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Masters, Craig Eugene Ashman Keith M. "The formation of low metallicity globular clusters". Diss., UMK access, 2007.
Znajdź pełny tekst źródła"A dissertation in physics and mathematics." Advisor: Keith M. Ashman. Typescript. Vita. Title from "catalog record" of the print edition Description based on contents viewed Nov. 13, 2007. Includes bibliographical references (leaves 67-70). Online version of the print edition.
Szécsi, Dorottya [Verfasser]. "The evolution of low-metallicity massive stars / Dorottya Szécsi". Bonn : Universitäts- und Landesbibliothek Bonn, 2016. http://d-nb.info/1113688262/34.
Pełny tekst źródłaFukushima, Hajime. "Radiative feedback from massive stars in low-metallicity environments". Kyoto University, 2019. http://hdl.handle.net/2433/242603.
Pełny tekst źródłaKrawchuk, Curtis A. P. "The determination of metallicity and temperature of low-mass stars using broad-band photometry". Thesis, National Library of Canada = Bibliothèque nationale du Canada, 1997. http://www.collectionscanada.ca/obj/s4/f2/dsk2/tape15/PQDD_0035/MQ27361.pdf.
Pełny tekst źródłaLindgren, Sara. "Metallicity determination of M dwarfs". Doctoral thesis, Uppsala universitet, Observationell astrofysik, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-332102.
Pełny tekst źródłaVerdugo, Salgado Celia Anahi. "Star formation in low gas density and low metallicity environments". Observatoire de Paris, 2015. https://hal.science/tel-02095302.
Pełny tekst źródłaIn nearby galaxies, an empirical relation has been established between star formation and gas surface densities, the Kennicutt-Schmidt (KS). The relation is nearly linear when molecular gas (H2) is considered, while is less tight with atomic hydrogen (HI). These low gas density regions are of a key importance in the field of star formation, since the are also low metallicity environments, resembling the conditions of a younger universe. This thesis summarizes the observational work done with the IRAM 30MT telescope in two kinds of such regions : disk galaxies with extended ultra-violet emission (XUV), and the interstellar medium going into the hot intra-cluster medium (ICM) under ram-pressure stripping in the Virgo cluster. The galex telescope has unveiled in far ultra-violet (FUV) star formation in the outer parts of some disk galaxies that was not traced by HA. To determine the presence of H2 and analyse the K-S relation in these regions, CO observations where done in the outskirts of several XUV disk galaxies, finding both detections and upper limits. These K-S relations showed a broken power law at low gas densities, below the HI-H2 threshold. In the Virgo cluster, similar CO observations were done along the HI tidal arm connecting NGC4388 and M86, where no H2 is expected. Two detections were found, showing very low star formation efficiencies (depleting less than 0,1 % of the gas reservoir per 10 [exposant] 8 yr), and showing again a disconuity of the K-S relation at low gas densities, probing that the process of a gas consumption into stars well known at high densities cannot be extrapolated to lower densities, and that H2 can survive a certain time in the hostile ICM
Rajpurohit, Arvind Singh. "Low-mass stars as tracers of the milky way populations : investigating the effects of metallicity in cool atmosphere". Thesis, Besançon, 2013. http://www.theses.fr/2013BESA2023/document.
Pełny tekst źródłaVery Low-Mass stars (M dwarfs) are an important source of information for probing the lowmass end of the main sequence, down to the hydrogen burning limit. They are the dominantstellar component of the Galaxy and make up the majority of baryonic matter in the Galaxy.Moreover, an increasing number of M dwarfs are now known to host exoplanets, includingsuper-Earth exoplanets. The determination of accurate fundamental parameters for M dwarfshas therefore relevant implications for both stellar and Galactic astronomy as well as planetology.Despite their large number in the Galaxy, M dwarfs remain elusive objects and themodelling of their photosphere has long remained a challenge (molecular opacities, dust cloudformation). The description of these stars therefore need a strong empirical basis, or validation.In particular, the effect of metallicity on the physics of cool atmospheres are still poorly known,even for early-type M-dwarfs.[...]
