International Telemetering Conference Proceedings / October 20-23, 2003 / Riviera Hotel and Convention Center, Las Vegas, Nevada / It is widely recognized that telemetry channels, particularly airborne channels, are afflicted by multipath propagation effects. It has also been shown that adaptive equalization can be highly effective in mitigating these effects. However, numerous other factors influence the behavior of adaptive equalization, and the type of modulation employed is certainly one of these factors. This is particularly true on modulations that exhibit different operating bandwidths. Computer simulations using the Constant Modulus Algorithm (CMA) have recently been reported for PCM/FM, ARTM Tier 1 SOQPSK, and Tier II SOQPSK. These encouraging results have led to a hardware implementation of a CMA equalizer. This paper presents the latest results from this work.

We present distances and kinematics and look at the possible populations for the blue plume (BP) stars in the Canis Major Overdensity (CMa). We conducted a medium resolution spectral survey on the BP stars (N=303) in CMa (centered at l = 238° ; b = -8°) using the data from AAOmega Spectrograph. We used a modified version of the Statistics-sensitive Non-linear Iterative Peak-clipping (SNIP) algorithm to normalize our fluxed absorption spectra. After determining the radial velocities from measurements of strong absorption features for the stars we use a Bayesian analysis of spectral feature strengths and photometric colors to determine Teff, Logg and [Fe/H]. Our procedure makes use of grid for model synthetic spectra computed using SPECTRUM with Atlas9 model atmospheres and Kurucz model colors. We determine the absolute magnitude using the stellar parameters and BaSTI isochrones and compute distances and ages for the BP stars. Our analysis of the BP stars indicates Teff ranging from 6500K to 8000K, metallicity ranging from 0.0 to -1.0 with an average of -0.5. We found for this temperature range that the surface gravity of the stars could not be well constrained. From the spatial and kinematics results we found that most of the stars are thick disk stars with a small mixture of thin disk stars. The stars are most likely a mixture of thick disk blue stragglers and normal A-type stars preferentially seen to greater depths due to the low dust extinction in this location of the Galaxy.

Traditionally, lead-based bearing overlays dominate the commercial automotive market and it has been proven that an excellent combination of properties can be attained through their use. However, lead is a toxic metal and a cumulative poison in humans. According to the European Union End-of-Life Vehicle (ELV) Directive proposed in 1997, vehicles that registered in'all the member states after 1st July 2003 should contain no lead, mercury, cadmium and hexavalent chromium. In this study, a new sulphate-gluconate electrolyte was used to produce multilayer SnCo coatings, aimed at a lead-free overlay for future market use. Tin-cobalt compositionally modulated alloy (CMA) coatings produced from sulphategluconate electrolytes have been previously examined as a potential replacement for lead-free bearing overlays [1]. However, some obstacles may exist which limit their potential use on an industrial scale. For example, long electroplating times are required to produce a thick coating which is very undesirable from an industrial viewpoint, and also the possible elemental interdiffusion occurring in the coating system under engine operating temperatures could rapidly deteriorate the coating properties. In addition, there is an increasing demand from automotive industry to further improve bearing overlay properties, for example for high performance and high compression ratio engines.

