Ciro Pinto | Universidade Federal do Rio Grande do Norte (original) (raw)

Papers by Ciro Pinto

Irriga, Oct 1, 2012

Este trabalho teve por objetivo estudar os efeitos da aplicação de água (CEa = 0,5 dS m -1 ) e/ou... more Este trabalho teve por objetivo estudar os efeitos da aplicação de água (CEa = 0,5 dS m -1 ) e/ou solução salina (CEa = 5,0 dS m -1 ), alternadamente, nas duas fases iniciais de desenvolvimento do feijão de corda cv. Epace 10. O experimento foi realizado, em condições de ambiente protegido (telado), na Embrapa Agroindústria Tropical. As sementes foram colocadas em vasos com capacidade para 15 L dispostos em um delineamento de blocos ao acaso, com 4 tratamentos e quatro repetições. As plantas foram submetidas aos tratamentos: 1. irrigação com água até o final da fase II; 2. irrigação com solução salina até o final da fase II, 3. irrigação com água até o final da fase I e solução salina até o final da fase II e 4. Irrigação com solução salina até o final da fase I e água até o final da fase II, momento em que os dados foram coletados. O crescimento não foi afetado pela aplicação de solução salina, independente da fase aplicada. Nos solutos compatíveis verificou-se redução nos teores de proteínas. PALAVRAS-CHAVE: Vigna unguiculata L. estresse salino, crescimento CALVET, A. S. F.; PINTO, C. de M.; LIMA, R. E. M.; MAIA-JOCA, R. P. M.; BEZERRA, M. A. GROWTH AND SOLUTE ACCUMULATION IN COWPEA IRRIGATED WITH WATERS RISING SALINITY IN DIFFERENT STAGES OF DEVELOPMENT

Revista Ciencia Agronomica, Nov 29, 2010

Resumo -Foram analisadas as variações sazonais nas taxas de trocas gasosas em lâminas foliares, s... more Resumo -Foram analisadas as variações sazonais nas taxas de trocas gasosas em lâminas foliares, sombreadas e a pleno sol, de cajueiro anão precoce (Anacardium occidentale L.), quando submetidas aos regimes de irrigação e de sequeiro. Os clones CCP 76 e BRS 189 foram mensalmente avaliados quanto ao seu desempenho fisiológico em relação à condutância estomática (g s ), às taxas transpiratórias (E) e fotossintéticas (A), à temperatura foliar e à relação entre as concentrações interna e externa de CO 2 (C i /C e ). O experimento foi conduzido entre setembro de 2006 e agosto de 2007, na estação experimental da Embrapa Agroindústria Tropical, localizada no município de Paraipaba, Ceará. As variáveis A, g s , E e C i /C e foram afetadas apenas em função da época do ano e dos tipos de folhas. A maior influência nos fatores fisiológicos analisados ocorreu devido às condições em que as folhas estavam submetidas (sol ou sombra) e aos fatores meteorológicos e não à supressão da irrigação. Isto, possivelmente porque os resultados aqui obtidos estejam mais bem relacionados com as fases fenológicas da cultura do que com os tratamentos, demonstrando assim o conspícuo efeito fisiológico da força dos drenos e da irradiância nessas plantas.

Revista Verde De Agroecologia E Desenvolvimento Sustentavel, Jun 13, 2011

... Junior Regis Batista Cysne Engenheiro Agrônomo, Doutor em Agronomia/Fitotecnia, UFC, Fortalez... more ... Junior Regis Batista Cysne Engenheiro Agrônomo, Doutor em Agronomia/Fitotecnia, UFC, Fortaleza-CE E-mail: junior.cysne@gmail.com ... JANA, AC; BARRIGA, BP; KRARUP, HA; FUENTES, RP Eficiencia de la asocion maiz (Zea mays) y frejol (Phaseolus vulgaris). ...

