Eruptions of Magnetic Ropes in Two Homologous Solar Events on 2002 June 1 and 2: a Key to Understanding of an Enigmatic Flare

The goal of this paper is to understand the drivers, configurations, and scenarios of two similar eruptive events, which occurred in the same solar active region 9973 on 2002 June 1 and 2. The June 2 event was previously studied by Sui, Holman, and Dennis (2006, 2008), who concluded that it was challenging for popular flare models. Using multi-spectral data, we analyze a combination of the two events. Each of the events exhibited an evolving cusp-like feature. We have revealed that these apparent ``cusps'' were most likely mimicked by twisted magnetic flux ropes, but unlikely to be related to the inverted Y-like magnetic configuration in the standard flare model. The ropes originated inside a funnel-like magnetic domain whose base was bounded by an EUV ring structure, and the top was associated with a coronal null point. The ropes appear to be the major drivers for the events, but their rise was not triggered by reconnection in the coronal null point. We propose a scenario and a three-dimensional scheme for these events in which the filament eruptions and flares were caused by interaction of the ropes.Comment: 22 pages, 11 figure

4pi Models of CMEs and ICMEs

Coronal mass ejections (CMEs), which dynamically connect the solar surface to the far reaches of interplanetary space, represent a major anifestation of solar activity. They are not only of principal interest but also play a pivotal role in the context of space weather predictions. The steady improvement of both numerical methods and computational resources during recent years has allowed for the creation of increasingly realistic models of interplanetary CMEs (ICMEs), which can now be compared to high-quality observational data from various space-bound missions. This review discusses existing models of CMEs, characterizing them by scientific aim and scope, CME initiation method, and physical effects included, thereby stressing the importance of fully 3-D ('4pi') spatial coverage.Comment: 14 pages plus references. Comments welcome. Accepted for publication in Solar Physics (SUN-360 topical issue

Velocity-space sensitivity of the time-of-flight neutron spectrometer at JET

The velocity-space sensitivities of fast-ion diagnostics are often described by so-called weight functions. Recently, we formulated weight functions showing the velocity-space sensitivity of the often dominant beam-target part of neutron energy spectra. These weight functions for neutron emission spectrometry (NES) are independent of the particular NES diagnostic. Here we apply these NES weight functions to the time-of-flight spectrometer TOFOR at JET. By taking the instrumental response function of TOFOR into account, we calculate time-of-flight NES weight functions that enable us to directly determine the velocity-space sensitivity of a given part of a measured time-of-flight spectrum from TOFOR

A Revisit of the Masuda Flare

We revisit the flare on 1992 January 13, which is now universally termed the "Masuda flare". The revisit is motivated not only by its uniqueness despite accumulating observations of \hxr coronal emission, but also by the improvement of Yohkoh hard X-ray imaging, which was achieved after the intensive investigations on this celebrated event. Through an uncertainty analysis, we show that the hard X-ray coronal source is located much closer to the soft X-ray loop in the re-calibrated HXT images than in the original ones. Specifically, the centroid of the M1-band (23--33 keV) coronal source is above the brightest pixel of the SXT loop by ~5000+/-1000 km (~9600 km in the original data); and above the apex of the 30% brightness contour of the SXT loop by ~2000+/-1000 km (~7000 km in the original data). We suggest that this change may naturally account for the fact that the spectrum of the coronal emission was reported to be extremely hard below ~20 keV in the pre-calibration investigations, whereas it has been considerably softer in the literature since Sato's re-calibration circa 1999. Still, the coronal spectrum is flatter at lower energies than at higher energies, owing to the lack of a similar source in the L-band (14--23 keV), which remains a puzzle

Elliptical galaxy nuclei activity powered by infalling globular clusters

Globular cluster systems evolve, in galaxies, due to internal and external dynamics and tidal phenomena. One of the causes of evolution, dynamical friction, is responsible for the orbital decay of massive clusters into the innermost galactic regions. It is found that these clusters are effective source of matter to feed a central galactic black hole such to make it grow and shine as an AGN.Comment: 8 pages, 2 eps figures, in press in the Proc. of the Meeting Baryons in Cosmic Structures, Monte Porzio (Italy), oct. 20-21 2003, ASP Conf. Ser., eds. E. Giallongo, G. De Zotti, N. Menc