Be stars are main-sequence stars and a specific subclass of B type stars with the unique characteristic of showing HI Balmer emission lines in their optical spectra that originates from a circumstellar disk around the star. Over the past 50 years, the Galactic Be star $\\omega$ CMa has exhibited quasi-regular outbursts, every 8 years or so, when the star brightens by about half a magnitude in the V-band. During these outbursts a new disk is formed during the first 3-4 years, and then dissipates in the following 4-6 years. We have access to a rich dataset (including photometry, polarimetry, interferometry and spectroscopy) of $\\omega$ CMa since March 1964 covering several outbursts and quiescence phases. Thus, nature has provided us the perfect experiment to study how Be star disks grow and dissipate. There is an increasing body of evidence that suggests that Be disks are well described by the Viscous Decretion Disk (VDD) model according to which the formation and structure of the disk depend on the kinematic viscosity of the gas. However, most observational tests of the VDD to-date were done for systems that do not display strong temporal variability. We use the rich dataset available for $\\omega$ CMa to perform the first in-depth test of the VDD scenario in a system with strong temporal variability. We use the radiative transfer code HDUST to analyze and interpret the observational dataset. From this analysis we (1) obtain a realistic physical model of the circumstellar environment; (2) measure the viscosity parameter of the gas, both during the formation and dissipation phases of the disk; (3) obtain a reliable estimate of the stellar mass and angular momentum loss rates during outburst. Our simulations offer a good description of the photometric variability, which suggests that the VDD model adequately describes the structural evolution of the disk. Furthermore, our analysis allowed us to determine the viscosity parameter $\\alpha$, as well as the net mass and angular momentum (AM) loss rates. We find that $\\alpha$ is variable, ranging from 0.1 to 1.0, not only from cycle to cycle but also within a given cycle. Additionally, build-up phases have larger values of $\\alpha$ than the dissipation phases. We also find that, contrary to what is generally assumed, during dissipation the outward AM flux is not necessarily zero, meaning that $\\omega$ CMa does not experience a true quiescence but, instead, switches between a high AM loss rate state to a low AM loss rate one during which the disk quickly assumes an overall lower density but never zero. We confront the average AM loss rate with predictions from stellar evolution models for fast-rotating stars, and find that our measurements are smaller by more than one order of magnitude. The model developed using the V-band photometry as a constraint was applied to several other observables. Overall, the results of this multi-technique study were very positive, with a good match for multi-band photometry, polarization, and most spectroscopic characteristics. This is a very relevant result, as it proves that a model that was constructed from constraints only from the very inner part of the disk (the $V$-band light curve), could be extended to the whole disk and to other physical processes. / Estrelas Be são um subtipo específico de estrelas de sequência principal de tipo espectral B. Elas possuem características únicas tais como a presença de linhas de emissão em seu espectro, que se originam de um disco circunstelar. Nos últimos 50 anos, a estrela Be galáctica CMa exibiu erupções quasi-regulares, a cada 8 anos aproximadamente, onde a estrela torna-se mais brilhante na banda V. Nestas erupções um novo disco se forma nos primeiros 3-4 anos e depois dissipa-se nos 4-6 anos seguintes. Temos acesso a uma base de dados rica (incluindo fotometria, polarimetria, interferometria e espectroscopia) de CMa desde março de 1964, que cobre vários ciclos de erupções e quiescências. Assim, a natureza nos proveu um experimento perfeito para estudar como discos de estrelas Be crescem e dissipam-se. Há um corpo de evidências cada vez maior que sugerem que os discos de estrela Be são bem descritos pelo modelo de decréscimo viscoso (VDD), segundo o qual a formação e estrutura do disco depende da viscosidade cinemática do gás. Entretanto, a maioria dos testes conduzidos com o VDD até o momento foram feitos para sistemas que não mostram forte variabilidade temporal. Usamos a rica base de dados de CMa para conduzir o primeiro teste aprofundado do VDD em um sistema fortemente variável. Usamos o código de transporte radiativo HDUST para analisar e interpretar os dados. Desta análise obtemos (1) um modelo fisicamente realista do ambiente circunstelar, (2) a viscosidade do gás, e (3) uma estimativa confiável das taxas de perda de massa e momento angular durante os eventos de formação do disco. Nossas simulações conseguem reproduzir a variabilidade fotométrica muito bem, o que sugere que o modelo VDD descreve corretamente a evolução estrutural do disco. Mostramos que o parâmetro de viscosidade é variável, com valores entre 0.1 e 1. Adicionalmente, as fases de construção do disco têm valores de viscosidade maior. Contrariamente ao que se acredita, mostramos que durante a dissipação a taxa de perda de momento angular não é necessariamente nula, o que implica que CMa não experimenta uma quiescência verdadeira, mas alterna entre uma fase de alta taxa de perda de momento angular (erupção) e uma fase de baixa taxa (quiescência). Confrontamos as taxas de perda de momento angular com as preditas pelos modelos evolutivos de Genebra, e encontramos que nossas taxas são mais que 10 vezes menores que as taxas de previstas pelos modelos. O modelo desenvolvido para reproduzir a curva de luz na banda V foi aplicado a vários outros observáveis. De forma geral, os resultados deste estudo multi-técnica foram muito positivos, com uma boa concordância com a fotometria multi-banda, polarização, e a maioria das características espectrais. Este é um resultado muito relevante, pois prova que um modelo que foi construído apenas a partir de vínculos para a interna do disco (a curva de luz na banda V), pode ser estendido para todo o disco e também outros processos físicos.

