Compact sources of suprathermal microwave emission detected in quiescent active regions during lunar occultations

Solar quiescent active regions are known to exhibit radio emission from discrete structures. The knowledge of their dimensions and brightness temperatures is essential for understanding the physics of quiescent, confined plasma regions. Solar eclipses of 10 August, 1980 and 26 January, 1990, observed with high sensitivity and high time resolution at 22 GHz, allowed an unprecedented opportunity to identify Fresnel diffraction effects during lunar occultations of active regions. The results indicate the presence of quiescent discrete sources smaller than one arcsecond in one dimension. Assuming symmetrical sources, their brightness temperatures were larger than 2 × 10⁷ K and 8 × 10⁷ K, for the 1980 and 1990 observations, respectively.In memoriam, 1942–1981.     

Search for circular polarized emission from solar hemispheres at microwaves

Solar mappings with moderate angular resolution at 7 GHz seem to support the hemispherical dependence of the sense of circular polarization being right-handed for the southern hemisphere, and left-handed for the northern hemisphere. One explanation of the effect can be found by taking into account the missing fields from active centers, emerging from one hemisphere and immersing into the other.     

On the long-term behaviour of the circular polarization from coronal condensation radio emission at 4.3 cm wavelength

The circular polarization from coronal condensations at = 4.3 cm correspond to the extraordinary mode of propagation, due to the contribution of preceding spots' polarities, being usually left-handed. The fewer cases of right-handed polarization are normally associated to an excess of sunspot plages in the southern hemisphere, thus making it difficult to give evidence for magnetoionic coupling phenomena as a general rule.     

Persistent 1.5 s oscillations superimposed to a solar burst observed at two mm-wavelengths

Long-enduring quasi-periodic oscilations (1.5s) superimposed upon a solar burst have for the first time been observed simultaneously at two different mm-wavelengths (22 GHz and 44 GHz). The oscillations were present throughout the burst duration (about 10 min), and were delayed at 44 GHz with respect to 22 GHz by 0.3 s. The relative amplitude of the oscillation was of about 20% at 44 GHz and of about 5% at 22 GHz. Interferometer measurements at 10.6 GHz indicated the burst source position stable within 1 arc sec. An He i D₃ line flare showed two persistent small spots separated by about 10 arc sec. The 22/44 GHz burst position corresponds well with the location of the He i D₃ spots. The oscillations display features which distinguish them from ultrafast time structures found in other bursts. One possible interpretation is a modulation of the synchrotron emission of trapped electrons by a variable magnetic field on a double burst source, optically thin at 44 GHz and with optical thickness 0.3 at 22 GHz.     

Design and implementation of a Space-Time Intelligence System for disease surveillance

Modeling chronic and infectious diseases entails tracking and describing individuals and their attributes (such as disease status, date of diagnosis, risk factors and so on) as they move and change through space and time. Using Geographic Information Systems, researchers can model, visualize and query spatial data, but their ability to address time has been limited by the lack of temporal referencing in the underlying data structures. In this paper, we discuss issues in designing data structures, indexing, and queries for spatio-temporal data within the context of health surveillance. We describe a space-time object model that treats modeled individuals as a chain of linked observations comprised of an ID, space-time coordinate, and time-referenced attributes. Movement models for these modeled individuals are functions that may be simple (e.g. linear, using vector representation) or more complex. We present several spatial, temporal, spatio-temporal and epidemiological queries emergent from the data model. We demonstrate this approach in a representative application, a simulation of the spread of influenza in a hospital ward.This research was supported by grant R44ES010220 from the National Institute of Environmental Health Sciences (NIEHS) and by grants R01CA092669 and R01CA96002 from the National Cancer Institute (NCI). The content of this paper does not necessarily represent the official views of the NIEHS or the NCI.     

Unusual Emissions at Various Energies Prior to the Impulsive Phase of the Large Solar Flare and Coronal Mass Ejection of 4 November 2003

The GOES X28 flare of 4 November 2003 was the largest ever recorded in its class. It produced the first evidence for two spectrally separated emission components, one at microwaves and the other in the THz range of frequencies. We analyzed the pre-flare phase of this large flare, twenty?minutes before the onset of the major impulsive burst. This period is characterized by unusual activity in X-rays, sub-THz frequencies, H??, and microwaves. The CME onset occurred before the onset of the large burst by about 6?min. It was preceded by pulsations of 3??C?5?s periods at sub-THz frequencies together with X-ray and microwave enhancements. The sub-THz pulsations faded out as impulsive bursts were detected at 100??C?300?keV and 7?GHz, close to the time of the first H?? brightening and the CME onset. The activities detected prior to and at the CME onset were located nearly 2?arcmin south of the following large flare, suggesting they were separate events. This unusual activity brings new clues to understanding the complex energy buildup mechanisms prior to the CME onset, occurring at a distinct location and well before the major flare that exploded afterwards.     