Ramachandran, Varsha [Verfasser], i Wolf-Rainer [Akademischer Betreuer] Hamann. "Massive star evolution, star formation, and feedback at low metallicity : quantitative spectroscopy of OB stars in the Magellanic Clouds / Varsha Ramachandran ; Betreuer: Wolf-Rainer Hamann". Potsdam : Universität Potsdam, 2019. http://d-nb.info/1218405058/34.
Pełny tekst źródłaKunawicz, Nadya. "Any old iron? : astrochemical modelling of star-forming regions at low metallicity". Thesis, University of Manchester, 2010. https://www.research.manchester.ac.uk/portal/en/theses/any-old-iron--astrochemical-modelling-of-starforming-regions-at-low-metallicity(2a356b1a-429c-40b5-b9c0-2b4cdab12ea8).html.
Pełny tekst źródłaLombardo, Linda. "Explorer l'histoire de la Galaxie grâce à la spectroscopie stellaire". Electronic Thesis or Diss., Université Paris sciences et lettres, 2022. http://www.theses.fr/2022UPSLO011.
Pełny tekst źródłaThis thesis project presents several studies that are focused on the investigation of the chemical properties of different stellar populations in the Milky Way by means of high-resolution spectroscopy.The thesis is structured as follows:The first chapter is an introduction to the thesis project, and is divided into three sections. The first section describes the structure and formation scenarios of the Milky Way, in particular by referring to the most recent discoveries. The second section introduces the basic concepts and objectives of the studies presented in this thesis work. The third section describes the methods used to analyse the spectroscopic data.The second chapter presents the studies carried out in the context of the MINCE project. The first study is devoted to the chemical analysis of a sample of young giant stars that was serendipitously discovered during the first MINCE observations. My contribution in this work was to derive the stellar parameters, analyse the spectroscopic data, measure the rotational velocities, compare the results with theoretical models and write the paper. The second study presents the results obtained from the analysis of the first sample of MINCE stars. In this work, I contributed to the analysis of some of the stars in the sample.The third chapter presents the results obtained in the context of the CERES project. The first study presents a detailed chemical analysis of the star RAVE J110842.1-715300, with the aim of understanding whether or not it originated in the Omega Centauri globular cluster. My contribution in this study was to derive the stellar parameters of the star. The second study presents the results obtained for the CERES star sample. My contribution was to derive the parameters, compute model atmospheres, measure the chemical abundances, and write the paper.The fourth chapter presents the results obtained in the context of the High-speed stars project. The first study reports the results obtained from the high-resolution follow-up of two young and metal-poor stars in the sample of Caffau et al. (2020), to check whether they are blue stragglers or not. My contribution in this study was to obtain the high-resolution observations with UVES and to analyse the data. These results have not been published yet. The second study presents a detailed analysis of two high-speed stars observed with Subaru. In this study I was involved in the C abundance determination.The fifth chapter presents the results obtained from the chemical analysis of samples of stars selected using the Pristine photometry. The first study presents the chemical analysis of a sample of metal-poor stars that may have been enriched by the explosion of pair instability supernovae. My contribution was to select promising candidates and observe them with the SOPHIE spectrographat Observatoire de le Haute Provence (OHP)in visitor mode. The second study presents the preliminary results obtained from the chemical analysis of a sample of Pristine extremely metal-poor candidates. My contribution in this study was to derive the stellar parameters and the chemical abundances. The paper is in preparation.The sixth chapter concludes the thesis and gathers final reflections and future projects
Polles, Fiorella Lucia. "Properties of the interstellar medium of the star-forming galaxy, IC10, at various spatial scales". Thesis, Université Paris-Saclay (ComUE), 2017. http://www.theses.fr/2017SACLS276/document.