Be stars are main-sequence stars and a specific subclass of B type stars with the unique characteristic of showing HI Balmer emission lines in their optical spectra that originates from a circumstellar disk around the star. Over the past 50 years, the Galactic Be star $\\omega$ CMa has exhibited quasi-regular outbursts, every 8 years or so, when the star brightens by about half a magnitude in the V-band. During these outbursts a new disk is formed during the first 3-4 years, and then dissipates in the following 4-6 years. We have access to a rich dataset (including photometry, polarimetry, interferometry and spectroscopy) of $\\omega$ CMa since March 1964 covering several outbursts and quiescence phases. Thus, nature has provided us the perfect experiment to study how Be star disks grow and dissipate. There is an increasing body of evidence that suggests that Be disks are well described by the Viscous Decretion Disk (VDD) model according to which the formation and structure of the disk depend on the kinematic viscosity of the gas. However, most observational tests of the VDD to-date were done for systems that do not display strong temporal variability. We use the rich dataset available for $\\omega$ CMa to perform the first in-depth test of the VDD scenario in a system with strong temporal variability. We use the radiative transfer code HDUST to analyze and interpret the observational dataset. From this analysis we (1) obtain a realistic physical model of the circumstellar environment; (2) measure the viscosity parameter of the gas, both during the formation and dissipation phases of the disk; (3) obtain a reliable estimate of the stellar mass and angular momentum loss rates during outburst. Our simulations offer a good description of the photometric variability, which suggests that the VDD model adequately describes the structural evolution of the disk. Furthermore, our analysis allowed us to determine the viscosity parameter $\\alpha$, as well as the net mass and angular momentum (AM) loss rates. We find that $\\alpha$ is variable, ranging from 0.1 to 1.0, not only from cycle to cycle but also within a given cycle. Additionally, build-up phases have larger values of $\\alpha$ than the dissipation phases. We also find that, contrary to what is generally assumed, during dissipation the outward AM flux is not necessarily zero, meaning that $\\omega$ CMa does not experience a true quiescence but, instead, switches between a high AM loss rate state to a low AM loss rate one during which the disk quickly assumes an overall lower density but never zero. We confront the average AM loss rate with predictions from stellar evolution models for fast-rotating stars, and find that our measurements are smaller by more than one order of magnitude. The model developed using the V-band photometry as a constraint was applied to several other observables. Overall, the results of this multi-technique study were very positive, with a good match for multi-band photometry, polarization, and most spectroscopic characteristics. This is a very relevant result, as it proves that a model that was constructed from constraints only from the very inner part of the disk (the $V$-band light curve), could be extended to the whole disk and to other physical processes. / Estrelas Be são um subtipo específico de estrelas de sequência principal de tipo espectral B. Elas possuem características únicas tais como a presença de linhas de emissão em seu espectro, que se originam de um disco circunstelar. Nos últimos 50 anos, a estrela Be galáctica CMa exibiu erupções quasi-regulares, a cada 8 anos aproximadamente, onde a estrela torna-se mais brilhante na banda V. Nestas erupções um novo disco se forma nos primeiros 3-4 anos e depois dissipa-se nos 4-6 anos seguintes. Temos acesso a uma base de dados rica (incluindo fotometria, polarimetria, interferometria e espectroscopia) de CMa desde março de 1964, que cobre vários ciclos de erupções e quiescências. Assim, a natureza nos proveu um experimento perfeito para estudar como discos de estrelas Be crescem e dissipam-se. Há um corpo de evidências cada vez maior que sugerem que os discos de estrela Be são bem descritos pelo modelo de decréscimo viscoso (VDD), segundo o qual a formação e estrutura do disco depende da viscosidade cinemática do gás. Entretanto, a maioria dos testes conduzidos com o VDD até o momento foram feitos para sistemas que não mostram forte variabilidade temporal. Usamos a rica base de dados de CMa para conduzir o primeiro teste aprofundado do