Development of lithium disilicate based glass-ceramics

O principal objectivo deste estudo foi o desenvolvimento de vitrocerâmicos à base de dissilicato de lítio no sistema Li2O-K2O-Al2O3-SiO2 contendo uma razão molar SiO2/Li2O muito afastada da do dissilicato de lítio (Li2Si2O5) usando composições simples e a técnica tradicional de fusão-vazamento de vidro de forma a obter materiais com propriedades mecânicas, térmicas, químicas e eléctricas superiores que permitam a utilização destes materiais em diversas aplicações funcionais. Investigou-se o fenómeno de separação de fases, a cristalização e as relações estrutura-propriedades de vidros nos sistemas Li2O-SiO2, Li2O-Al2O3-SiO2 e Li2O-K2O-Al2O3-SiO2. Os vidros nos sistemas Li2O-SiO2 e Li2O-Al2O3-SiO2 apresentaram fraca densificação e resultaram em materiais frágeis, contrastando com a boa sinterização dos vidros no sistema Li2O-K2O-Al2O3-SiO2. Pequenas adições de Al2O3 e K2O ao sistema Li2O-SiO2 permitiram controlar a separação de fases devido à formação de espécies de Al(IV) que confirmaram o papel de Al2O3 como formador de rede. Os compactos de pó de vidro das composições contendo Al2O3 e K2O tratados termicamente resultaram em vitrocerâmicos bem densificados, apresentando dissilicato de lítio como a principal fase cristalina, e valores de resistência mecânica à flexão, resistência química e condutividade eléctrica (173-224 MPa, 25-50 mg/cm2 e ~2´10-18 S/cm, respectivamente) que possibilitam a utilização destes materiais em diversas aplicações funcionais. A adição de P2O5, TiO2 e ZrO2 ao sistema Li2O-K2O-Al2O3-SiO2 como agentes nucleantes revelou que os vidros contendo apresentaram cristalização em volume, com a formação de metassilicato de lítio a temperaturas mais baixas e dissilicato de lítio para as temperaturas mais elevadas, enquanto a adição de zircónia reduz o grau de segregação, aumenta a polimerização da matriz vítrea e desloca o valor de Tg para temperaturas superiores, inibindo a cristalização.

Efeito da temperatura de secagem de dois tipos de silano e da supressão ou redução do tempo de condicionamento com ácido hidrofluorídrico na resistência de união entre uma cerâmica de dissilicato de lítio e um cimento resinoso

Este estudo avaliou o efeito de diferentes métodos de silanização e aplicação do ácido hidrofluorídrico (HF) sobre a resistência à microtração de uma cerâmica de dissilicato de lítio a um cimento resinoso. Quarenta blocos de IPS e.max Press /Ivoclar Vivadent (5x5x6mm) foram cimentados a blocos de resina Z250/3M ESPE (5x5x6mm) usando o cimento resinoso RelyX ARC/3M ESPE de acordo com os seguintes métodos de tratamento superficial: G1: 20s de ácido fluorídrico (HF) + silano não hidrolisado Primer-Activactor/Dentsply (SNH) seco à temperatura ambiente; G2: 20s HF + silano pré-hidrolisado RelyX Ceramic-Primer/3M ESPE (SPH) seco à temperatura ambiente; G3: 10s HF + SNH seco com ar quente (50oC-2min); G4: 10sHF + SPH seco com ar quente (50oC-2min); G5: sem ácido, SNH seco com ar quente (50oC-2min); G6: sem ácido, SPH seco com ar quente (50oC-2min); G7: sem ácido, SNH seco à temperatura ambiente; G8: sem ácido, SPH seco à temperatura ambiente. Antes de cada método de silanização, os blocos cerâmicos receberam acabamento com lixas de carbeto de silício (220-600) e limpeza com ácido fosfórico 37% (1min). A cimentação foi realizada com carga vertical de 1kg por 10min. Os conjuntos de cerâmica/cimento/resina foram armazenados em água destilada (37C) por 24 horas e depois seccionados em máquina de corte Isomet 1000 a fim de obter palitos (n = 40) de 1mm2 de área da seção transversal, que foram submetidos ao teste de microtração em máquina de ensaio universal Emic (v = 0,5mm/min). O modo de fratura foi avaliado em microscópio eletrônico de varredura. A análise estatística foi realizada utilizando ANOVA / Dunnett (p-valor = 0,000). As médias MPa e desvio padrão foram: G1-21,5 (8,9) BC; G2-30,5 (7,2) A; G3-19.4 (9.1) BC; G4-24,0 (9,0) B; G5-8.1 (3.2) D; G6 -18,0 (6,2) C; G7-7.8 (2,6) D; G8-6.3 (2,5) D. Grupos 2, 3, 4 e 6 não tiveram falhas prematuras dos palitos contra os grupos 1, 5, 7 e 8, que apresentaram 2,2; 44,4; 75,6 e 33,3% de perdas prematuras, respectivamente. O teste de correlação foi realizado apresentando significância estatística, com valor de -0,736 (p-valor = 0,000), mostrando que, a medida que o percentual de perda prematura aumenta, a média da MPa diminui. Quanto ao modo de fratura, observou-se 44,97% de falhas do tipo mista, 51,70% de falhas do tipo adesiva, 3,33% de falhas do tipo coesiva do cimento. Quando é realizada a supressão do condicionamento com HF como pré-tratamento da superfície cerâmica IPS e.max Press, a aplicação de silano SPH, associada ao seu tratamento térmico, deve ser o método de silanização recomendado, embora os valores mais elevados de resistência de união tenham sido os obtidos quando utilizado o condicionamento com HF por 20s. Quando é realizada a redução do tempo de condicionamento com HF para 10s, a aplicação do silano (SPH ou SNH) deve ser sempre associada ao seu tratamento térmico. O SNH só deve ser usado se as superfícies das cerâmicas IPS e.max Press forem tratadas com HF.

