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Dissertations / Theses on the topic 'Stars of low metallicity'

Author: Grafiati

Published: 8 June 2024

Last updated: 31 July 2025

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1

Masters, Craig Eugene Ashman Keith M. "The formation of low metallicity globular clusters." Diss., UMK access, 2007.

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Thesis (Ph. D.)--Dept. of Physics and Dept. of Mathematics. University of Missouri--Kansas City, 2007.<br>"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.

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2

Szécsi, Dorottya [Verfasser]. "The evolution of low-metallicity massive stars / Dorottya Szécsi." Bonn : Universitäts- und Landesbibliothek Bonn, 2016. http://d-nb.info/1113688262/34.

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3

Fukushima, Hajime. "Radiative feedback from massive stars in low-metallicity environments." Kyoto University, 2019. http://hdl.handle.net/2433/242603.

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4

Krawchuk, 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.

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5

Lindgren, 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.

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M dwarfs constitute around 70% of all stars in the local Galaxy. Their multitude together with their long main-sequence lifetimes make them important for studies of global properties of the Galaxy such as the initial mass function or the structure and kinematics of stellar populations. In addition, the exoplanet community is showing an increasing interest for those small, cold stars. However, very few M dwarfs are well characterized, and in the case of exoplanetary systems the stellar parameters have a direct influence on the derived planet properties. Stellar parameters of M dwarfs are diffic

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6

Verdugo, Salgado Celia Anahi. "Star formation in low gas density and low metallicity environments." Observatoire de Paris, 2015. https://hal.science/tel-02095302.

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Dans les galaxies proches, la relation empirique de Kennicutt-Schmidt (KS) a été établie entre la densité surfacique de formation d’étoiles et la densité surfacique de gaz. Elle est forte et presque linéaire quand on considère le gaz moléculaire (H2) mais devient moins valable lorsque l’hydrogène n’est qu’atomique (HI). Ces régions de densité de gaz faible sont d’une importance cruciale dans le domaine de la formation d’étoiles, car elles possèdent les mêmes conditions que dans les galaxies de l’univers jeune, de faible métallicité. Cette thèse compile les données observationnelles obtenues au

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7

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.

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Les étoiles de petite masse (naines M) forment la composante stellaire dominante de notre galaxie et contribuent à la majeure partie de la matière baryonique dans la galaxie. Notre compréhension de la galaxie repose donc sur la connaissance de cette composante peu lumineuse. Par ailleurs, un nombre grandissant d’exoplanètes sont découverte autour de naines M, y compris des super-terres. L’étude des naines M a ainsi des implications importantes sur la physique stellaire, permettant de comprendre les processus en jeu dans ces atmosphères froides. Ces astres restent cependant peu connus du fait d

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8

Ramachandran, Varsha [Verfasser], and 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.

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9

Kunawicz, 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.

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Two pseudo-time-dependent chemical models have been utilised - one of a dark cloud,and one of a hot core - in order to model these clouds in low metallicity environments, such as other galaxies. The dark cloud model uses gas-phase chemistry, whereas the hot core model includes both gas-phase and surface chemistry. The simulations have been calculated with varying initial elemental abundances of C, O, N, S and the heavy metals Fe, Mg and Na (henceforth, M). These initial abundances are taken from observations of HII regions in the Galaxy, the Large Magellanic Cloud and the Small Magellanic Clou

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10

Lombardo, 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.

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Ce travail de thèse présente plusieurs études qui utilisent la spectroscopie à haute résolution pour déterminer les propriétés chimiques des différentes populations stellaires de la Voie Lactée. Le document est structuré comme suit : Le premier chapitre de la thèse, divisée en 3 sections, est une introduction générale à la structure de la Voie lactée et à ses populations stellaires, suivie d'une partie décrivant les différentes méthodes utilisées pour mesurer les abondances chimiques des étoiles. La première section décrit les différents scénarios concernant la structure et la formation de la

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11

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.

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Les propriétés du milieu interstellaire (MIS) influencent fortement l’environnement et les processus menant à la formation d’étoiles qui, à son tour, dicte l’évolution d’une galaxie. Les galaxies naines du Groupe Local sont de parfaits laboratoires pour comprendre comment le contenu en métaux (ou métallicité) du MIS affecte l’interaction entre le gaz, la poussière et les étoiles. Mon travail de thèse porte sur les propriétés physiques des régions HII et du gaz diffus ionisé de la galaxie naine IC10, de métallicité 1/3 solaire. La proximité de cette galaxie (d=700kpc) permet l’analyse du MIS à

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12

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.

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13

PACE, 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.

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14

García, Pérez Ana E., Melissa Ness, Annie C. Robin, et al. "The Bulge Metallicity Distribution from the APOGEE Survey." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/626538.