VDD em um sistema fortemente variável. Usamos o código de transporte radiativo HDUST para analisar e interpretar os dados. Desta análise obtemos (1) um modelo fisicamente realista do ambiente circunstelar, (2) a viscosidade do gás, e (3) uma estimativa confiável das taxas de perda de massa e momento angular durante os eventos de formação do disco. Nossas simulações conseguem reproduzir a variabilidade fotométrica muito bem, o que sugere que o modelo VDD descreve corretamente a evolução estrutural do disco. Mostramos que o parâmetro de viscosidade é variável, com valores entre 0.1 e 1. Adicionalmente, as fases de construção do disco têm valores de viscosidade maior. Contrariamente ao que se acredita, mostramos que durante a dissipação a taxa de perda de momento angular não é necessariamente nula, o que implica que CMa não experimenta uma quiescência verdadeira, mas alterna entre uma fase de alta taxa de perda de momento angular (erupção) e uma fase de baixa taxa (quiescência). Confrontamos as taxas de perda de momento angular com as preditas pelos modelos evolutivos de Genebra, e encontramos que nossas taxas são mais que 10 vezes menores que as taxas de previstas pelos modelos. O modelo desenvolvido para reproduzir a curva de luz na banda V foi aplicado a vários outros observáveis. De forma geral, os resultados deste estudo multi-técnica foram muito positivos, com uma boa concordância com a fotometria multi-banda, polarização, e a maioria das características espectrais. Este é um resultado muito relevante, pois prova que um modelo que foi construído apenas a partir de vínculos para a interna do disco (a curva de luz na banda V), pode ser estendido para todo o disco e também outros processos físicos.

La quantité d'hydrocarbures récupérés peut être considérablement augmentée si un placement optimal des puits non conventionnels à forer, peut être trouvé. Pour cela, l'utilisation d'algorithmes d'optimisation, où la fonction objectif est évaluée en utilisant un simulateur de réservoir, est nécessaire. Par ailleurs, pour des réservoirs avec une géologie complexe avec des hétérogénéités élevées, le problème d'optimisation nécessite des algorithmes capables de faire face à la non-régularité de la fonction objectif. L'objectif de cette thèse est de développer une méthodologie efficace pour déterminer l'emplacement optimal des puits et leurs trajectoires, qui offre la valeur liquidative maximale en utilisant un nombre techniquement abordable de simulations de réservoir.Dans cette thèse, nous montrons une application réussie de l'algorithme "Covariance Matrix Adaptation - Evolution Strategy" (CMA-ES) qui est reconnu comme l'un des plus puissants optimiseurs sans-dérivés pour l'optimisation continue. Par ailleurs, afin de réduire le nombre de simulations de réservoir (évaluations de la fonction objectif), nous concevons deux nouveaux algorithmes. Premièrement, nous proposons une nouvelle variante de la méthode CMA-ES avec des méta-modèles, appelé le nouveau-local-méta-modèle CMA-ES (nlmm-CMA), améliorant la variante déjà existante de la méthode local-méta-modèle CMA-ES (lmm-CMA) sur la plupart des fonctions de benchmark, en particulier pour des tailles de population plus grande que celle par défaut. Ensuite, nous proposons d'exploiter la séparabilité partielle de la fonction objectif durant le processus d'optimisation afin de définir un nouvel algorithme appelé la partiellement séparable local-méta-modèle CMAES (p-sep lmm-CMA), conduisant à une réduction importante en nombre d'évaluations par rapport à la méthode CMA-ES standard.Dans cette thèse, nous appliquons également les algorithmes développés (nlmm-CMA et p-sep lmm-CMA) sur le problème de placement des puits pour montrer, à travers plusieurs exemples, une réduction significative du nombre de simulations de réservoir nécessaire pour trouver la configuration optimale des puits. Les approches proposées sont révélées prometteuses en considérant un budget restreint de simulations de réservoir, qui est le contexte imposé dans la pratique.Enfin, nous proposons une nouvelle approche pour gérer l'incertitude géologique pour le problème d'optimisation de placement des puits. L'approche proposée utilise seulement une réalisation, ainsi que le voisinage de chaque configuration, afin d'estimer sa fonction objectif au lieu d'utiliser multiples réalisations. L'approche est illustrée sur un cas de réservoir de benchmark, et se révèle être en mesure de capturer l'incertitude géologique en utilisant un nombre réduit de simulations de réservoir.