Síntesis y caracterización de nuevos silicatos complejos [por] Blanca Nájera Martínez

Tesis (Maestría en Ciencias, con especialidad en Química Analítica) U.A.N.L.

Estudo da perda de energia e da flutuação estatística da perda de energia de íons de lítio em direções aleatórias do silício

Usando a técnica de Retroespalhamento Rutherford (RBS). no presente trabalho medimos a perda de energia e a flutuação estatística da perda de energia (straggling) como função da energia para íons de Li em alvos de silicio amorfo. Através do método dos marcadores. com amostras produzidas por implantação iônica e por epitaxia de feixe molecular,o poder de freamento foi medido em um intervalo de energia entre 250keV e 9MeV enquanto que o straggling foi determinado em um intervalo que foi de 450keV a 3MeV. Os resultados experimentais foram comparados com medidas prévias e com cálculos semi-empiricos realizados por Ziegler. Biersack e Littmark e por Konac et el., sendo encontrado um razoável acordo teórico-experimental. Foram também realizados cálculos baseados nos modelos teóricos de Aproximação por Convolução Perturbativa (PCA) e Aproximação por Convolução Unitária (UCA) propostos por Grande e Schiwielz O modelo PCA apresentou resultados aceitáveis para energias acima de 6MeV enquanto que os valores apresentados pelo divergem dos valores experimentais para energias abaixo de 2MeV. As medidas de straggling quando comparados com as predições da teoria de Bohr mostraram discrepâncias que foram entre 20% e 60%. Cálculos feitos com a aproximação para encontros binários (BEA) usando-se a secção de choque de Thompsom e a secção de choque proposta no trabalho de Vriens foram comparados com as medidas experimentais. Os resultados usando-se a secção de choque de Thompsom divergem por até 50%, enquanto que os valores calculados a secção de choque proposta por Vriens mostram uma concordância razoável para energias abaixo de 1MeV.

Alterações na via intracelular do fosfoinositol : implicações para a fisiopatologia do transtorno bipolar e mecanismo de ação do lítio

