Dissertations / Theses on the topic 'Stars – Initial mass function'
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Bressert, Eli Walter. "The initial distribution of stars." Thesis, University of Exeter, 2012. http://hdl.handle.net/10036/3890.
Full textThompson, Simon. "Low mass stars, brown dwarfs and the initial mass function in Cepheus OB3b." Thesis, Keele University, 2002. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.288434.
Full textLuhman, Kevin Lee 1971. "Low-mass star formation and the initial mass function in young clusters." Diss., The University of Arizona, 1998. http://hdl.handle.net/10150/288884.
Full textSelman, Fernando Javier Scoville Nicholas Zabriskie. "The initial mass function and star-formation history in the 30 Doradus super-association /." Diss., Pasadena, Calif. : California Institute of Technology, 2004. http://resolver.caltech.edu/CaltechETD:etd-05122004-130955.
Full textJones, Michael Oliver. "The role of protostellar heating in star formation." Thesis, University of Exeter, 2018. http://hdl.handle.net/10871/34560.
Full textBurgess, Andrew. "Exploration de la fonction de faible masse initiale dans les amas jeunes et les r ´egions de formation stellaire." Phd thesis, Université de Grenoble, 2010. http://tel.archives-ouvertes.fr/tel-00576460.
Full textFaimali, Alessandro Daniele. "The history and rate of star formation within the G305 complex." Thesis, University of Hertfordshire, 2013. http://hdl.handle.net/2299/13732.
Full textCanameras, R., N. P. H. Nesvadba, R. Kneissl, M. Limousin, R. Gavazzi, D. Scott, H. Dole, et al. "Planck's dusty GEMS III. A massive lensing galaxy with a bottom-heavy stellar initial mass function at z=1.5." EDP SCIENCES S A, 2017. http://hdl.handle.net/10150/624365.
Full textLyo, A.-Ran Physical Environmental & Mathematical Sciences Australian Defence Force Academy UNSW. "The nearby young [special character] Chamaeleontis cluster as a laboratory for star formation and evolution." Awarded by:University of New South Wales - Australian Defence Force Academy. School of Physical, Environmental and Mathematical Sciences, 2004. http://handle.unsw.edu.au/1959.4/38707.
Full textMor, Crespo Roger. "The star formation history and the stellar initial mass function of the Milky Way disc. The population synthesis Besançon Galaxy Model in the Gaia era." Doctoral thesis, Universitat de Barcelona, 2019. http://hdl.handle.net/10803/667482.
Full textSimon, Jacob B., Philip J. Armitage, Andrew N. Youdin, and Rixin Li. "Evidence for Universality in the Initial Planetesimal Mass Function." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626045.
Full textCovey, 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.
Full textAshworth, Greg. "Exploring the initial mass function by stochastically lighting up galaxies." Thesis, Durham University, 2018. http://etheses.dur.ac.uk/12739/.
Full textCardoso, Catia Vanessa Varejao. "Observational properties of brown dwarfs : the low-mass end of the mass function." Thesis, University of Exeter, 2012. http://hdl.handle.net/10036/3592.
Full textCatalán, Ruiz Sílvia. "Testing the initial-final mass relationship of white dwarfs." Doctoral thesis, Universitat Politècnica de Catalunya, 2008. http://hdl.handle.net/10803/6591.
Full textSince white dwarfs are long-lived objects, they also constitute useful objects to study the structure and evolution of our Galaxy. For instance, the initial-final mass relationship, which connects the final mass of a white dwarf with the initial mass of its main-sequence progenitor, is of paramount importance for different aspects in modern astrophysics. This function is used for determining the ages of globular clusters and their distances, for studying the chemical evolution of galaxies, and also to understand the properties of the Galactic population of white dwarfs. Despite its relevance, this relationship is still relatively poorly constrained.
The main aim of this thesis is the study of the initial-final mass relationship. For such purpose we have used two different approaches. From an observational perspective, the statistical significance of the current initial final mass relationship can be improved by performing spectroscopic observations of white dwarfs for which some important parameters are available. Since this approach involves the use of theoretical stellar evolutionary tracks the resulting initial-final mass relationship is, in fact, semi-empirical. In this thesis we present a promising method which consists in using common proper motion pairs comprised of a white dwarf and a FGK star. It is sound to assume that the members of the system were born simultaneously and with the same chemical composition. Moreover, these stars are well separated and it can be considered that they have evolved as isolated stars, since mass exchange between them is unlikely. Thus, a careful analysis of the observational data of both members of each pair allows us to derive the initial and final masses of the white dwarf components, something which is totally impossible when white dwarfs are isolated. Considering the new data that we have obtained with this work and the observational data currently used to define the initial-final mass relationship we have carried out a revision of this relationship, giving some clues on its dependence on different parameters, especially on metallicity.
