Characterization of the X-ray light curve of the gamma Cas-like B1e star HD110432

HD 110432 (BZ Cru; B1Ve) is the brightest member of a small group of "gamma Cas analogs" that emit copious hard X-ray flux, punctuated by ubiquitous "flares." To characterize the X-ray time history of this star, we made a series of six RXTE multi-visit observations in 2010 and an extended observation with the XMM-Newton in 2007. We analyzed these new light curves along with three older XMM-Newton observations from 2002--2003. Distributed over five months, the RXTE observations were designed to search for long X-ray modulations over a few months. These observations indeed suggest the presence of a long cycle with P = 226 days and an amplitude of a factor of two. We also used X-ray light curves constructed from XMM-Newton observations to characterize the lifetimes, strengths, and interflare intervals of 1615 flare-like events in the light curves. After accounting for false positive events, we infer the presence of 955 (2002-2003) and 386 (2007) events we identified as flares. Similarly, as a control we measured the same attributes for an additional group of 541 events in XMM-Newton light curves of gamma Cas, which after a similar correction yielded 517 flares. We found that the flare properties of HD 110432 are mostly similar to our control group. In both cases the distribution of flare strengths are best fit with log-linear relations. Both the slopes of these distributions and the flaring frequencies themselves exhibit modest fluctuations. We discovered that some flares in the hard X-ray band of HD 110432 were weak or unobserved in the soft band and vice versa. The light curves also occasionally show rapid curve drop offs that are sustained for hours. We discuss the existence of the long cycle and these flare properties in the backdrop of two rival scenarios to produce hard X-rays, a magnetic star-disk interaction and the accretion of blobs onto a secondary white dwarf.Comment: 11 pages, 10 figures; accepted by the Astrophysical Journa

Executable graphics for PBNM

The specification of a policy is performed in a policy language, usually following a textual representation. However, humans process images faster than text and they are prepared to process information presented in two or more dimensions: sometimes it is easier to explain things using figures and their graphical relations than writing textual representations. This paper describes a visual language, in the form of graphics that are executed in a networking environment, to define a network management policy. This approach allows to map visual tokens and corresponding arrangements into other languages to which a mapping is defined

Revisiting the fossil group candidates UGC 842 and NGC 6034

We present a new insight on NGC 6034 and UGC 842, two groups of galaxies previously reported in the literature as being fossil groups. The study is based on optical photometry and spectroscopy obtained with the CTIO Blanco telescope and Sloan Digital Sky Survey archival data. We find that NGC 6034 is embedded in a large structure, dominated by three rich clusters and other small groups. Its first and next four ranked galaxies have magnitude differences in the r band and projected distances which violate the optical criteria to classify it as a fossil group. We confirm that the UGC 842 group is a fossil group, but with about half the velocity dispersion that is reported in previous works. The velocity distribution of its galaxies reveals the existence of two structures in its line of sight, one with sigmaV ~ 223 km/s and another with sigmaV ~ 235 km/s, with a difference in velocity of ~820 km/s. The main structure is dominated by passive galaxies, while these represent ~60% of the second structure. The X-ray temperature for the intragroup medium of a group with such a velocity dispersion is expected to be kT ~0.5-1 keV, against the observed value of kT ~1.9 keV reported in the literature. This result makes UGC 842 a special case among fossil groups because (1) it represents more likely the interaction between two small groups, which warms the intragroup medium and/or (2) it could constitute evidence that member galaxies lost energy in the process of spiraling toward the group center, and decreased the velocity dispersion of the system. As far as we know, UGC 842 is the first low-mass fossil group studied in detail.Comment: 18 pages, 8 figures, published in A

Mycorrhizal fungi were more effective than zeolites in increasing the growth of non-irrigated young olive trees