Uma possível disfunção nos processos intracelulares de transdução de sinais pode estar implicada na fisiopatologia do transtorno bipolar (Soares and Mallinger 2000). Particularmente, a via intracelular do fosfoinositol (PI) pode ser um sitio de disfunção (Soares et al 1997b). Plaquetas, células periféricas, e amostras de cérebro pós-mortem têm sido utilizados como modelos em estudos prévios com o objetivo de investigar esta hipótese. Os achados que emergem destes estudos são consistentes com a hipótese de uma hiperatividade na via do PI na fase maníaca, que pode estar relacionada com a fase do transtorno. Nesta tese de doutoramento está descrita uma série de estudos preliminares que utilizaram um modelo plaquetário para estudar alterações da via do PI em pacientes com transtorno afetivo bipolar, e também em relação ao mecanismo de ação do carbonato de lítio. Utilizando um método para quantificação de fosfoinositois em membrana plaquetária desenvolvido pelo Professor Alan Mallinger e colaboradores na Universidade de Pittsburgh, o passo inicial envolveu o estudo da reprodutibilidade teste/reteste do mesmo, que foi documentada como estando dentro de limites aceitáveis (Soares et al 1999a). Subseqüentemente, conduzimos um estudo preliminar em pacientes bipolares já tratados com monoterapia com o lítio (Soares et al 1999b). Nestes pacientes, alem de estudarmos os níveis de fosfolipídios de membrana comparados com voluntários normais, também estudamos, em colaboração com o Professor Husseini Manji e colaboradores do National Institute of Mental Health (NIMH), EUA, os níveis de subespécies especificas de PKC em plaquetas de pacientes bipolares (Soares et al 2000a). Nossos achados principais destes estudos colaborativos sugerem uma redução dos níveis plaquetários de PIP2, concomitantemente com redução seletiva de subespécies especificas de PKC. Como um passo adicional, também estudamos os níveis de fosfoinositois de membrana em indivíduos bipolares na fase depressiva, quando não medicados, que estavam significativamente elevados comparados com voluntários normais (Soares et al 2001). Por último, conduzimos um ensaio clinico aberto com carbonato de lítio em doses terapêuticas em um grupo pequeno de pacientes bipolares, que sugeriu uma diminuição significativa dos níveis de PIP2 após o tratamento (Soares et al 2000b). Estes estudos documentam uma disfunção na via do PI em plaquetas de pacientes bipolares, possivelmente modulada pelo tratamento com o lítio, sugerindo o envolvimento desta via na fisiopatologia do transtorno e no mecanismo de ação do lítio. não se sabe se tais alterações plaquetárias refletem o que se passa nesta via em neurônios humanos in vivo, o que constitui uma limitação importante, em potencial, desta abordagem. No entanto, na falta de metodologia de neuroimagem que permita o estudo destas vias no cérebro de pacientes vivos, o modelo periférico plaquetário é de valia para se começar a fazer inferências sobre o funcionamento desta via em pacientes bipolares. Estudos futuros com amostras maiores de pacientes que possam segui-los em fases diferentes do transtorno e tentar determinar correlações entre alterações nesta via produzidas pelo lítio e os efeitos terapêuticos desta medicação serão de grande valia.

A evolução do lítio em estrelas do tipo-solar através do diagrama HR

Important advances have been made along the last decade in the study of the lithium behavior in solar-type stars. Among the most important discoveries what attracts attention is that the distribution of lithium abundance in the late F-type giant stars tends to be discontinuous, at the same time of a sudden decline in rotation and a gradual decline according to the temperature for giant red stars of such spectral type. Other studies have also shown that synchronized binary systems with evolved components seem to keep more of their original lithium than the unsynchronized systems. evertheless, the connection between rotation and lithium abundance as well as the role of tidal effects on lithium dilution seem to be more complicated matters, depending on mass, metallicity and age. This work brings an unprecedented study about the behavior of lithium abundance in solartype evolved stars based on an unique sample of 1067 subgiant, giant and supergiant stars, 236 of them presenting spectroscopic binary characteristics, with precise lithium abundance and projected rotational speed. Now the lithium-rotation connection for single and binary evolved stars is analyzed taking into account the role of mass and stellar age

Sobre a relação entre rotação, atividade crosmosférica e abundância de lítio em estrelas subgigantes

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior

Lítio e parâmetros orbitais em sistemas binários com componentes evoluídas

One of the best established properties of the single late type evolved stars is that their rotational velocity and lithium content decrease with effective temperature and age. Nevertheless, the root cause of this property, as well as the link between rotation and lithium abundance and, in particular, the effects of binarity on rotation and lithium content in binary systems with evolved component, are not yet completely established. How does the gravitational tides, in binary systems, affects rotational evolution and lithium dilution? Trying to answer these questions, we have carried out an observational survey, in the lithium region centered at the lithium I line A6707.81A, for a large sample of about 100 binary systems with evolved component along the spectral range F, G and K, with the CES spectrometer mounted at the CAT 1.44 m Telescope of the ESO, La Silla, Chile. By combining the abundances of lithium issued from these observations with rotational velocity and orbital parameters, we have found a number of important results. First of all, we confirm that in this class of binary systems rotation is effectively affected by tidal effects. Binary systems with orbital period lower than about 100 days and circular or nearly circular orbits, present rotational velocity enhanced in relation to the single giant stars and to the binary systems with an orbital period larger than 100 days. This is clearly the result of the synchonization between the rotational and orbital motions due to tidal effects. In addition, we have found that lithium abundances in binary systems with giant components present the same gradual decreasing with effective temperature, observed in the single giants of same luminosity class and spectral types. We have found no lithium-rich binary systems, in contrast with single giants. A remarkable result from the present study is the one showing that synchronized binary systems with giant component retains more of their original lithium than the unsynchronized systems. In fact, we have found a possible "inhibited zone", in which synchronized binary systems with giant component having lithium abundance lower than a threshold level should be unusual. Finally, the present study also shows that the binary systems with giant component presenting the highest lithium contents are those with the highest rotation rates