The second approach to improve the initial-final mass relationship involves an indirect measurement, which has been carried out by studying its influence on one of the powerful tools related to the white dwarf population, the white dwarf luminosity function. We have computed a series of luminosity functions using different theoretical initial-final mass relationships, and also, considering the semi-empirical relation derived in this thesis. We have compared these computations with the available observational data in order to evaluate the validity of each of these relations.
In order to increase the statistical significance of the white dwarf luminosity function and to improve the initial-final mass relationship it is necessary to extend the amount of accurate and reliable observational data. For this reason part of the thesis is devoted to the Alhambra Survey, which is a good example of the new deep surveys currently under development. These observational projects will detect thousands of new white dwarfs, some of them belonging to common proper motion pairs, which could be eventually used to extend our analysis. Thus, we have performed an exhaustive study to optimize the identification procedure of the white dwarf candidates which will be eventually detected by the Alhambra survey.
Liebert, J., C. C. Dahn, and D. G. Monet. "Luminosity Function of White Dwarfs in the Local Disk and Halo." Steward Observatory, The University of Arizona (Tucson, Arizona), 1988. http://hdl.handle.net/10150/623908.
Full textMunn, Jeffrey A., Hugh C. Harris, Hippel Ted von, Mukremin Kilic, James W. Liebert, Kurtis A. Williams, Steven DeGennaro, et al. "A DEEP PROPER MOTION CATALOG WITHIN THE SLOAN DIGITAL SKY SURVEY FOOTPRINT. II. THE WHITE DWARF LUMINOSITY FUNCTION." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/622633.
Full textKilic, Mukremin, Jeffrey A. Munn, Hugh C. Harris, Ted von Hippel, James W. Liebert, Kurtis A. Williams, Elizabeth Jeffery, and Steven DeGennaro. "The Ages of the Thin Disk, Thick Disk, and the Halo from Nearby White Dwarfs." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623864.
Full textNelson, Katy. "On the origin of the stellar initial mass function and multiple stellar systems." Thesis, Cardiff University, 2014. http://orca.cf.ac.uk/65971/.
Full textVignola, Matteo. "Constraining the initial mass function of the giant early-type galaxies NGC 1332 and NGC 7619." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2018. http://amslaurea.unibo.it/15597/.
Full textBurke, Christopher J. "Survey for transiting extrasolar planets in stellar systems stellar and planetary content of the Open Cluster NGC 1245 /." Columbus, Ohio : Ohio State University, 2005. http://rave.ohiolink.edu/etdc/view?acc%5Fnum=osu1132168623.
Full textCanty, James Ignatius. "Investigating the properties of brown dwarfs using intermediate-resolution spectroscopy." Thesis, University of Hertfordshire, 2015. http://hdl.handle.net/2299/15194.
Full textAchitouv, Ixandra. "Halo mass function of dark matter halos : imprints of the initial matter density field and of the non-linear collapse." Paris 7, 2012. http://www.theses.fr/2012PA077245.
Full textOrsi, Maia. "Population synthesis models for IMF studies." Thesis, Liverpool John Moores University, 2014. http://researchonline.ljmu.ac.uk/4525/.
Full textDrass, Holger [Verfasser], Rolf [Gutachter] Chini, and Susanne [Gutachter] Hüttemeister. "The substellar initial mass function of the Orion Nebula cluster / Holger Drass ; Gutachter: Rolf Chini, Susanne Hüttemeister ; Fakultät für Physik und Astronomie." Bochum : Ruhr-Universität Bochum, 2014. http://d-nb.info/1207543152/34.
Full textSmith, Rowan Johnston. "The earliest fragmentation in molecular clouds : and its connection to star formation." Thesis, University of St Andrews, 2010. http://hdl.handle.net/10023/929.
Full textLee, Yueh-Ning. "Formation and fragmentation of stellar proto-clusters." Thesis, Sorbonne Paris Cité, 2017. http://www.theses.fr/2017USPCC152/document.