Pełny tekst źródłaThe properties of the Interstellar Medium (ISM) strongly influence the environment and processes that lead to star-formation, which in turn, drives the evolution of a galaxy. Dwarf galaxies in the Local Group are perfect laboratories to investigate how the metal-poor ISM affects the interplay between gas, dust and stars. In this thesis, I investigate the properties of the HII regions and the diffuse ionized gas of the nearby dwarf galaxy IC10, which has a metallicity of 1/3 solar. Its proximity (d=700 kpc) enables the analysis on different spatial scales: from the compact clumps (~25 pc) to the whole star-forming body of the galaxy (~650pc). In order to measure the physical properties of the ISM, I model the infrared emission lines observed with Spitzer and Herschel with photoionization and photodissociation models. I present an extensive exploration of different methods to determine the most reliable ISM properties, based on the available constraints. I determined the properties of the brightest star-forming clumps within the galaxy and show that the emission at large scales (~300 pc) is dominated by that of the compact, bright clumps that lie within the region. I further demonstrate the need for a multi-component model to fully reproduce the observations
Lau, Ho Bun. "Evolution and nucleosynthesis of zero-metallicity AGB stars". Thesis, University of Cambridge, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.612023.
Pełny tekst źródłaPACE, GIANCARLO. "AGE, METALLICITY AND ACTIVITY IN SOLAR-TYPE STARS". Doctoral thesis, Università degli studi di Trieste, 2005. http://thesis2.sba.units.it/store/handle/item/13164.
Pełny tekst źródłaGarcía, Pérez Ana E., Melissa Ness, Annie C. Robin, Inma Martinez-Valpuesta, Jennifer Sobeck, Gail Zasowski, Steven R. Majewski i in. "The Bulge Metallicity Distribution from the APOGEE Survey". IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/626538.
Pełny tekst źródłaWisniewski, John Patrick. "The effect of age and metallicity on Be circumstellar disk formation /". See Full Text at OhnioLINK ETD Center (Requires Adobe Acrobat Reader for viewing), 2005. http://www.ohiolink.edu/etd/view.cgi?acc%5Fnum=toledo1124412024.
Pełny tekst źródłaTypescript. "A dissertation [submitted] as partial fulfillment of the requirements of the Doctor of Philosophy degree in Physics." Bibliography: leaves 328-333.
Covarrubias, Ricardo Alberto. "Does the metallicity affect the fate of massive stars? /". Thesis, Connect to this title online; UW restricted, 2007. http://hdl.handle.net/1773/5442.
Pełny tekst źródłaAlves, Cruz Monique. "Nucleosynthesis in extremely metal-poor and zero metallicity stars". Diss., lmu, 2012. http://nbn-resolving.de/urn:nbn:de:bvb:19-153061.
Pełny tekst źródłaMasters, Craig Eugene Ashman Keith M. "The low metallicity globular clusters". Diss., UMK access, 2005.
Znajdź pełny tekst źródła"A thesis in physics." Typescript. Advisor: K. M. Ashman Vita. Title from "catalog record" of the print edition Description based on contents viewed June 26, 2006. Includes bibliographical references (leaves 54-56). Online version of the print edition.
Mulders, Gijs D., Ilaria Pascucci, Dániel Apai, Antonio Frasca i Joanna Molenda-Żakowicz. "A SUPER-SOLAR METALLICITY FOR STARS WITH HOT ROCKY EXOPLANETS". IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622435.
Pełny tekst źródłaBadenes, Carles, Christine Mazzola, Todd A. Thompson, Kevin Covey, Peter E. Freeman, Matthew G. Walker, Maxwell Moe i in. "Stellar Multiplicity Meets Stellar Evolution and Metallicity: The APOGEE View". IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/627094.
Pełny tekst źródłaGáspár, András, George H. Rieke i Nicholas Ballering. "THE CORRELATION BETWEEN METALLICITY AND DEBRIS DISK MASS". IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621391.
Pełny tekst źródłaBolatto, Pereira Alberto D. "The interstellar medium in low metallicity environments". Thesis, Boston University, 2001. https://hdl.handle.net/2144/36768.