Um estudo da abundância de lítio, rotação, atividade cromosférica e magnetismo das estrelas análogas e gêmeas solares

The study physical process that control the stellar evolution is strength influenced by several stellar parameters, like as rotational velocity, convective envelope mass deepening, and magnetic field intensity. In this study we analyzed the interconnection of some stellar parameters, as Lithium abundance A(Li), chromospheric activity and magnetic field intensity as well as the variation of these parameters as a function of age, rotational velocity, and the convective envelope mass deepening for a selected sample of solar analogs and twins stars. In particular, we analyzed the convective envelope mass deepening and the dispersion of lithium abundance for these stars. We also studied the evolution of rotation in subgiants stars, because its belong to the following evolutionary stage of solar analogs, and twins stars. For this analyze, we compute evolutionary models with the TGEC code to derive the evolutionary stage, as well as the convective envelope mass deepening, and derive more precisely the stellar mass, and age for this 118 stars. Our Investigation shows a considerable dispersion of lithium abundance for the solar analogs stars. We also realize that this dispersion is not by the convective zone deep, in this way we observed which the scattering of A(Li) can not be explained by classical theories of mixing in the convective zone. In conclusion we have that are necessary extra-mixing process to explain this decrease of Lithium abundance in solar analogs and twins stars. We analyzed the subgiant stars because this are the subsequent evolutionary stage after the solar analogs and twins stars. For this analysis, we compute the rotational period for 30 subgiants stars observed by Co- RoT satellite. For this task we apply two different methods: Lomb-Scargle algorithm, and the Plavchan Periodogram. We apply the TGEC code we compute models with internal distribution of angular momentum to confront the predict results with the models, and the observational results. With this analyze, we showed which solid body rotation models are incompatible with the physical interpretation of observational results. As a result of our study we still concluded that the magnetic field, convective envelope mass deepening, and internal redistribution of angular momentum are essential to explain the evolution of low-mass stars, and its observational characteristics. Based on population synthesis simulation, we concluded that the solar neighborhood presents a considerable quantity of solar twins when compared with the discovered set nowadays. Altogether we foresee the existence around 400 solar analogs in the solar neighborhood (distance of 100 pc). We also study the angular momentum of solar analogs and twins, in this study we concluded that added angular momentum from a Jupiter type planet, putted in the Jupiter position, is not enough to explain the angular momentum predicted by Kraft law (Kraft 1970)

Evolução da atividade cromosférica, abundância de lítio e rotação das estrelas análogas e gêmeas solares

The study of solar-type stars also includes the familiar solar analogs and twins. These objects have been one of the major research subjects in astrophysics nowadays. A direct comparison of solar activity with chromospheric activity indices for a set of stars very similar to the Sun (twins and analogs) provides an excellent opportunity to study the evolution of stellar activity on timescales of the order of the lifetime on the main sequence. This work deals with the relationship between the abundance of lithium, chromospheric activity, X-ray emission and rotation period in terms of stellar ages. We explore the influence of stellar evolution in the global properties of the stars and the aspects linked to its coronal, chromospheric and magnetic activity. Our main objective is to probe the law of decay of each of these parameters based on a sample of stars classified as well-connected as analogs stars and solar twins.