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The Apache Point Observatory Galactic Evolution Experiment (APOGEE) provides spectroscopic information of regions of the inner Milky Way, which are inaccessible to optical surveys. We present the first large study of the metallicity distribution of the innermost Galactic regions based on high-quality measurements for 7545 red giant stars within 4.5 kpc of the Galactic center, with the goal to shed light on the structure and origin of the Galactic bulge. Stellar metallicities are found, through multiple Gaussian decompositions, to be distributed in several components, which is indicative of the

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Wisniewski, 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.

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Thesis (Ph.D.)--University of Toledo, 2005.<br>Typescript. "A dissertation [submitted] as partial fulfillment of the requirements of the Doctor of Philosophy degree in Physics." Bibliography: leaves 328-333.

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16

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.

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17

Alves, Cruz Monique. "Nucleosynthesis in extremely metal-poor and zero metallicity stars." Diss., lmu, 2012. http://nbn-resolving.de/urn:nbn:de:bvb:19-153061.

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Masters, Craig Eugene Ashman Keith M. "The low metallicity globular clusters." Diss., UMK access, 2005.

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Thesis (M.S.)--Dept. of Physics. University of Missouri--Kansas City, 2005.<br>"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.

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19

Mulders, Gijs D., Ilaria Pascucci, Dániel Apai, Antonio Frasca, and Joanna Molenda-Żakowicz. "A SUPER-SOLAR METALLICITY FOR STARS WITH HOT ROCKY EXOPLANETS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622435.

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Host star metallicity provides a measure of the conditions in protoplanetary disks at the time of planet formation. Using a sample of over 20,000 Kepler stars with spectroscopic metallicities from the LAMOST survey, we explore how the exoplanet population depends on host star metallicity as a function of orbital period and planet size. We find that exoplanets with orbital periods less than 10 days are preferentially found around metal-rich stars ([Fe/H] similar or equal to 0.15 +/- 0.05 dex). The occurrence rates of these hot exoplanets increases to similar to 30% for super-solar metallicity s

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Badenes, Carles, Christine Mazzola, Todd A. Thompson, et al. "Stellar Multiplicity Meets Stellar Evolution and Metallicity: The APOGEE View." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/627094.

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We use the multi-epoch radial velocities acquired by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey to perform a large-scale statistical study of stellar multiplicity for field stars in the Milky Way, spanning the evolutionary phases between the main sequence (MS) and the red clump. We show that the distribution of maximum radial velocity shifts (Delta RVmax) for APOGEE targets is a strong function of log g, with MS stars showing Delta RVmax as high as similar to 300 km s(-1), and steadily dropping down to similar to 30 km s(-1) for log g similar to 0, as stars clim

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Gáspár, András, George H. Rieke, and Nicholas Ballering. "THE CORRELATION BETWEEN METALLICITY AND DEBRIS DISK MASS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621391.

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We find that the initial dust masses in planetary debris disks are correlated with the metallicities of their central stars. We compiled a large sample of systems, including Spitzer, the Herschel DUNES and DEBRIS surveys, and WISE debris disk candidates. We also merged 33 metallicity catalogs to provide homogeneous [Fe/H] and sigma([Fe/H]) values. We analyzed this merged sample, including 222 detected disks (74 warm and 148 cold) around a total of 187 systems (some with multiple components) and 440 disks with only upper limits (125 warm and 315 cold) around a total of 360 systems. The disk dus

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22

Bolatto, Pereira Alberto D. "The interstellar medium in low metallicity environments." Thesis, Boston University, 2001. https://hdl.handle.net/2144/36768.

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Thesis (Ph.D.)--Boston University<br>PLEASE 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.<br>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

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23

Spalding, Eckhart. "A New Set of Spectroscopic Metallicity Calibrations for RR Lyrae Variable Stars." UKnowledge, 2014. http://uknowledge.uky.edu/physastron_etds/22.

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RR Lyrae stars are old, iron-poor, Helium-burning variable stars. RR Lyraes are extremely useful for tracing phase-space structures and metallicities within the galaxy because they are easy to identify, have consistent luminosities, and are found in large numbers in the galactic disk, bulge, and halo. Here we present a new set of spectroscopic metallicity calibrations that use the equivalent widths of the Ca II K, Hγ, and Hδ lines to calculate metallicity values. Applied to spectroscopic survey data, these calibrations will help shed light on the evolution of the Milky Way and other galaxies.

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24

Santucci, 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/.