Revista Verde De Agroecologia E Desenvolvimento Sustentavel, May 4, 2013

Helioseismology is the branch of the Solar Physics which studies the solar global oscillations, a... more Helioseismology is the branch of the Solar Physics which studies the solar global oscillations, a phenomenon very important in order to understand the inside of the Sun. We explain here a method for measuring the solar velocity fields along the line of sight by the VAMOS instrument developed at the Astronomical Observatory of Capodimonte in Naples, in particular we present the measures of the so called five-minutes oscillations and of the Supergranulation

Com o objetivo de avaliar o potencial do bagaço de caju na composição de substratos foi desenvolv... more Com o objetivo de avaliar o potencial do bagaço de caju na composição de substratos foi desenvolvido um experimento sob condições de casa de vegetação. O delineamento experimental utilizado foi em blocos ao acaso com c inco tratamentos (0; 15; 30; 45 e 60 t ha -1 , na base seca) e quatro repetições, totalizando 20 parcelas experimentais. Avali aram-se os atributos químicos do substrato antes e depois do cultivo de pimentão : pH, matéria orgânica (M.O.), P, K, Ca, Mg, acidez potencial (H+Al), soma de bases (SB), capacidade de troca de cátions (CTC) e índice de saturação por base (V%). Todas as variáveis avaliadas foram alteradas significativamente pela adição crescente de bagaço de caju ao substrato. As concentrações médias de M.O., P, K, H+Al e valores de SB, CTC e V% variaram de 13 a 18,7 g dm -3 ; 7 a 19 mg dm -3 ; 3,4 a 9; 12,9 a 14,8; 19,8 a 26,3; 33,6 a 39,4 e 59 a 67 mmol c dm -3 , respectivamente, e apresentaram um modelo linear de regressão. As médias de pH, Ca e Mg apresentaram modelo quadrático de regressão e variaram de 5,0 a 5,2; 6 a 13 e 3,8 a 6,3 mmol c dm -3 , respectivamente. Palavras-chaves: Anacardium occidentale, bagaço de caju

Revista Ciencia Agronomica

Revista Ciência Agronômica, 2010

Irriga, 2012

The Astrophysical Journal, 2011

Two XMM-Newton observations of the fast classical nova V2491 Cyg were carried out in short succes... more Two XMM-Newton observations of the fast classical nova V2491 Cyg were carried out in short succession on days 39.93 and 49.62 after discovery, during the supersoft source (SSS) phase, yielding simultaneous X-ray and UV light curves and high-resolution X-ray spectra. The first X-ray light curve is highly variable, showing oscillations with a period of 37.2 minutes after an extended factor of three decline lasting ∼ 3 hours, while the second X-ray light curve is less variable. The cause of the dip is currently unexplained and has most likely the same origin as similar events in the early SSS light curves of the novae V4743 Sgr and RS Oph, as it occurred on the same time scale. The oscillations are not present during the dip minimum and also not in the second observation. The UV light curves are variable but contain no dips and no period. High-resolution X-ray spectra are presented for 4 intervals of differing intensity. All spectra are atmospheric continua with deep absorption lines and absorption edges. Two interstellar lines of O i and N i are clearly seen at their rest wavelengths, while a large number of high-ionization absorption lines are found at blue shifts indicating an expansion velocity of 3000−3400 km s −1 , which does not change significantly during the epochs of observation. Comparisons with the slower nova V4743 Sgr and the symbiotic recurrent nova RS Oph are presented. The SSS spectrum of V4743 Sgr is much softer with broader and more complex photospheric absorption lines. The ejecta are extended, allowing us to view a larger range of the radial velocity profile. Meanwhile, the absorption lines in RS Oph are as narrow as in V2491 Cyg, but they are less blue shifted. A remarkable similarity in the continua of V2491 Cyg and RS Oph is found. The only differences are smaller line shifts and additional emission lines in RS Oph that are related to the presence of a dense stellar wind from the evolved companion. Three unidentified absorption lines are present in the X-ray spectra of all three novae, with projected rest wavelengths 26.05Å, 29.45Å, and 30.0Å. No entirely satisfactory spectral model is currently available for the soft X-ray spectra of novae in outburst, and careful discussion of assumptions is required.

