the outer corona. The topology and evolution of the coronal structures were imaged in high resolution using the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). In addition, large field-of-view images of the corona were obtained using the Sun Watcher using Active Pixel System detector and Image Processing (SWAP) telescope onboard the PRoject for Onboard Autonomy (PROBA2) microsatellite, providing evidence for the connectivity of the coronal structures with outer coronal features that were imaged with the Large Angle Spectrometric Coronagraph (LASCO) C2 on Solar and Heliospheric Observatory (SOHO). The data-sets reveal an Eiffel-tower type jet configuration extending into a narrow jet in the outer corona. The event starts from the growth of a dark area in the central part of the structure. The darkening was also observed in projection on the disk by the Solar TErrestrial RElations Observatory-Ahead (STEREO-A) spacecraft from a different point of view. We assume that the dark volume in the corona descends from a coronal cavity of a flux rope that moved up higher in the corona but still failed to erupt. The quadrupolar magnetic configuration corresponds to a saddle-like shape of the dark volume and provides a possibility for the plasma to escape along the open field lines into the outer corona, forming the white-light jet.Comment: 15 pages, 10 figure

Precision Measurement of the Proton Flux in Primary Cosmic Rays from Rigidity 1 GV to 1.8 TV with the Alpha Magnetic Spectrometer on the International Space Station

A precise measurement of the proton flux in primary cosmic rays with rigidity (momentum/charge) from 1 GV to 1.8 TV is presented based on 300 million events. Knowledge of the rigidity dependence of the proton flux is important in understanding the origin, acceleration, and propagation of cosmic rays. We present the detailed variation with rigidity of the flux spectral index for the first time. The spectral index progressively hardens at high rigidities.</p

Qualidade do inhame 'Da Costa' em função das épocas de colheita e da adubação orgânica Da Costa yam quality in relation to harvest time and organic fertilization

Foi desenvolvido um trabalho na EMEPA em João Pessoa, entre setembro/98 e junho/99, com o objetivo de quantificar o teor de matéria seca, de amido e de cinzas em rizomas do inhame, cultivar Da Costa, em função das épocas de colheita e da adubação orgânica, em solo Podzólico Vermelho-Amarelo, textura arenosa. Estudaram-se níveis de esterco bovino (5; 10; 15 e 20 t/ha) e de esterco de galinha (2,8; 5,6; 8,4 e 11,2 t/ha), duas épocas de colheita (sete e nove meses após o plantio) e uma testemunha, sem resíduo orgânico. Os tratamentos foram arranjados como fatorial 2x4x2+1, no delineamento de blocos casualizados, com quatro repetições. O teor de matéria seca nos rizomas aumentou com a maturidade do cará-da-costa, passando de 33% em rizomas colhidos aos sete meses, para 36% em rizoma colhidos aos nove meses. Os teores de matéria seca nos rizomas colhidos aos sete meses decresceram de 35,80% e 34,71%, respectivamente, na ausência de estercos para 30,03% e 29,25%, respectivamente, com as doses de 20 t/ha de esterco bovino e de 11,2 t/ha de esterco de galinha. Na colheita realizada aos sete meses, o teor de amido foi de 26%, elevando-se para 29% na colheita aos noves meses. O teor de amido, na colheita realizada aos nove meses, aumentou com as doses de esterco de galinha, atingindo o máximo de 31,6% com a dose de 4,8 t/ha. O teor de cinzas nos rizomas não foi influenciado pelas épocas de colheita, mas naqueles colhidos aos nove meses, o teor aumentou com as doses de esterco bovino e de galinha, atingindo o máximo de 0,78 e 0,67%, respectivamente, nas doses de 12,8 e 6,7 t/ha.<br>An experiment was carried out in EMEPA, João Pessoa, Brazil between September 98 and June 99 to quantify the dry matter, starch and ash content of yam rhizomes, cv. Da Costa, in relation to harvest time and organic fertilization. The area consisted of a red-yellow podzolic sandy soil. Four levels of cattle manure (5; 10; 15 and 20 t/ha), four levels of chicken manure (2.8; 5.6; 8.4 and 11.2 t/ha), and two harvest times [seven and nine months after planting date (APD))] plus a treatment without organic residue, were studied, arranged in a factorial cheme 2x4x2+1 in randomized blocks, with four replications. Dry matter was of 33% and 36% in rhizomes harvested seven and nine months APD, respectively. At seven months APD, dry matter decreased from 35.80% and 34.71%, without cattle or chicken manure, respectively, to 30.03% and 29.25%, for highest levels of cattle manure (20 t/ha) and chicken manure (11.2 t/ha). Starch content increased from 26% at seven months APD to 29% at nine months APD. Nine months APD, starch content in rhizomes increased (31.6%) with increasing levels of chicken manure (4.8 t/ha). Ash content was not affected by harvest dates. However, applying 12.8 t/ha of cattle manure and 6.7 t/ha of chicken manure, rhizomes presented increase in ash content of 0.78% and 0.67% respectively, when harvested nine months APD