Four soil treatments, consisting of two commercial mycorrhizal fungi, one zeolite and an untreated control, were arranged in a factorial design with two foliar fertilization treatments, a foliar spray and a control to study the effects of commercial mycorrhizal fungi and zeolites on the growth of young, rainfed olive trees planted in very acidic soil. The concentrations in the plant tissues of most of essential nutrients, particularly nitrogen (N), phosphorus (P), potassium (K) and boron (B), did not significantly change with the soil treatments, whereas leaf N and B concentrations significantly increased with foliar fertilization. Leaf calcium (Ca) and magnesium (Mg) levels were found to be much lower than their respective sufficiency ranges and increased with soil amendments, also giving positive outcomes for plant water status, photosynthetic activity and assimilation area. Ultimately, the mycorrhizal fungi increased the growth of the young trees, whereas the effect of zeolites was much smaller and not significantly different to the control. Thus, it seems that in this very acidic soil and under rainfed conditions, the major benefits for plants from the application of mycorrhizal fungi and zeolites were the alleviation of drought stress and tissue Ca and Mg disorders.info:eu-repo/semantics/publishedVersio

On the mass‐to‐light ratios of fossil groups. Are they simply dark clusters?

Defined as X‐ray bright galaxy groups with large differences between the luminosities of their brightest and second brightest galaxies, ‘fossil groups’ are believed to be some of the oldest galaxy systems in the Universe. They have therefore been the subject of much recent research. In this work we present a study of 10 fossil group candidates with an average of 33 spectroscopically confirmed members per group, making this the deepest study of its type to date. We also use these data to perform an analysis of the luminosity function of our sample of fossil groups. We confirm the high masses previously reported for many of fossil systems, finding values more similar to those of clusters than of groups. We also confirm the high dynamical mass‐to‐light ratios reported in many previous studies. While our results are consistent with previous studies in many ways, our interpretation is not. This is because we show that, while the luminosities of the bright central galaxies (BCGs) in these systems are consistent with their high dynamical masses, their richnesses (total number of galaxies above some canonical value) are extremely low. This leads us to suggest a new interpretation of fossil systems in which the large differences between the luminosities of their brightest and second brightest galaxies are simply the result of the high BCG luminosities and low richnesses, while the high masses and low richnesses also explain the high mass‐to‐light ratios. Our results therefore suggest that fossil systems can be characterized as cluster‐like in their masses and BCG luminosities, but possessing the richnesses and optical luminosities of relatively poor groups. These findings are not predicted by any of the current models for the formation of fossil groups. Therefore, if this picture is confirmed, current ideas about the formation and evolution of fossil systems will need to be reformulated.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/89559/1/j.1365-2966.2011.19625.x.pd

Prognostic significance of the anatomical location and TNM clinical classification in oral squamous cell carcinoma

Objetives: The aim of this study was to investigate the existence of correlation between the TNM clinical classification, anatomical location and prognosis of oral squamous cell carcinoma. Study design: A total of 130 oral squamous cell carcinomas were selected from the files of the Dr. Luiz Antonio Hospital (Natal, Rio Grande do Norte, Brazil). Data concerning TNM clinical classification, anatomical location and prognosis were obtained. Pearsons correlation test was applied for the statistical analysis of data. Results: It revealed a statistically significant correlation (p = 0.01) between TNM clinical classification and prognosis. It also revealed correlation between TNM classification and the anatomical location of oral squamous cell carcinomas (p = 0.01). Conclusions: We concluded that TNM classification presented correlation with prognosis and with the different anatomical locations of oral squamous cell carcinomas

OS TUPIS DO GURUPI (ENSAIO COMPARATIVO)

A presente memória é um resumo do que observei, a serviço do Museu Nacional, entre os índios Urubus e tembés, em setembro e outubro de 1930, e dos resultados até agora alcançados no estudo comparativo dessas tribos. As minhas observações tiveram lugar nos postos Pedro Dantas (CanindéUaçu) e Filipe Camarão (Jararaca), do Serviço de Proteção aos Índios, na maloca tembé de Igarapé Grande e em outros da zona das cachoeiras do Gurupi. Nessa região de matas equatoriais, travou-se, desde meado do século XIX, a tragédia das incursões Urubus. Datando só de outubro de 1928 as relações pacíficas (no posto de Canindé-Uaçu), o presente estudo tem um desenvolvimento com- patível com tais circunstâncias, que em todo caso permitiram ao Autor observar-lhes costumes, dialeto e tipos, e obter boa documentação, sobretudo da arte plumária excepcional dessa horda até então considerada ferocissima e que cerceara, com os golpes das suas flechas de ferro, a área das populações rurais do Pará e do Maranhã