An Observational Overview of Solar Flares

We present an overview of solar flares and associated phenomena, drawing upon a wide range of observational data primarily from the RHESSI era. Following an introductory discussion and overview of the status of observational capabilities, the article is split into topical sections which deal with different areas of flare phenomena (footpoints and ribbons, coronal sources, relationship to coronal mass ejections) and their interconnections. We also discuss flare soft X-ray spectroscopy and the energetics of the process. The emphasis is to describe the observations from multiple points of view, while bearing in mind the models that link them to each other and to theory. The present theoretical and observational understanding of solar flares is far from complete, so we conclude with a brief discussion of models, and a list of missing but important observations.Comment: This is an article for a monograph on the physics of solar flares, inspired by RHESSI observations. The individual articles are to appear in Space Science Reviews (2011

Consumo de nutrientes e comportamento ingestivo de cordeiros da raça Santa Inês alimentados com rações com diferentes níveis de energia metabolizável

Objetivou-se avaliar o consumo de nutrientes e o comportamento ingestivo de cordeiros da raça Santa Inês na fase de cria alimentados com diferentes níveis de energia metabolizável (EM). Foram utilizados 20 cordeiros não-castrados, com idade e peso corporal médio de 50 dias e 13,00 ± 0,56 kg, respectivamente, distribuídos em quatro tratamentos experimentais com diferentes níveis de energia metabolizável (2,08; 2,28; 2,47 e 2,69 Mcal de EM/kg de matéria seca), em delineamento em blocos casualizados, com cinco repetições. Como volumoso utilizou-se feno de capim-tifton adicionado à ração concentrada. Os níveis de energia metabolizável (EM) tiveram efeito linear sobre os consumos de matéria seca, matéria orgânica, proteína bruta, extrato etéreo, carboidratos não-fibrosos e nutrientes digestíveis totais, expressos em g/dia. O consumo de FDN, expresso em %PV e kg/PV0,75, decresceu linearmente com o aumento dos níveis de energia nas rações, devido à redução no teor de FDN na matéria seca total das rações. Os tempos de alimentação e mastigação total, expressos em hora/dia, diminuíram linearmente com os níveis energéticos das rações experimentais. Em compensação, o tempo de ócio aumentou linearmente e o de ruminação não foi influenciado pelos níveis energéticos das rações. O número de bolos ruminais, de mastigações merícicas e de mastigações merícicas por bolo ruminal e o tempo de mastigações merícicas por bolo ruminal não foram influenciados pelos níveis de energia metabolizável nas rações. O aumento dos níveis de energia metabolizável das rações influencia o consumo de nutrientes e o comportamento ingestivo de cordeiros da raça Santa Inês na fase de cria.The objective of this work was to evaluate the nutrient intake and ingestive behavior of growing Santa Inês lambs fed different levels of metabolizable energy (ME). It was used 20 non-castrated lambs at 50 days of age and with 13.00 ± 0.56 kg of body weight. The animals were distributed into four experimental treatments with different levels of metabolizable energy (2.08, 2.28, 2.47 and 2.69 Mcal/kg of dry matter) in a randomized block design with five replications. It was used as roughage tifton hay added to concentrate diet. Levels of metabolizable energy (ME) linearly affected intakes of dry matter, organic matter, crude protein, ether extract, no-fiber carbohydrates, and total digestible nutrients, expressed in g/day. The NDF intake, expressed as % BW and kg/BW0.75, decreased linearly with the increase of levels of energy in the diet due to the reduction in NDF content in the total dietary dry matter. Feeding and total chewing time, expressed in hour/day, decreased linearly with the energy levels of the experimental diets. However, idle time increased linearly, whereas rumination was not influenced by energy levels of the diets. Number of ruminate boli, of ruminating chews, of ruminating chews per bolus and time of chewing per bolus were not influenced by levels of metabolizable energy in the diets. Increase in metabolizable energy levels of diets affects intake of nutrients and ingestive behavior of growing Santa Inês lambs

Star clusters near and far; tracing star formation across cosmic time

© 2020 Springer-Verlag. The final publication is available at Springer via https://doi.org/10.1007/s11214-020-00690-x.Star clusters are fundamental units of stellar feedback and unique tracers of their host galactic properties. In this review, we will first focus on their constituents, i.e.\ detailed insight into their stellar populations and their surrounding ionised, warm, neutral, and molecular gas. We, then, move beyond the Local Group to review star cluster populations at various evolutionary stages, and in diverse galactic environmental conditions accessible in the local Universe. At high redshift, where conditions for cluster formation and evolution are more extreme, we are only able to observe the integrated light of a handful of objects that we believe will become globular clusters. We therefore discuss how numerical and analytical methods, informed by the observed properties of cluster populations in the local Universe, are used to develop sophisticated simulations potentially capable of disentangling the genetic map of galaxy formation and assembly that is carried by globular cluster populations.Peer reviewedFinal Accepted Versio