Background:     The microdialysis (MD) technique is widely spread and used both experi­mentally and in clinical practice. The MD technique allows continuous collection of small molecules such as glucose, lactate, pyruvate and glycerol. Samples are often analysed using the CMA 600 analyser, an enzymatic and colorimetric analyser.  Data evaluating the performance of the CMA 600 analysis system and associated sample han­dling are sparse. The aim of this work was to identify sources of variability related to han­dling of microdialysis samples and sources of error associated with use of the CMA 600 analyser. Further, to develop and compare different application techniques of the micro­dialysis probes both within an organ and on the surface of an organ.  Material and Methods:  Papers I and II are mainly in vitro studies with the exception of the No Net Flux calibration method in paper I where a pig model (n=7) was used to exam­ine the true concen­tration of glucose and urea in subcutaneous tissue. Flow rate, sampling time, vial and caps material and performance of the analyser device (CMA 600) were examined. In papers III and IV normoventilated anaesthetised pigs (n=33) were used. In paper III, heart ischemia was used as intervention to compare microdialysis measurements in the myocardium with corresponding measurements on the heart surface. In paper IV, microdialysis measurements in the liver parenchyma were compared with measurements on the liver surface in associa­tion with induced liver ischemia. All animal studies were approved by the Animal Experi­mental Ethics Committee at Umeå University Sweden. Results:  In paper I we succeeded to measure true concentrations of glucose (4.4 mmol/L) and Urea (4.1 mmol/L) in subcutaneous tissue. Paper II showed that for a batch analyse of 24 samples it is preferred to store microdialysis samples in glass vials with crimp caps. For reliable results, samples should be centrifuged before analysis. Paper III showed a new application area for microdialysis sampling from the heart, i.e. surface sampling. The sur­face probe and myocardial probe (in the myocardium) showed a similar pattern for glucose, lactate and glycerol during baseline, short ischemic and long ischemic interventions. In paper IV, a similar pattern was observed as in paper III, i.e. data obtained from the probe on the liver surface showed no differences compared with data from the probe in liver paren­chyma for glucose, lactate and glycerol concentrations during baseline, ischemic and reperfusion interven­tions. Conclusion:  The MD technique is adequate for local metabolic monitoring, but requires methodological considerations before starting a new experimental serie. It is important to consider factors such as flow rate, sampling time and handling of samples in association with the analysis device chosen. The main finding in this thesis is that analyses of glucose, lactate and glycerol in samples from the heart surface and liver surface reflect concentra­tions sampled from the myocardium and liver parenchyma, respectively.

No description available.