Pełny tekst źródłaPLEASE NOTE: Boston University Libraries did not receive an Authorization To Manage form for this thesis or dissertation. It is therefore not openly accessible, though it may be available by request. If you are the author or principal advisor of this work and would like to request open access for it, please contact us at open-help@bu.edu. Thank you.
This dissertation studies the interstellar medium (ISM) in dwarf galaxies. Dwarf galaxies are important because: 1) they constitute the largest fraction of extragalactic systems, and 2) they provide templates for primordial galaxies. Indeed, local active dwarf galaxies resemble primitive systems, since they are poor in dust and heavy elements and they are profusely forming massive stars. Because dwarf galaxies are nearby, however, they can be observed in much greater detail than distant primordial systems. Therefore studies of the ISM in nearby dwarf galaxies can be used to understand the processes at work in primitive galaxies. This work focuses on the effects of low heavy element abundances (i.e., low metallicities) on the star-forming ISM. Low metallicities are known to drastically affect the ISM. With decreasing metallicity, an increasingly large fraction of the molecular ISM is photodissociated into atoms and ions. We modeled and observed the emission of a sample of low metallicity dwarf galaxies in the millimeter, submillimeter, and far-infrared wavebands. The submillimeter waveband allows us to observe the mid-J rotational transitions of carbon monoxide (CO), the usual tracer of the molecular ISM, and the fine structure transit ions of neutral carbon ([C I]), a tracer of translucent and photodissociated material. We studied regions in the Large and Small Magellanic Clouds and the Northern Hemisphere dwarf galaxy IC 10. We find that the preponderant mechanism producing neutral carbon inside molecular clouds is photodissociation. We observe a moderate increase in the ratio of [C I] to CO emission for decreasing metallicity. Our models of clumpy, unresolved photo dissociation regions explain these observations as the natural result of an augmented fraction of photo dissociated material. Finally, our observations of the submillimeter thermal dust continuum in IC 10 find an abnormally low emissivity exponent for its graybody emission. We conclude that the unusual dust continuum is caused by the selective destruction of small grains, brought about by the combined effects of low metallicities and high radiation fields.
2031-01-01
Spalding, Eckhart. "A New Set of Spectroscopic Metallicity Calibrations for RR Lyrae Variable Stars". UKnowledge, 2014. http://uknowledge.uky.edu/physastron_etds/22.
Pełny tekst źródłaSantucci, Rafael Miloni. "Identificação de subestruturas no halo galáctico através de estrelas azuis tardias". Universidade de São Paulo, 2016. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-12062018-113847/.
Pełny tekst źródłaEverything that lives long enough is able to contribute with good stories about the past. This statement also applies to the blue straggler stars (BSSs), which can be found in all stellar environments. These old stars appear to be very young and perhaps because of this have never been properly addressed in a context larger than their own lives. This work interprets the story they tell about the nature of the Galactic halo, through their fundamental physical parameters: coordinates, temperatures, surface gravities, metallicities, colors, distances and ages. This work uses the Sloan Digital Sky Survey (SDSS) database to select BSS candidates through photometric and spectroscopic criteria. Altogether, 8001 BSS candidates survived the various selection methods applied and were used as the database for this study. This large sample allowed the determination of the average frequency of BSSs in the halo, compared to the number of blue horizontal branch stars (BHBs). The average frequency of BSS/BHB found in the galactic halo by this work is 2.15±0.13, very similar to this ratio in nearby dwarf galaxies (~2.24±0.17). In addition, this work verified that the BSSs show a color gradient as a function of distance to the galactic center, which appears to be independent from metallicity. To this color variation was assigned an age variation, yielding an average gradient of -0.034±0.002 Gyr/kpc in the halo. This result shows that the older regions preferentially occur in the center of the Galaxy and get younger for larger distances. The BSSs color gradient allowed the construction of galactic halo age maps. These maps were superimposed to the central positions of a collection of substructures found in the literature. Approximately 60% of them have positions that agree with the color fluctuations observed in the maps, as well as having similar kinematic and chemical properties to the BSSs in those regions (within 2).