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Tudo que vive por muito tempo está apto a contribuir com boas histórias sobre o passado. Isto não é diferente com as estrelas azuis tardias que são encontradas em todos os ambientes estelares. Essas estrelas velhas mostram-se aparentemente muito jovens, e talvez por isso, nunca tenham sido ouvidas em um contexto maior que suas próprias vidas. Este trabalho interpreta a história que elas contam sobre a natureza do halo galáctico, através de seus parâmetros físicos fundamentais: coordenadas, temperaturas, gravidades superficiais, metalicidades, cores, distâncias e idades. Este trabalho utiliz

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25

Alves, Cruz Monique [Verfasser], and 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.

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26

de, Koter A., J. S. Vink, and 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/.

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We present the latest results on the observational dependence of the mass-loss rate in stellar winds of O and early-B stars on the metal content of their atmospheres, and compare these with predictions. Absolute empirical rates for the mass loss of stars brighter than 10$^{5.2} L_{odot}$, based on H$alpha$ and ultraviolet (UV) wind lines, are found to be about a factor of two higher than predictions. If this difference is attributed to inhomogeneities in the wind this would imply that luminous O and early-B stars have clumping factors in their H$alpha$ and UV line forming regime of about a fac

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Santucci, 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/.

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As estrelas azuis tardias (blue straggler stars ou estrelas BS) são estrelas de sequência principal que apresentam um aparente atraso evolutivo em relação às suas vizinhanças. Elas foram identificadas inicialmente na sequência principal de aglomerados globulares acima do ponto de turnoff no diagrama HR. Desde então, têm sido encontradas em todos os ambientes estelares: aglomerados abertos e globulares, galáxias anãs próximas e entre as estrelas de campo na Galáxia. O principal objetivo deste trabalho é construir uma grande amostra de estrelas BS no campo galáctico. Para tanto, métodos de sepa

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28

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/.

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Asymptotic Giant Branch (AGB) stars and red supergiants (RSGs) are some of the largest contributors of dust and material back to the Universe. While a substantial amount of RSG dust will be destroyed by the subsequent supernova, the dust from AGB stars will be injected into the Interstellar Medium. Understanding the contribution of these stars and how it is affected by changes in stellar parameters is critically important to determining stellar lifetimes, constraining stellar models, and understanding the evolutionary paths of core-collapse progenitors and their subsequent supernova. This stud

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Young, 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.

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30

Cormier, Diane. "The physical properties in the interstellar medium of low-metallicity dwarf galaxies." Paris 7, 2012. http://www.theses.fr/2012PA077193.

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Les galaxies naines locales à formation d'étoiles sont des laboratoires idéaux pour analyser les processus de formation d'étoiles à faible métallicité et le rôle de l'enrichissement en métaux sur les conditions physiques et, plus généralement, l'évolution des galaxies. Mon travail de thèse concerne l'étude des propriétés du gaz dans les galaxies naines du "The Herschel Dwarf Galaxy Survey", combinant observations et modélisation. J'ai examiné le rôle des traceurs les plus importants du milieu interstellaire (MIS) multi phases, de l'infrarouge moyen au submillimétrique. Je me suis particulièrem

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31

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.

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During my Ph.D. study, I have been concentrating on the evolutionary tracks and atmosphere models of very low mass stars (VLMSs; ∼ 0.1 − 0.6 Msun) and very massive stars (VMSs; ∼ 12−350 Msun), based on the PAdova-TRieste Stellar Evolution Code (PARSEC). For the very low mass models, it appeared that the previous models computed with PARSEC were unable to correctly predict some basic observational relations. These relations include the mass–radius relation and the colour-magnitude relations of cool dwarfs. We replace the approximate boundary conditions used in PARSEC with those provided by more

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32

Schlesinger, 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.

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33

Pineda, John Sebastian. "Activity and kinematics of low mass stars." Thesis, Massachusetts Institute of Technology, 2010. http://hdl.handle.net/1721.1/61260.

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Thesis (S.B.)--Massachusetts Institute of Technology, Dept. of Physics, 2010.<br>Cataloged from PDF version of thesis.<br>Includes bibliographical references (p. 95-96).<br>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 measure

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34

Rainger, Paul P. "Studies of low-mass interacting binary stars." Thesis, University of St Andrews, 1990. http://hdl.handle.net/10023/14369.

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Spectroscopic and photometric observations of eight contact/near-contact binaries are presented and analysed. Spectroscopic observations were obtained at 4200 Å (radial velocity spectra) and 6563 Å (hydrogen-alpha line profiles). New photometric observations were obtained at visual and infrared wavelengths, and other previously published light curves are also re-analysed. Absolute dimensions have been obtained for five systems; TY Boo, VW Boo, BX And, SS Ari and AG Vir, and their evolutionary positions discussed. Four of the systems are found to be in marginal but poor thermal contact, exhib

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35

Mendes, Luiz Themystokliz Sanctos. "Evolutionary models of rotating low mass stars." Universidade Federal de Minas Gerais, 1999. http://hdl.handle.net/1843/BUOS-9GGP5S.

