995 resultados para Stars: individual: LS III 46 11
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324 p.
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This work presents the first integral field spectroscopy of the Homunculus nebula around eta Carinae in the near-infrared spectral region (J band). We confirmed the presence of a hole on the polar region of each lobe, as indicated by previous near-IR long-slit spectra and mid-IR images. The holes can be described as a cylinder of height (i.e. the thickness of the lobe) and diameter of 6.5 and 6.0 x 10(16) cm, respectively. We also mapped the blue-shifted component of He I lambda 10830 seen towards the NW lobe. Contrary to previous works, we suggested that this blue-shifted component is not related to the Paddle but it is indeed in the equatorial disc. We confirmed the claim of N. Smith and showed that the spatial extent of the Little Homunculus matches remarkably well the radio continuum emission at 3 cm, indicating that the Little Homunculus can be regarded as a small H II region. Therefore, we used the optically thin 1.3 mm radio flux to derive a lower limit for the number of Lyman-continuum photons of the central source in eta Car. In the context of a binary system, and assuming that the ionizing flux comes entirely from the hot companion star, the lower limit for its spectral type and luminosity class ranges from O5.5 III to O7 I. Moreover, we showed that the radio peak at 1.7 arcsec NW from the central star is in the same line-of-sight of the `Sr-filament` but they are obviously spatially separated, while the blue-shifted component of He I lambda 10830 may be related to the radio peak and can be explained by the ultraviolet radiation from the companion star.
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A full description of the 5.5-yr low excitation events in. Carinae is presented. We show that they are not as simple and brief as previously thought, but a combination of two components. The first, the slow variation component, is revealed by slow changes in the ionization level of circumstellar matter across the whole cycle and is caused by gradual changes in the wind wind collision shock-cone orientation, angular opening and gaseous content. The second, the collapse component, is restricted to around the minimum, and is due to a temporary global collapse of the wind-wind collision shock. High-energy photons (E > 16 eV) from the companion star are strongly shielded, leaving the Weigelt objects at low-ionization state for more than six months. High-energy phenomena are sensitive only to the collapse, low energy only to the slow variation and intermediate energies to both components. Simple eclipses and mechanisms effective only near periastron (e. g. shell ejection or accretion on to the secondary star) cannot account for the whole 5.5-yr cycle. We find anti-correlated changes in the intensity and the radial velocity of P Cygni absorption profiles in Fe II lambda 6455 and He I lambda 7065 lines, indicating that the former is associated to the primary and the latter to the secondary star. We present a set of light curves representative of the whole spectrum, useful for monitoring the next event (2009 January 11).
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Extensive spectral observations of eta Carinae over the last cycle, and particularly around the 2003.5 low-excitation event, have been obtained. The variability of both narrow and broad lines, when combined with data taken from two earlier cycles, reveal a common and well-defined period. We have combined the cycle lengths derived from the many lines in the optical spectrum with those from broad-band X-rays, optical and near-infrared observations, and obtained a period length of P(pres) = 2022.7 +/- 1.3 d. Spectroscopic data collected during the last 60 yr yield an average period of P(avg) = 2020 +/- 4 d, consistent with the present-day period. The period cannot have changed by more than Delta P/P = 0.0007 since 1948. This confirms the previous claims of a true, stable periodicity, and gives strong support to the binary scenario. We have used the disappearance of the narrow component of He I 6678 to define the epoch of the Cycle 11 minimum, T(0) = JD 245 2819.8. The next event is predicted to occur on 2009 January 11 (+/- 2 d). The dates for the start of the minimum in other spectral features and broad-bands are very close to this date, and have well-determined time-delays from the He I epoch.
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We show that the significantly different effective temperatures (T(eff)) achieved by the luminous blue variable AG Carinae during the consecutive visual minima of 1985-1990 (T(eff) similar or equal to 22,800 K) and 2000-2001 (T(eff) similar or equal to 17,000 K) place the star on different sides of the bistability limit, which occurs in line-driven stellar winds around T(eff) similar to 21,000 K. Decisive evidence is provided by huge changes in the optical depth of the Lyman continuum in the inner wind as T(eff) changes during the S Dor cycle. These changes cause different Fe ionization structures in the inner wind. The bistability mechanism is also related to the different wind parameters during visual minima: the wind terminal velocity was 2-3 times higher and the mass-loss rate roughly two times smaller in 1985-1990 than in 2000-2003. We obtain a projected rotational velocity of 220 +/- 50 km s(-1) during 1985-1990 which, combined with the high luminosity (L(star) = 1.5 x 10(6) L(circle dot)), puts AG Car extremely close to the Eddington limit modified by rotation (Omega Gamma limit): for an inclination angle of 90 degrees, Gamma(Omega) greater than or similar to 1.0 for M(circle dot) less than or similar to 60. Based on evolutionary models and mass budget, we obtain an initial mass of similar to 100 M(circle dot) and a current mass of similar to 60-70 M(circle dot) for AG Car. Therefore, AG Car is close to, if not at, the Omega Gamma limit during visual minimum. Assuming M = 70 M(circle dot), we find that Gamma(Omega) decreases from 0.93 to 0.72 as AG Car expands toward visual maximum, suggesting that the star is not above the Eddington limit during maximum phases.