Alves, Cruz Monique [Verfasser], i Achim [Akademischer Betreuer] Weiss. "Nucleosynthesis in extremely metal-poor and zero metallicity stars / Monique Alves Cruz. Betreuer: Achim Weiss". München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2012. http://d-nb.info/1032131225/34.
Pełny tekst źródłade, Koter A., J. S. Vink i L. Muijres. "Constraints on wind clumping from the empirical mass-loss vs. metallicity relation for early-type stars". Universität Potsdam, 2007. http://opus.kobv.de/ubp/volltexte/2008/1773/.
Pełny tekst źródłaSantucci, Rafael Miloni. "Caracterização de estrelas azuis tardias no campo galáctico". Universidade de São Paulo, 2012. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-20062013-155903/.
Pełny tekst źródłaBlue straggler stars (BSSs) are main sequence stars that exhibit an apparent evolutionary delay over the region where they are found in the HR diagram. They were initially identified in the main sequence of globular clusters above the turnoff point. Since then, they have been found in many different stellar environments: globular and open clusters, near dwarf galaxies, and also in the field of the Galaxy. The main goal of this work is to build a large sample of BSSs in the galactic field region. In order to accomplish this task, classical methods of separation of BSS from BHB stars were compared with proposed restrictions based on their atmospheric parameters, which are estimated by the SEGUE Stellar Parameter Pipeline (SSPP). The latter procedure allowed to include stars with magnitudes g greater than 18, not handled by traditional methods when signal-noise ratio is smaller than 9. The selection methods gathered a sample of 8001 BS stars. These stars were kinematically analyzed through their radial velocities. The results suggest that many of them (about 1500) can have extragalactic origin, associated with Sagittarius stream.
Goldman, Steve. "The metallicity dependence of maser emission and mass loss from red supergiants and asymptotic giant branch stars". Thesis, Keele University, 2017. http://eprints.keele.ac.uk/4258/.
Pełny tekst źródłaYoung, D. R. "Core-collapse supernovae in low-metallicity galaxies and all-sky transient surveys". Thesis, Queen's University Belfast, 2010. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.517021.
Pełny tekst źródłaCormier, Diane. "The physical properties in the interstellar medium of low-metallicity dwarf galaxies". Paris 7, 2012. http://www.theses.fr/2012PA077193.
Pełny tekst źródłaIn the framework of galaxy evolution, local star-forming dwarf galaxies are ideal laboratories to study star formation processes at low metallicity and the role of metal enrichment on the physical conditions. My thesis has focused on the study of the gas properties of the dwarf galaxies from "The Herschel Dwarf Galaxy Survey", combining observations and modeling efforts. I have investigated the role of the most important tracers of the multi-phase the interstellar medium (ISM), in the mid-infrared to submillimeter range. Particular attention was paid to the ionized and neutral gas coolants observed with Herschel Space Observatory (e. G. [OIII] 88, [OI]63, [CII] 157 micron lines), and to the CO molecule, probing the molecular phase, with complementary ground-based observations. The data are interpreted in physical terms (density, radiation field, filling factors) with radiative transfer models. This work has helped elucidate the structure and conditions of the low-metallicity ISM. It highlights the porosity of the ISM of dwarf galaxies, with ultraviolet photons from the massive star-forming regions excitinig the gas out to large distances. This results in the presence of large volume filling factor diffuse ionized/neutral gas, clumpy photodissociation regions, and little observed molecular gas due to large-scale photodissociation
Chen, Yang. "Evolution of Very Low Mass Stars and Very Massive Stars in PARSEC". Doctoral thesis, SISSA, 2015. http://hdl.handle.net/20.500.11767/4879.
Pełny tekst źródłaSchlesinger, Katharine J. "The Metallicity Distribution Functions of Cool Stars in the SEGUE Survey: Clues to Understanding Milky Way Formation and Evolution". The Ohio State University, 2011. http://rave.ohiolink.edu/etdc/view?acc_num=osu1312924463.