Simulation is often used in research and industry as a low cost, high efficiency alternative to real model testing. Simulation has also been used to develop and test powerful learning algorithms. However, optimized values in simulation do not translate directly to optimized values in application. In fact, heavy optimization in simulation is likely to exploit the simplifications made in simulation. This observation brings to question the utility of learning in simulation. The UT Austin Villa 3D Simulation Team developed an optimization framework on which a robot agent was trained to maximize the speed of an omni-directional walk. The resulting agent won first place in the 2011 RoboCup 3D Simulation League. This thesis presents the adaptation of this optimization framework to learn parameters in simulation that improved the forward walk speed of the real Aldebaran Nao. By constraining the simulation with tree models learned from the real robot, and manually guiding the optimization based on testing on the real robot, the Nao's walk speed was improved by about 30%. / text

Gelasine Herb. (Tigridieae: Iridaceae) é composto por sete espécies nativas da América do Sul, sendo três delas encontradas no Rio Grande do Sul (Brasil): G. coerulea (Vell.) Ravenna, G. elongata (Graham) Ravenna e G. uruguaiensis Ravenna. São plantas bulbosas de folhas plicadas, flores perfeitas azuis ou roxas e compostas por dois conjuntos de tépalas desiguais. Gelasine elongata e G. coerulea encontram-se na lista de espécies ameaçadas para o RS, sendo a primeira delas ameaçada e a segunda criticamente ameaçada. Apesar de seu atual estado de vulnerabilidade, Gelasine é um gênero ainda pouco estudado, não havendo nenhuma informação quanto à variabilidade e diversidade genética. Os dados citogenéticos são também ainda escassos. Assim, a presente dissertação tem por objetivo caracterizar as três espécies de Gelasine ocorrentes no sul do Brasil quanto a aspectos moleculares, citogenéticos, além de compreender suas relações. Para a caracterização da diversidade genética foram usadas duas populações de G. coerulea e duas de G. elongata; não foi possível a utilização de G. uruguaiensis em função do número restrito de indivíduos. As amostras de DNA foram obtidas a partir de folhas das espécies mencionadas e empregada a técnica de ISSR (Inter Simple Sequence Repeat). Foram testados 44 primers para ISSR, destes, 12 apresentaram um bom padrão de amplificação que em conjunto geraram 91 loci. A quantidade de bandas por primer variou em média de 7,5. Este trabalho resultou em dados inéditos para o gênero Gelasine quanto à variabilidade genética inter e intra-populacional. Os resultados indicam que a variação genética intrapopulacional é muito baixa e que a maior diversidade encontrada para estas espécies ocorreu entre as populações. Não foi verificada correlação significativa com a distância geográfica entre as populações. Tais resultados indicam que o sistema reprodutivo, o método de dispersão de sementes e a presença de descendência clonal oriunda da divisão dos bulbos subterrâneos são fatores de grande influência na diversidade. Para caracterização citogenética das espécies foi empregada coloração convencional e bandeamento CMA/DAPI, e realizadas medidas cromossômicas. Foi também estimado o tamanho do genoma por citometria de fluxo a partir de folhas frescas das três espécies. As análises citogenéticas se mostraram bastante eficientes para a diferenciação das três espécies de Gelasine investigadas. Gelasine coerulea e G. uruguaiensis apresentam o mesmo número cromossômico básico e somático (2n = 2x = 14), não sendo encontrados citótipos poliploides. Ambas têm cariótipos relativamente simétricos, porém se mostram bastante distintas quanto ao tamanho dos cromossomos e seu padrão de bandeamento, com uma grande variação na ocorrência e distribuição de sequências de DNA repetitivo (bandas CMA/DAPI). O conteúdo de DNA também permite a clara diferenciação dessas espécies, tendo G. coerulea 2C = 11,30 pg e G. uruguaiensis 2C = 16,88 pg. Gelasine elongata possui número cromossômico básico diferente das anteriores (2n = 2x = 12) e cariótipo claramente bimodal. Os cromossomos têm menor tamanho, o que, consequentemente reflete no menor tamanho de genoma (2C = 3,45 pg). Além disso, o padrão de bandas CMA/DAPI é notadamente mais simples que das outras duas espécies, onde o maior par de cromossomos (par I) exibe as únicas bandas CMA+ presentes na região da constrição secundária. Os dados obtidos para G. elongata apontam para uma maior semelhança dessa espécie com outras duas do gênero Eleuthenine (2n = 2x = 12), o que reforça os