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Coordenao de Aperfeioamento de Pessoal de Nvel Superior (CAPES)
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O trabalho teve como objetivo comparar a eficincia produtiva e reprodutiva de ovelhas em dois sistemas de alimentao. Noventa e oito matrizes da raa Santa Ins e trinta e nove mestias Suffolk (3/4 Suffolk + 1/4 Santa Ins) foram divididas em dois tratamentos: tratamento 1 (T1) - mantidas em pastagem, com suplementao de silagem de capim elefante na seca invernal, e tratamento 2 (T2) -mantidas em pastagem, com suplementao de silagem de capim elefante na seca invernal e de concentrado trs semanas antes e durante a estao de monta, trs semanas antes do parto e durante a lactao. Verificou-se diferena (P<0,05) entre peso inicial (PI) (52,5kg e 54,33kg), e peso final (PF) (53,38kg e 55,76kg) para T1 e T2, respectivamente. Houve efeito de gentipo (P<0,05), sendo PI 51,46 kg para a raa Santa Ins (SI) e 55,38kg para as mestias Santa Ins-Suffolk (SF). Para PF, observou-se 52,36kg para a Santa Ins e 56,78kg na mestia Santa Ins-Suffolk. O peso pr-parto (PPP) diferiu (P<0,05) apenas entre as estaes, tendo sido de 65,23kg na estao reprodutiva I (2 a 4/2002), 58,15kg na estao reprodutiva II (10 a 12/2002) e 59,73kg na estao reprodutiva III (6 a 8/2003). No peso ps-parto (PPART), tambm ocorreram diferenas (P<0,05) entre a raa Santa Ins (53,59kg) e a mestia Santa Ins-Suffolk (57,05kg); no peso aos 30 dias de lactao (P30d) a Santa Ins registrou 52,94kg e a mestia Santa Ins-Suffolk 55,45kg. O peso aos 70 dias (P70d) de lactao foi para a Santa Ins de 50,83kg e de 53,22 kg para a mestia Santa Ins-Suffolk; e o peso aos 100dias (P100d) de lactao foi de 51,55kg e de 53,61kg para a Santa Ins e para a mestia Santa Ins-Suffolk, respectivamente. A condio corporal inicial (CCI) foi maior (P<0,05) para o T2 2,47 do que para o T1 2,16. Na condio corporal final (CCF), 2,19 e 2,6, respectivamente para T1 e T2, mas os tratamentos no diferiram na condio corporal pr-parto (CCPP). A CCI 2,4 para a mestia Santa Ins-Suffolk foi (P<0,05) em relao a Santa Ins 2,22. A CCF da mestia Santa Ins-Suffolk de 2,49 tambm foi maior (P<0,05) que da Santa Ins que obteve 2,3, mas no diferiram na CCPP. em relao as trs estaes reprodutivas, apenas na estao I a CCI 2,55, CCF 2,8 e a CCPP 3,03 foram maiores (P<0,05). J as estaes reprodutivas II= 2,47 e III= 2,1 diferiram somente na CCPP que foi menor na estao III. Na estao I e T1 ambos os gentipos obtiveram 72,5% de fertilidade e o T2 apresentou para as mestias Santa Ins-Suffolk 77% e para a Santa Ins 88%. Na estao II o T1 obteve para as mestias Santa Ins-Suffolk 42% e para as Santa Ins 38% e o T2 resultou em 56 e 50% para as mestias Santa Ins-Suffolk e Santa Ins respectivamente. Na estao III a fertilidade do T1 foi para as mestias 60% e para as Santa Ins 54% e o T2 87% e 76% para as mestias e Santa Ins respectivamente. Encontrou-se diferena na prolificidade, entre os tratamentos, sendo na estao I a prolificidade foi de 1,20 e 1,55, na estao II foi 0,90 e 1,03 e na estao III obteve-se 1,11 e 1,14, respectivamente para o T1 e T2. Concluiu-se que a suplementao melhorou o desempenho reprodutivo das ovelhas.