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We have investigated the combined effects of rotation and internal ngular momentum redistribution on the structure and evolution of low mass tars, from the pre-main sequence to the main sequence phase. As a tool for that study, the ATON stellar evolutionary code (Mazzitelli 1989; Ventura et al. 1998) has been modified in order to include those effects. Rotation as implemented according to the equipotential technique developed by Kippenhahn and Thomas (1970) and later improved by Endal and Sofia (1976). Angular momentum redistribution in radiative regions was modeled through an advection-diffus

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36

Dopcke, Gustavo [Verfasser], and 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.

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Kumari, Nimisha. "Spatially-resolved studies of nearby star-forming galaxies." Thesis, University of Cambridge, 2018. https://www.repository.cam.ac.uk/handle/1810/283605.

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Spatially-resolved studies of nearby star-forming galaxies are essential to understand various physical and chemical phenomena at play in the interstellar medium in the galaxies, and consequently to obtain a comprehensive picture of galaxy formation and evolution. In this thesis, I perform spatially-resolved analyses of chemical abundances and star-formation in nearby star-forming galaxies - blue compact dwarf galaxies (BCDs) and spiral galaxies. I map various properties of H II regions and the surrounding gas within three BCDs, using integral field spectroscopic (IFS) data from the Gemini Mul

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Cossburn, Martin R. "The study of low-mass stars and brown dwarfs." Thesis, University of Leicester, 1999. http://hdl.handle.net/2381/30616.

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This thesis describes the search for brown dwarfs in open clusters using optical and infrared photometry, optical spectroscopy and surveys using the Hubble Space Telescope (HST). It also includes an observational study of very low-mass stars (VLMS) using a filter combination (I and Z), unused previously in this field enabling the calibration of the colour (I--Z), for future survey work. Following a short introduction explaining the reasons for studying brown dwarfs this thesis reviews the theory of their formation and evolution and describes recent searches for brown dwarfs and their results.

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Pinfield, David J. "Low mass stars and brown dwarfs in open clusters." Thesis, University of Leicester, 1998. http://hdl.handle.net/2381/30612.

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This thesis describes several open cluster searches for very low mass stars (VLM) and brown dwarfs (BD) (M/M? < 0.08). With recent developments in charged coupled devices, it has become possible to survey open clusters to well into the BD regime. The principal aim of this work is to employ these new instruments to conduct such open cluster surveys, to investigate the properties of VLM and BD populations. The thesis begins with a short introduction, which describes the fundamental properties of brown dwarfs, relates research in this field to other areas of astronomy, and summarises the project

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Kenyon, Michael John. "Low mass stars and brown dwarfs around Ïƒ Orionis." Thesis, Keele University, 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.409546.

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Lehner, 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.

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Pokorny, 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.

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Brown, 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.

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Quanz, 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.

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Ziegerer, Eva [Verfasser], and 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.

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Birkby, 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.

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Saylor, Dicy, Sebastien Lepine, Ian Crossfield, and 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.

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The K2 mission is targeting large numbers of nearby (d < 100 pc) GKM dwarfs selected from the SUPERBLINK proper motion survey (mu > 40 mas yr(-1), V < 20). Additionally, the mission is targeting low-mass, high proper motion stars associated with the local (d < 500 pc) Galactic halo population also selected from SUPERBLINK. K2 campaigns 0 through 8 monitored a total of 26,518 of these cool main-sequence stars. We used the auto-correlation function to search for fast rotators by identifying short-period photometric modulations in the K2 light curves. We identified 481 candidate fast rotators wit

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Covey, 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.

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Szigeti, László, Szabolcs Mészáros, Verne V. Smith, et al. "12C/13C isotopic ratios in red-giant stars of the open cluster NGC 6791." OXFORD UNIV PRESS, 2018. http://hdl.handle.net/10150/627135.

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Abstract:

Carbon isotope ratios, along with carbon and nitrogen abundances, are derived in a sample of 11 red-giant members of one of the most metal-rich clusters in the Milky Way, NGC 6791. The selected red-giants have a mean metallicity and standard deviation of [Fe/H] = +0.39 +/- 0.06 (Cunha et al. 2015). We used high-resolution H-band spectra obtained by the SDSS-IV Apache Point Observatory Galactic Evolution Experiment. The advantage of using high-resolution spectra in the H band is that lines of CO are well represented and their line profiles are sensitive to the variation of C-12/C-13. Values of

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Cuadrado, 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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