Astronomy and Astrophysics, 2010

Aims. The interstellar medium (ISM) has a multiphase structure characterized by gas, dust and mol... more Aims. The interstellar medium (ISM) has a multiphase structure characterized by gas, dust and molecules. The gas can be found in different charge states: neutral, low-ionized (warm) and high-ionized (hot). It is possible to probe the multiphase ISM through the observation of its absorption lines and edges in the X-ray spectra of background sources. Methods. We present a high-quality RGS spectrum of the low-mass X-ray binary GS 1826−238 with an unprecedent detailed treatment of the absorption features due to the dust and both the neutral and ionized gas of the ISM. We constrain the column density ratios within the different phases of the ISM and measure the abundances of elements such as O, Ne, Fe and Mg. Results. We found significant deviations from the proto-Solar abundances: oxygen is over-abundant by a factor 1.23 ± 0.05, neon 1.75 ± 0.11, iron 1.37 ± 0.17 and magnesium 2.45 ± 0.35. The abundances are consistent with the measured metallicity gradient in our Galaxy: the ISM appears to be metal-rich in the inner regions. The spectrum also shows the presence of warm/hot ionized gas. The gas column has a total ionization degree less than 10%. We also show that dust plays an important role as expected from the position of GS 1826−238: most iron appears to be bound in dust grains, while 10−40% of oxygen consists of a mixture of dust and molecules.

Astronomy & Astrophysics, 2012

The X-ray flux of Nova V2491 Cyg reached a maximum some forty days after optical maximum. The X-r... more The X-ray flux of Nova V2491 Cyg reached a maximum some forty days after optical maximum. The X-ray spectrum at that time, obtained with the RGS of XMM-Newton, shows deep, blue-shifted absorption by ions of a wide range of ionization. We show that the deep absorption lines of the X-ray spectrum at maximum, and nine days later, are well described by the following phenomenological model with emission from a central blackbody and from a collisionally ionized plasma (CIE). The blackbody spectrum (BB) is absorbed by three main highly-ionized expanding shells; the CIE and BB are absorbed by cold circumstellar and interstellar matter that includes dust. The outflow density does not decrease monotonically with distance. The abundances of the shells indicate that they were ejected from an O-Ne white dwarf. We show that the variations on time scales of hours in the X-ray spectrum are caused by a combination of variation in the central source and in the column density of the ionized shells. Our phenomenological model gives the best description so far of the supersoft X-ray spectrum of nova V2491 Cyg, but underpredicts, by a large factor, the optical and ultraviolet flux. The X-ray part of the spectrum must originate from a very different layer in the expanding envelope, presumably much closer to the white dwarf than the layers responsible for the optical/ultraviolet spectrum. This is confirmed by absence of any correlation between the X-ray and UV/optical observed fluxes.

Arxiv preprint arXiv:1010.5922, Oct 28, 2010

Abstract: The Wide Field X-ray Telescope (WFXT) is a proposed mission with a high survey speed, d... more Abstract: The Wide Field X-ray Telescope (WFXT) is a proposed mission with a high survey speed, due to the combination of large field of view (FOV) and effective area, ie grasp, and sharp PSF across the whole FOV. These characteristics make it suitable to detect a large number of variable and transient X-ray sources during its operating lifetime. Here we present estimates of the WFXT capabilities in the time domain, allowing to study the variability of thousand of AGNs with significant detail, as well as to constrain the rates and properties of ...

Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 2014

The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions ... more The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions developed by the Institute of Space and Astronautical Science (ISAS), with a planned launch in 2015. The ASTRO-H mission is equipped with a suite of sensitive instruments with the highest energy resolution ever achieved at E > 3 keV and a wide energy range spanning four decades in energy from soft X-rays to gamma-rays. The simultaneous broad band pass, coupled with the high spectral resolution of ∆E 7 eV of the micro-calorimeter, will enable a wide variety of important science themes to be pursued. ASTRO-H is expected to provide breakthrough results in scientific areas as diverse as the large-scale structure of the Universe and its evolution, the behavior of matter in the gravitational strong field regime, the physical conditions in sites of cosmic-ray acceleration, and the distribution of dark matter in galaxy clusters at different redshifts.

ABSTRACT We discuss some of the highlights of our monitoring campaign on the Seyfert 1 galaxy Mrk... more ABSTRACT We discuss some of the highlights of our monitoring campaign on the Seyfert 1 galaxy Mrk 509 that was conducted in 2009. We focus here on the ionization structure of the outflow.

We observed Mrk 509 during the fall of 2009 during a multiwavelength campaign using XMM-Newton, C... more We observed Mrk 509 during the fall of 2009 during a multiwavelength campaign using XMM-Newton, Chandra, HST/COS, SWIFT, and Integral. The 600ks XMM/RGS spectrum finds two kinematic components and a discrete distribution of ionized absorbers. Our high S/N COS spectrum detects additional complexity in the known UV absorption troughs from a variety of sources in Mrk 509, including the out-1 2 Kriss et al.