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JUSTIFICATIVA E OBJETIVOS: A dor ps-operatria continua sendo uma das principais complicaes ps-operatrias e motivo de desconforto, principalmente em crianas. O objetivo deste estudo foi avaliar o uso de analgsicos desde o trmino da cirurgia at a alta da sala de recuperao ps-anestsica (SRPA), como medida teraputica ou profiltica, para crianas com menos de 1 ano de idade. MTODO: Utilizando o banco de dados do Departamento de Anestesiologia, foi realizada anlise retrospectiva, envolvendo o perodo de janeiro de 2000 a abril de 2001, das anestesias de crianas menores que 1 ano de idade submetidas a procedimentos cirrgicos diversos, avaliando aspectos relacionados analgesia ps-operatria. RESULTADOS: No perodo do estudo, foram anestesiadas 402 crianas menores que 1 ano, sendo que 194 (48,2%) no receberam analgsicos e 208 (51,8%) receberam. Com relao ao uso ou no de analgsicos, foi observado o que se segue: Sem analgsicos: (1) Idade: at 1 ms, 68/99; entre 1 e 6 meses, 53/126; entre 6 meses e 1 ano, 73/177. (2) Peso: 6,7 3,1 kg (3). Sexo: masculino, 106/240; feminino, 88/162. (4) Estado fsico ASA: ASA I, 69/187; ASA II, 56/113; ASA III, 46/79; ASA IV, 23/23. (5) Anestesia peridural sacral: 3/4. (6) Tempo de anestesia: 106 32 minutos. (7) Encaminhamento para unidade de terapia intensiva (UTI): 93/119. Uso de analgsicos: (1) Idade: at 1 ms, 31/99; entre 1 e 6 meses, 73/126; entre 6 meses e 1 ano, 104/177. (2) Peso: 9 2,3 kg. (3) Sexo: masculino, 134/240; feminino, 74/162. (4) Estado fsico ASA: ASA I, 118/187; ASA II, 57/113; ASA III, 33/79; ASA IV, 0/23. (5) Anestesia peridural sacral: 1/4. (6) Tempo de anestesia: 130 38 minutos. (7) Encaminhamento para UTI: 26/119. Os frmacos empregados para promover analgesia foram: dipirona (60,6%), dipirona + tramadol (25,5%), dipirona + nalbufina (5,3%), tramadol (3,8%), nalbufina (3,8%), meperidina (0,5%) e fentanil (0,5%). CONCLUSES: Utilizar analgsicos em crianas desde o trmino da cirurgia at a alta da SRPA no foi habitual, principalmente nas crianas menores e mais graves e em procedimentos cirrgicos mais rpidos. O uso de dipirona, isoladamente, ou a associao dipirona/tramadol, foram as drogas analgsicas mais freqentemente empregadas.
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Includes bibliography
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Coordenao de Aperfeioamento de Pessoal de Nvel Superior (CAPES)
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Esta dissertao versa sobre o papel da Ouvidoria no Hospital Ophir Loyola a partir das informaes contidas nas manifestaes dos usurios do servio. Trata-se de uma pesquisa retrospectiva, realizada entre os anos de 2008 a 2010, de cunho exploratrio-descritivo, baseada na anlise de documentos oriundos do servio. Tem por objetivo geral analisar em que medida a Ouvidoria cumpriu as suas atribuies quanto s manifestaes dos usurios do HOL. Visa tambm identificar quais as principais manifestaes de insatisfao apontadas pelos usurios da ouvidoria que prejudicam a dinmica do atendimento, e, ainda, verificar como a gesto do HOL responde as manifestaes dos usurios da ouvidoria, no sentido de atender individual ou coletivamente as suas necessidades. O instrumento utilizado foi um roteiro de coleta de dados, inspirado em um modelo desenvolvido por Falco (2010) em pesquisa semelhante, dentro da seguinte composio: manifestaes relacionadas esfera da gesto hospitalar e manifestaes relacionadas esfera da gesto do Sistema nico de Sade (SUS). Dentro da esfera da gesto hospitalar, as manifestaes foram assim distribudas: denncia, reclamao, solicitao, informao, elogio e sugesto, para cada um dos eixos de composio. Para a esfera da gesto do SUS, foram adotadas apenas: a reclamao, a solicitao e a informao, devido no terem tido ocorrncias nas demais categorias. A amostra selecionada foi de 398 registros do servio de ouvidoria. Contudo, no decorrer da pesquisa identificou-se que um registro gerava manifestao nas duas esferas de gesto, hospitalar e do SUS, o que gerou um acrscimo de 46 ocorrncias, passando para 444, destas 81% contempla a esfera da gesto hospitalar e apenas 19%, a gesto do SUS. Quanto aos resultados, o estudo constatou que 50% das manifestaes no foram atendidas no seu pleito, dessas, 8% esto relacionadas s no respondidas e 42% refere-se s respostas no satisfatrias, no entanto, esse dado chama ateno para o fato de a ouvidoria dar respostas, mesmo que no alcance o pleito desejado, principalmente quando este se relaciona gesto do SUS, pela ingerncia da gesto nesse processo. Com relao aos 50% restantes, 188 equivalem s respostas satisfatrias do pleito, destes 94% contemplam a solues individuais e somente 6% (11 manifestaes), alcanaram a coletividade, e apenas duas destas provocaram mudana de ordem gerencial. Desta forma, conclui-se que a ouvidoria do HOL no conseguiu cumprir as sua atribuies institucionais devido ao comportamento da gesto frente s informaes geradas no servio de ouvidoria mostrar-se pontual, com resolues individuais e no voltado para a coletividade, no sentido de realinhar os entraves que prejudicam o desenvolvimento da assistncia, sinalizados pelo usurio e promover a aprendizagem. Nesse sentido, o objetivo geral de analisar em que medida a Ouvidoria cumpriu as suas atribuies quanto s manifestaes dos usurios do HOL foi alcanado.