O enigmático problema das gigantes ricas em Lítio e as perspectivas com o satélite Kepler

Lithium (Li) is a chemical element with atomic number 3 and it is among the lightest known elements in the universe. In general, the Lithium is found in the nature under the form of two stable isotopes, the 6Li and 7Li. This last one is the most dominant and responds for about 93% of the Li found in the Universe. Due to its fragileness this element is largely used in the astrophysics, especially in what refers to the understanding of the physical process that has occurred since the Big Bang going through the evolution of the galaxies and stars. In the primordial nucleosynthesis in the Big Bang moment (BBN), the theoretical calculation forecasts a Li production along with all the light elements such as Deuterium and Beryllium. To the Li the BNB theory reviews a primordial abundance of Log log ǫ(Li) =2.72 dex in a logarithmic scale related to the H. The abundance of Li found on the poor metal stars, or pop II stars type, is called as being the abundance of Li primordial and is the measure as being log ǫ(Li) =2.27 dex. In the ISM (Interstellar medium), that reflects the current value, the abundance of Lithium is log ǫ(Li) = 3.2 dex. This value has great importance for our comprehension on the chemical evolution of the galaxy. The process responsible for the increasing of the primordial value present in the Li is not clearly understood until nowadays. In fact there is a real contribution of Li from the giant stars of little mass and this contribution needs to be well streamed if we want to understand our galaxy. The main objection in this logical sequence is the appearing of some giant stars with little mass of G and K spectral types which atmosphere is highly enriched with Li. Such elevated values are exactly the opposite of what could happen with the typical abundance of giant low mass stars, where convective envelops pass through a mass deepening in which all the Li should be diluted and present abundances around log ǫ(Li) ∼1.4 dex following the model of stellar evolution. In the Literature three suggestions are found that try to reconcile the values of the abundance of Li theoretical and observed in these rich in Li giants, but any of them bring conclusive answers. In the present work, we propose a qualitative study of the evolutionary state of the rich in Li stars in the literature along with the recent discovery of the first star rich in Li observed by the Kepler Satellite. The main objective of this work is to promote a solid discussion about the evolutionary state based on the characteristic obtained from the seismic analysis of the object observed by Kepler. We used evolutionary traces and simulation done with the population synthesis code TRILEGAL intending to evaluate as precisely as possible the evolutionary state of the internal structure of these groups of stars. The results indicate a very short characteristic time when compared to the evolutionary scale related to the enrichment of these stars

Sobre a relação entre rotação, atividade crosmosférica e abundância de lítio em estrelas subgigantes

The connection between rotation, CaII emission flux and lithium abundance is analyzed for a sample of subgiant stars, with evolutionary status was determined from the Toulouse-Geneve code and HlPPARCOS trigonometric parallax measurements. We noted that the distribution of rotation and CaII emission flux, as a function of effective temperature, shows a discontinuity located around the same spectral type, F8IV. Stars located blueward of this spectral type, exhibit a large spread of values of rotation and CaII flux, whereas stars redward of F8lV show essentially low ratation anel low CaII flux. The strength of these declines nevertheless, depends on stellar mass. The distribution of lithium abundances also shows a discontinuity, however with behavior a little more complex for subgiants with mass lower than about 1.2 Solar Masses, this decrease is observed later than that in rotation and CaII flux, whereas for masses higher than 1.2 Solar Masses the decrease in lithium abundance is located around the spectral type F8IV. The discrepancy between the location of the discontinuities of rotation and CaII flux and log n(Li) for stars with masses lower than 102 Solar Masses, seems to reflect the sensitivity of these phenomena to the mass of the convective envelope. The drop in rotation, which results mostly from a magnetic braking, requires an increase in the mass of the convective envelope less than that required for the decrease in lithium abundance The location of the discontinuity in log n( Li) in the same region of the discontinuity ties in rotation and CaII flux, for stars with masses higher than 1.2 Solar Masses, may also be explained by the behavior of the deepening of the convective envelope. In contrast to the relationship between rotation and CaII flux the relationship between lithium abundance and rotation shows no dear tendency toward linear behavior. Similarly, the same tendency is observed in the relationship between lithium abundance and CaII flux in spite of these facts, subgiants with high lithium content also have high rotation and high CaII emission flux. We also observed that stars with high lithium content present, in its majority, an undeveloped convective envelope, whereas stars with low lithium content have a developed convective envelope. In the case of the rotation, stars with undeveloped convective envelope, show rotational velocities as much high as low, whereas stars with developed convective envelope only present low rotation

Efeitos do tratamento com lítio na memória aversiva, comportamentos relacionados à ansiedade e depressão e na expressão de BDNF em ratos