Pełny tekst źródłaPineda, John Sebastian. "Activity and kinematics of low mass stars". Thesis, Massachusetts Institute of Technology, 2010. http://hdl.handle.net/1721.1/61260.
Pełny tekst źródłaCataloged from PDF version of thesis.
Includes bibliographical references (p. 95-96).
We present an analysis of the magnetic activity, photometry and kinematics of approximately 70000 M dwarfs from the Sloan digital Sky Survey (SDSS) Data Release 7. This new analysis explores the spatial distribution of these M dwarf properties as a function of vertical distance from the Galactic plane (Z) and distance from the Galactic center (R). We confirm the established trends of decreasing magnetic activity, as measured by Ha emission, with increasing distance from the mid-plane of the disk but also observe a new trend in Galactocentric radius, apparent in the analysis of spectral types M3 and M4 of a small increase in activity with increasing R. Examining the color indices r - z, r - i and g - r from the SDSS ugriz photometry reveals noticeable gradients in the vertical direction but not in the radial direction. To analyze the kinematics we develop a new technique utilizing probability distributions and a pseudo-montecarlo data fitting scheme to determine the parameters (o- 1, pi, 0-2, 12) and normalization of the underlying Gaussians making up the kinematic distributions of the stellar population. We analyze each of the spatial velocities VR, Vz , and Ve defined in a Galactocentric cylindrical coordinate system. The kinematic analysis reproduced previous trends of increasing dispersion with increasing distance from the mid-plane, but with much greater accuracy and reliability and to distances farther out away from the mid-plane. The analysis did not reveal any significant kinematic trends in the radial domain.
by John Sebastian Pineda.
S.B.
Rainger, Paul P. "Studies of low-mass interacting binary stars". Thesis, University of St Andrews, 1990. http://hdl.handle.net/10023/14369.
Pełny tekst źródłaMendes, Luiz Themystokliz Sanctos. "Evolutionary models of rotating low mass stars". Universidade Federal de Minas Gerais, 1999. http://hdl.handle.net/1843/BUOS-9GGP5S.
Pełny tekst źródłaNeste trabalho nós investigamos os efeitos combinados da rotação e da redistribuição de momento angular em estrelas de baixa massa, desde a etapa pré-sequência principal até a sequência principal. Como uma ferramenta para tal estudo, o código evolutivo estelar ATON (Mazzitelli 1989; Ventura et al. 1998b) foi alterado de forma a incluir tais efeitos. A rotação foi implementada segundo a técnica de superfícies equipotenciais desenvolvida por Kippenhahn & Thomas (1970) e posteriormente aperfeiçoada por Endal & Sofia (1976). A redistribuição de momento angular foi modelada por intermédio de uma equação diferencial parcial do tipo difusivo-advectivo, com base na teoria originalmente desenvolvida por Chaboyer & Zahn (1992), a qual considera como único pressuposto que o transporte turbulento é muito mais forte na direção horizontal que na vertical. O coeficiente de difusão desta equação é obtido a partir de comprimentos e velocidades característicos de instabilidades hidrodinâmicas induzidas pela rotação. Este novo código foi empregado para calcular uma série de modelos com rotação de estrelas de baixa massa (na faixa de 0.6 M_ a 1.2 M_). As características gerais destes modelos, com relação aos efeitos estruturais (hidrostáticos) da rotação, mostram que estrelas com rotação comportam-se como se fossem estrelas sem rotação, porém de massa ligeiramente menor, estando de acordo com resultados anteriores por outros pesquisadores. Um estudo deste efeito de abaixamento de massa" para a faixa de massas considerada revela que a rotação diminui a queima de lítio enquanto a estrela é totalmente convectiva, mas aumenta a mesma tão logo a estrela desenvolve um núcleo radiativo. O efeito líquido é um aumento da queima de lítio, em desacordo com dados observacionais que mostram que as estrelas de aglomerados abertos jovens que giram mais rápido são as que apresentam menor queima de lítio. A redistribuição de momento angular nos modelos considerados torna-se muito eficaz na suavização do gradiente interno de velocidade angular tão logo a estrela atinja a idade zero na sequência principal, mas não é capaz de reproduzir a curva de rotação solar obtida da heliosismologia, indicando que o transporte de momento angular no Sol é mais eficiente do que o predito pelos atuais modelos. O transporte interno de momento angular também contribui para uma queima ainda maior de lítio com relação aos modelos calculados somente com os efeitos estruturais. Isto sugere que outros fenômenos físicos devem ser importantes tanto para a queima de lítio quanto para a evolução da curva de velocidade angular das estrelas.