Characterization of marine debris in North Carolina salt marshes

Marine debris composition, density, abundance, and accumulation were evaluated in salt marshes in Carteret County, North Carolina seasonally between 2007 and 2009. We assessed relationships between human use patterns and debris type. Wave effects on marine debris density were examined using a GIS-based forecasting tool. We assessed the influence of site wave exposure, period, and height on debris quantity. Presence and abundance of debris were related to wave exposure, vegetation type and proximity of the strata to human population and human use patterns. Plastic pieces accounted for the majority of all debris. Small debris (0–5 cm) was primarily composed of foam pieces and was frequently affiliated with natural wrack. Large debris (>100 cm) was encountered in all marsh habitat types surveyed and was primarily composed of anthropogenic wood and derelict fishing gear. Marsh cleanup efforts should be targeted to specific habitat types or debris types to minimize further damage to sensitive habitats.     

Fast discrete emissions at hard X-rays and sub-mm-IR waves in the impulsive phase of solar bursts

The time profiles of electromagnetic fluxes at hard X-rays and short microwaves are signatures of the energy conversion mechanisms at the origin of solar flares. The distinction between continuum and discrete energy production brings drastic conceptual consequences for the interpretation of the energy conversion processes. As more sensitive detectors were used on measurements with higher time resolution, the notion of continuum energy release in the impulsive phase is being replaced by the concept of repetitive energy production or Elementary Flare Bursts manifested at hard X-rays and by rapid time structures in microwave emissions. These discrete time structures are now known to be as short as tens of milliseconds, and part of their emissions are possibly produced by the same populations of accelerated electrons. Fast spikes, with mm-wave emission fluxes increasing for shorter wavelengths, simultaneous with hard X-rays, bring severe constraints for interpretation. This problem is reviewed, with the suggestion of a possible significant burst emission component in the sub-mm-IR range, due to primeval short-lived explosive compact sources, for which there are still no diagnostics.Dedicated to Cornelis de Jager     

Sedimentologische Untersuchungen im Jungpaläozoikum der Östlichen Iberischen Ketten (Spanien)

Zusammenfassung Das Jungpaläozoikum (Unterkarbon — 'Namuro-Westfal) im Südteil der Östlichen Iberischen Ketten ist über 1000 m mächtig. Es sind eugeosynklinale Sedimente in Flyschfazies.Im Flysch kommen Rutschmassen im Wechsel mit Turbiditen, synsedimentäre und syndiagenetische Schichtverbiegungen und 'en-bloc-Bewegungen größerer Schichtverbände vor.Lithofazielle Vergleiche der jungpaläozoischen Schichten der Östlichen Iberischen Ketten mit denen Kataloniens, sowie Vergleiche der Schüttungsrichtungen beider Gebiete deuten darauf hin, daß im Jungpaläozoikum keine 'Ebro-Masse bestanden haben kann.

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In the southern part of the East Iberian Chains the upper paleozoic (lower Carboniferous — 'Namuro-Westfal) piles up to a thickness of more than 1000 m. The sediments are eugeosynclinal and in a flysch facies.This flysch contains slumps alternating with turbidites, synsedimentary and syndiagenetic deformations of beds as well as 'en bloc movements of bigger units.Comparing the upper paleozoic sediments of the East Iberian Chains with those of Catalonia, due to their rock facies and their current directions in both regions we come to the conclusion that during the upper paleozoic an 'Ebro-Masse was absent.

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Résumé La puissance du paléozoïque supérieur (Carbonifère inférieur — 'Namuro-Westfal) situé au Sud de le Chaîne Ibérique atteint plus de 1000 m. Dans le faciès du Flysch il est formé de sédiments eugéosynclinaux.Dans le Flysch, on observe des glissements alternant avec des turbidites ainsi que des déformations synsédimentaires et syndiagénétiques des couches et des mouvements 'en bloc des grands ensembles des couches.Des comparaisons lithofaciales entre les couches du paléozoïque supérieur de la Chaîne Ibérique et celles de Catalogne, ainsi que des comparaisons entre les directions des matériaux transportés de ces deux régions laissent penser qu'il est impossible qu'une 'Ebro-Masse se soit formée dans le paléozoïque supérieur.

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