Lithium (Li) is the first choice to treat bipolar disorder, a psychiatric illness characterized by mood oscillations between mania and depression. However, studies have demonstrated that this drug might influence mnemonic process due to its neuroprotector, antiapoptotic and neurogenic effects. The use of Li in the treatment of cognitive deficits caused by brain injury or neurodegenerative disorders have been widely studied, and this drug shows to be effective in preventing or even alleviating the memory impairment. The effects of Li on anxiety and depression are controversial and the relationship of the effects of lithium on memory, anxiety and depression remain unknown. In this context, this study aims to: evaluate the effects of acute and chronic administration of lithium carbonate in aversive memory and anxiety, simultaneously, using the plus maze discriminative avoidance task (PMDAT); test the antidepressant effect of the drug through the forced swimming test (FS) and analyze brainderived neurotrophic factor (BDNF) expression in structures related to memory and emotion. To evaluation of the acute effects, male Wistar rats were submitted to i.p. administration of lithium carbonate (50, 100 or 200 mg/kg) one hour before the training session (PMDAT) or lithium carbonate (50 or 100 mg/kg) one hour before the test session (FS). To evaluation of the chronic effects, the doses administered were 50 or 100 mg/kg or vehicle once a day for 21 days before the beginning of behavioral tasks (PMDAT and FS). Afterwards, the animals were euthanized and their brains removed and submitted to immunohistochemistry procedure to quantify BDNF. The animals that received acute treatment with 100 and 200 mg/kg of Li did not discriminated between the enclosed arms (aversive and non-aversive) in the training session of PMDAT, showing that these animal did not learned the task. This lack of discrimination was also observed in the test session, showing that the animals did not recall the aversive task. We also observed an increased exploration of the open arms of these same groups, indicating an anxiolytic effect. The same groups showed a reduction of locomotor activity, however, this effect does not seem to be related with the anxiolytic effect of the drug. Chronic treatment with Li did not promote alterations on learning or memory processes. Nevertheless, we observed a reduction of open arms exploration by animals treated with 50 mg/kg when compared to the other groups, showing an anxiogenic effect caused by this dose. This effect it is not related to locomotor alterations since there were no alterations in these parameters. Both acute and chronic treatment were ineffective in the FS. Chronic treatment with lithium was not able to modify BDNF expression in hippocampus, amygdala and pre-frontal cortex. These results suggest that acute administration of lithium promote impairments on learning in an aversive task, blocking the occurrence of memory consolidation and retrieval. The reduction of anxiety following acute treatment may have prevented the learning of the aversive task, as it has been found that optimum levels of anxiety are necessary for the occurrence of learning with emotional context. With continued, treatment the animals recover the ability to learn and recall the task. Indeed, they do not show differences in relation to control group, and the lack of alterations on BDNF expression corroborates this result. Possibly, the regimen of treatment used was not able to promote cognitive improvement. Li showed acute anxiolytic effect, however chronic administration 4 promoted the opposite effect. More studies are necessary to clarify the potential beneficial effect of Li on aversive memory

Lítio e rotação nas estrelas análogas solares: análise teórica das observações

The projected rotational velocity together with lithium abundance and the onset of the dilution by the deepening in mass of the convective envelope provide a key tool to investigate the so far poorly understood processes at work in stellar interiors of solar-analog stars. To investigate the link between abundances, convection and rotational velocities in solar-analog G dwarf stars, we study a bona fide sample of 118 selected solar-analog G dwarf stars presenting measured lithium abundances, rotational velocities, and fundamental parameters together with computed evolutionary tracks (Toulouse-Geneva code) for a range of stellar masses around 1 M and metallicity consistent with the solar-analog range. The aim of this work is to build up an evolution of lithium and rotation as a function of stellar age, mass, effective temperature, and convection. We analyze the evolutionary status of the sample of 118 solar-analog G dwarf in the HR diagram based on Hipparcos data and using a grid of stellar models in the effective temperature and mass range of the solar-analog stars. We discuss the deepening (in mass) of the convective envelope and the influence on the Li abundances and projected rotational velocities. We determined the stellar mass and the mass of the convective envelope for a bona fide sample of 118 selected solar-analog G dwarf and checked the evolutionary link between the rotational velocity, lithium abundance, and the deepening of the convective envelope. Fast rotators (vsini 6 km s��1) are also stars with high Li content. Slow rotators present a wide range of values of log n(Li). Our results shed new light on the lithium and rotational behavior in G dwarf stars. We confirmed the presence of a large Li abundance spread among the solar-analog stars and concluded that the solar twins probably share a similar mixing history with the Sun

Análise espectroscópica da estrela HD 150050: uma nova estrela gigante rica em lítio

Conselho Nacional de Desenvolvimento Científico e Tecnológico