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Ps-graduao em Zootecnia - FCAV
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Aims. Our goal is to study the circumstellar environment associated with each component of the wide intermediate-mass pre-main sequence binary system PDS 144 using broadband polarimetry. Methods. We present near-infrared (NIR) linear polarimetric observations of PDS 144 gathered with the IAGPOL imaging polarimeter along with the CamIV infrared camera at the Observatorio do Pico dos Dias (OPD). In addition, we re-analyzed OPD archive optical polarization to separate the binary and estimate the interstellar polarization using foreground stars. Results. After discounting the interstellar component, we found that both stars of the binary system are intrinsically polarized. The polarization vectors at optical and NIR bands of both components are aligned with the local magnetic field and the jet axis. These findings indicate an interplay between the interstellar magnetic field and the formation of the binary system. We also found that the PDS 144N is less polarized than its southern companion in the optical. However, in the NIR PDS 144N is more polarized. Our polarization data can only be explained by high inclinations (i greater than or similar to 80 degrees) for the disks of both members. In particular, comparisons of our NIR data with young stellar objects disk models suggest predominantly small grains in the circumstellar environment of PDS 144N. In spite of the different grain types in each component, the infrared spectral indexes indicate a coeval system. We also found evidence of coplanarity between the disks.
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The periodic spectroscopic events in eta Carinae are now well established and occur near the periastron passage of two massive stars in a very eccentric orbit. Several mechanisms have been proposed to explain the variations of different spectral features, such as an eclipse by the wind-wind collision (WWC) boundary, a shell ejection from the primary star or accretion of its wind onto the secondary. All of them have problems explaining all the observed phenomena. To better understand the nature of the cyclic events, we performed a dense monitoring of eta Carinae with five Southern telescopes during the 2009 low-excitation event, resulting in a set of data of unprecedented quality and sampling. The intrinsic luminosity of the He II lambda 4686 emission line (L similar to 310 L-circle dot) just before periastron reveals the presence of a very luminous transient source of extreme UV radiation emitted in the WWC region. Clumps in the primary's wind probably explain the flare-like behavior of both the X-ray and He II lambda 4686 light curves. After a short-lived minimum, He II lambda 4686 emission rises again to a new maximum, when X-rays are still absent or very weak. We interpret this as a collapse of the WWC onto the "surface" of the secondary star, switching off the hard X-ray source and diminishing the WWC shock cone. The recovery from this state is controlled by the momentum balance between the secondary's wind and the clumps in the primary's wind.
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Be stars possess gaseous circumstellar decretion disks, which are well described using standard alpha-disk theory. The Be star 28 CMa recently underwent a long outburst followed by a long period of quiescence, during which the disk dissipated. Here we present the first time-dependent models of the dissipation of a viscous decretion disk. By modeling the rate of decline of the V-band excess, we determine that the viscosity parameter alpha = 1.0 +/- 0.2, corresponding to a mass injection rate (M) over dot = (3.5 +/- 1.3) x 10(-8) M-circle dot yr(-1). Such a large value of a suggests that the origin of the turbulent viscosity is an instability in the disk whose growth is limited by shock dissipation. The mass injection rate is more than an order of magnitude larger than the wind mass-loss rate inferred from UV observations, implying that the mass injection mechanism most likely is not the stellar wind, but some other mechanism.