dados filogenéticos existentes, onde G. elongata está separada de G. coerulea e agrupada no mesmo ramo de Eleutherine. Não foi observado heteromorfismo cromossômico para Gelasine elongata e nem para as outras duas espécies investigadas, embora tal situação tenha sido reportada para aquela espécie. Os dados obtidos para Gelasine com o uso dos fluorocromos CMA e DAPI, bem como os demais parâmetros citogenéticos investigados permitiram a clara diferenciação entre as espécies. Associados a uma abordagem filogenética, tais resultados auxiliam a compreensão das relações entre essas espécies e sua evolução. / Gelasine Herb. (Tigridieae: Iridaceae) comprises seven native species from South America, three of them are found in Rio Grande do Sul (Brasil): G. coerulea (Vell.) Ravenna, G. elongata (Graham) Ravenna and G. uruguaiensis Ravenna. These species are bulbous plants with plicate leaves and blue or violet perfect flowers which are composed of two unequal groups of tepals. Gelasine elongata and G. coerulea are included in the list of endangered species from RS, the first one is considered endangered and the latter, critically endangered. Notwithstanding its current vulnerability status, Gelasine is still a poorly studied genus and genetic variability and diversity information concerning its species are lacking. Cytogenetic data are also scarce. Thus the present dissertation aims to characterize the three Gelasine species occurring in Southern Brazil regarding its molecular and cytogenetic aspects in addition to understand their relationships. To characterize their genetic diversity, two populations of G. coerulea and two of G. elongata were used; it was not possible to investigate G. uruguaiensis due to its restricted number of individuals. DNA samples were obtained from leaves of the aforementioned species and ISSR (Inter Simple Sequence Repeat) technique was employed. Fourty-four ISSR primers were tested, 12 of these presented good amplification pattern which generated a total of 97 loci. The number of bands per primer had an average of 7.5. The present study resulted in novelty data for Gelasine concerning its inter and intrapopulation genetic variability. The results indicate a very low intrapopulation genetic variation and most of the diversity found in these species occurred among their populations. No significant correlation was verified between geographical distances of populations. Such results indicate that reproductive system, seed dispersal mechanisms and presence of clonal descendants generated from divisions of subterranean bulbs are factors that greatly influence in diversity. For cytogenetic characterization of the species, conventional staining and CMA/DAPI banding were employed and chromosome measurements were made. Also, genome size was estimated through flow cytometry using fresh leaves from the three species. Cytogenetic analyses were very efficient to differentiate all investigated species of Gelasine. Gelasine coerulea and G. uruguaiensis have the same basic and somatic chromosome number (2n = 2x = 14); polyploid cytotypes were not found. Both species display fairly symmetric karyotypes, however they are very distinct with respect to chromosome sizes and banding patterns, with a great variation in the occurrence and distribution of repetitive DNA sequences (CMA/DAPI bands). DNA content also allows clear differentiation of these species; G. coerulea has 2C = 11,30 pg and G. uruguaiensis has 2C = 16,88 pg. Gelasine elongata has a different base chromosome number than both former species (2n = 2x = 12) and a clearly bimodal karyotype. Its chromosomes are smaller which, consequently, reflects on the smaller genome size (2C = 3,45 pg). Furthermore, its CMA/DAPI band pattern is markedly simpler than the ones from the other two species, where the largest chromosome pair (pair I) contains the only CMA+ bands present in the secondary constriction region. Data obtained from G. elongata points out a larger resemblance between this species and two others belonging to Eleuthenine (2n = 2x = 12), which supports the phylogenetic data where G. elongata is separate from G. coerulea and groups with Eleutherine. Chromosome heteromorphism was not observed in Gelasine elongata nor in the two other investigated species, even though it had been reported for the first one. Data obtained from Gelasine with the use of CMA and DAPI fluorochromes, along with the other cytogenetic parameters investigated, allowed clear differentiation between species. Allied to a phylogenetic approach, these results can bring better understanding to the relations between these species and their evolution.