Dopcke, Gustavo [Verfasser], i Ralf S. [Akademischer Betreuer] Klessen. "On the physics of the low metallicity IMF / Gustavo Dopcke ; Betreuer: Ralf S. Klessen". Heidelberg : Universitätsbibliothek Heidelberg, 2013. http://d-nb.info/1177148528/34.
Pełny tekst źródłaKumari, Nimisha. "Spatially-resolved studies of nearby star-forming galaxies". Thesis, University of Cambridge, 2018. https://www.repository.cam.ac.uk/handle/1810/283605.
Pełny tekst źródłaCossburn, Martin R. "The study of low-mass stars and brown dwarfs". Thesis, University of Leicester, 1999. http://hdl.handle.net/2381/30616.
Pełny tekst źródłaPinfield, David J. "Low mass stars and brown dwarfs in open clusters". Thesis, University of Leicester, 1998. http://hdl.handle.net/2381/30612.
Pełny tekst źródłaKenyon, Michael John. "Low mass stars and brown dwarfs around σ Orionis". Thesis, Keele University, 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.409546.
Pełny tekst źródłaLehner, Nicolas. "Interstellar gas and hot stars in low density environments". Thesis, Queen's University Belfast, 2000. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.343034.
Pełny tekst źródłaPokorny, Richard S. "A high proper motion search for low mass stars". Thesis, Liverpool John Moores University, 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.419966.
Pełny tekst źródłaBrown, Daniel. "Impact of rotation on the evolutionof low-mass stars". Thesis, Liverpool John Moores University, 2007. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.446410.
Pełny tekst źródłaQuanz, Sascha Patrick. "Circumstellar disks and envelopes around young low-mass stars". [S.l. : s.n.], 2007. http://nbn-resolving.de/urn:nbn:de:bsz:16-opus-74785.
Pełny tekst źródłaZiegerer, Eva [Verfasser], i Ulrich [Gutachter] Heber. "Hypervelocity Stars - Kinematic studies of low-mass stars and hot subdwarfs / Eva Ziegerer ; Gutachter: Ulrich Heber". Erlangen : Friedrich-Alexander-Universität Erlangen-Nürnberg (FAU), 2017. http://d-nb.info/1152438239/34.
Pełny tekst źródłaBirkby, Jayne Louise. "Observational constraints on low-mass stellar evolution and planet formation". Thesis, University of Cambridge, 2012. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.610381.
Pełny tekst źródłaSaylor, Dicy, Sebastien Lepine, Ian Crossfield i Erik A. Petigura. "Light-curve Modulation of Low-mass Stars in K2. I. Identification of 481 Fast Rotators in the Solar Neighborhood". IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626405.
Pełny tekst źródłaCovey, Kevin R. "Dynamical properties of embedded protostars and the luminosity function of the galactic disk /". Thesis, Connect to this title online; UW restricted, 2006. http://hdl.handle.net/1773/5448.
Pełny tekst źródłaSzigeti, László, Szabolcs Mészáros, Verne V. Smith, Katia Cunha, Nadège Lagarde, Corinne Charbonnel, D. A. García-Hernández i in. "12C/13C isotopic ratios in red-giant stars of the open cluster NGC 6791". OXFORD UNIV PRESS, 2018. http://hdl.handle.net/10150/627135.
Pełny tekst źródłaCuadrado, Regina Aznar. "Binarity and the origin of subdwarf B stars". Thesis, Queen's University Belfast, 2001. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.483466.
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