Full textStars are building blocks of the Universe. They emit energy in form of light and make the material in the night sky visible. They are the elementary constituents of galaxies, determining their evolution and dynamics. On the other hand, stars are the hosts o planetary systems. The debris disc around a new-born star eventually cools down and form planets. The characteristic of the planetary system, essentially the mass of the central star, plays a major role in the formation of living being on planets. The formation of stars often occur in a clusters manner, and one of the important issues constantly under debate is the distribution of the mass of newly-born stars. This thesis is aimed to understand the Initial Mass Function which seems to be universal among different environments.This manuscripts comprises two introductory chapters on the physics of star formation and the numerical methods, respectively. Three following chapters present the projets carried out during the thesis: formation of proto-clusters, effects of initial condition in the molecular cloud, and the formation of prestellar cores from filament fragmentation, all followed by published journal articles. The last chapter concludes the manuscript and discuss the perspectives
Prichard, Laura Jane. "The evolution of early-type galaxies." Thesis, University of Oxford, 2018. http://ora.ox.ac.uk/objects/uuid:35fbf5c7-76de-4179-8e68-032ba8b5f3ee.
Full textKhorrami, Zeinab. "Imagerie à haute résolution des amas R136 et NGC3603 dévoilent la nature de leurs populations stellaires." Thesis, Nice, 2016. http://www.theses.fr/2016NICE4030/document.
Full textThis thesis aims at studying 2 massive clusters NGC3603 and R136, and the mechanisms that govern their physics, These clusters host the most massive stars known in the local universe so far and are important clues to understand the formation and fate of very massive star clusters. The manuscript outlines the photometric analysis of the core of R136 and NGC3603 on the basis of HST data in the visible and the VLT high dynamic imaging that I obtained in the infrared thanks to the SPHERE focal instrument operated since 2015 and its extreme Adaptive Optics, In an extensive photometric study of these data I discovered a significantly larger number of faint low-mass stars in the core of both these clusters compared to previous works. These stars are often detected in the vicinity of known massive bright objects. By comparing HST and SPHERE measures, NGC3603 does not show any signature of mass segregation in its core since the MF slope of the very core and the next radial bin are similarly flat and agree well with the MF found in previous works of the outer regions. On the other hand R136 is partially resolved using the SPHERE/IRDIS mode with most of the massive stars having visual companions. Considering the spectroscopic and photometric errors on the extinction and the age of cluster members, I estimate a mass range for each detected star. The MF is plotted at different ages with given errors on stellar masses. Finally I demonstrate that we need more resolution to go further on studying R136 which is 7-8 times further than NGC3603
Hill, David T. "The optical and NIR luminous energy output of the Universe : the creation and utilisation of a 9 waveband consistent sample of galaxies using UKIDSS and SDSS observations with the GAMA and MGC spectroscopic datasets." Thesis, University of St Andrews, 2011. http://hdl.handle.net/10023/1696.
Full textSelman, Fernando Javier. "The Initial Mass Function and Star-Formation History in the 30 Doradus Super-Association." Thesis, 2004. https://thesis.library.caltech.edu/1748/2/fselman_phdthesis.pdf.
Full textSadavoy, Sarah I. "The mass distribution of protostellar and starless cores in Gould Belt clouds." Thesis, 2009. http://hdl.handle.net/1828/1611.
Full textDufour, Pierre. "Étude spectroscopique d'étoiles naines blanches riches en hélium de type DB et DBA." Thèse, 2009. http://hdl.handle.net/1866/3460.
Full textNew model atmospheres are presented, including improved neutral helium lines from Beauchamp (1995) and the occupation probability formalism for that atom. These models are used to compute a grid of synthetic spectra for helium rich atmospheres with different hydrogen abundances. This grid is used to determine the principal atmospheric parameters of the stars in our sample, e.g. effective temperature, surface gravity and hydrogen abundance. There are 102 high quality spectra of helium-rich white dwarfs in our sample, making it the largest sample of this kind. 29 of these spectra were observed for this project. Synthetic spectra using different values of the α parameter from the mixing length theory have been calculated in order to determine the correct value of this parameter for DB model atmospheres. Finally, we have computed the mass distribution of our sample and the DB luminosity funtion. The mass distribution shows a clear cutoff at 0.5 solar masses which is predicted by stellar evolution theory and gives a significantly higher mean mass for the DBA stars of the sample. However, the global mean mass of our sample is very close to that of DA stars. With our luminosity function, we found a number ratio of DB stars over DA stars of about 25%.