Browsing by Title
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Senić, Aleksandra (MATEMATIČKI FAKULTET UNIVERZITETA U BEOGRADU , 2010)[more][less]
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Marković, Ana (Beograd , 2017)[more][less]
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Momirović, Miloš (Beograd , 2018)[more][less]
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Tepavčević, Andreja (Novi Sad)[more][less]
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Dimitrijević, S. Milan (Astronomical Observatory Belgrade , 2008)[more][less]
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Dimitrijević, M.; Csillag, L. (JOURNAL OF APPLIED SPECTROSCOPY , 2006)[more][less]
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Popović, Luka Č. (Astronomical Observatory Belgrade , 2008)[more][less]
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Dimitrijević, Milan; Popović, Luka (MDPI , 2020)[more][less]
URI: http://hdl.handle.net/123456789/5444 Files in this item: 1
Spectral_Line_S ... ics_and_Related_Topics.pdf ( 4.595Mb ) -
Simić, Saša; Popović, Luka Č. (Nenad Milovanović & Milan S. Dimitrijević, Astronomical Observatory, Belgrade , 2007)[more][less]
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Ilić, D.; Stavrev, K.; Tsvetkova, K.; Tsvetkov, M.; Popović, L. Č. (Astron. Soc. 'Rudjer Bošković' , 2005)[more][less]
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Popović, Luka Č.; Kovačević, Jelena; Ilić, Dragana (Astr. Soc. "Rudjer Bošković" , 2009)[more][less]
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Min'ko, L. Ya.; Avramenko, V. B.; Bakanovich, G. I.; Chumakov, A. N. (Obs. Astron. Belgrade , 1995)[more][less]
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Arazimova, Eva; Kawka, Adela; Stephane, Vennus (Astronomical Observatory Belgrade , 2008)[more][less]
URI: http://hdl.handle.net/123456789/1552 Files in this item: 2
Arazimova.pdf ( 640.4Kb )Arazimova.pdf ( 640.4Kb ) -
Bulatović, Jelena (Belgrade)[more][less]
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Cvetković, Dragoš (Beograd , 2012)[more][less]
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Stojisavljević, Vukašin (Beograd , 2015)[more][less]
URI: http://hdl.handle.net/123456789/4228 Files in this item: 1
Stojisavljevic_Vukasin.pdf ( 1.020Mb ) -
Borovićanin, Bojana (Kragujevac, Serbia , 2008)[more][less]
Abstract: Different spectral characterizations of certain classes of graphs are considered in this dissertation. The large number of papers concerning this topic, indicates that problems of this kind are very interesting in spectral graph theory. This dissertation, beside Preface and References with 46 items, consists of two chapters: 1. Harmonic graphs, 2. Graphs with maximal index. Harmonic graphs are introduced and studied in details in Chapter 1. This chapter consists of four sections. In section 1.1 the definition of harmonic graphs, as well as their basic properties, are given. Harmonic trees are discussed in section 1.2. In section 1.3 we characterize harmonic graphs with small number of cycles; in particular, all unicyclic, bicyclic, tricyclic and tetracyclic graphs are determined. Finally, in section 1.4, we determine all connected 3-harmonic graphs with integral spectrum. The solution of maximal index problem in certain classes of graphs is given in Chapter 2. This chapter consists of four sections. In sections 2.1 and 2.2 we review some results related to the index of a graph. The emphasis is on graphs with given number of both vertices and edges; in particular we discuss graphs having the fixed number of pendant edges, too. In section 2.3 we give the solution of maximal index problem in the class of connected tricyclic graphs with n vertices and k pendant edges. Finally, in section 2.4, we determine graphs with maximal index among all connected cactuses with n vertices. URI: http://hdl.handle.net/123456789/1834 Files in this item: 1
disertacija_Bojana Borovicanin.pdf ( 1.939Mb ) -
Jovanović, Irena (Beograd , 2014)[more][less]
Abstract: Spectral graph theory is a mathematical theory where graphs are considered by means of the eigenvalues and the corresponding eigenvectors of the matrices that are assigned to them. The spectral recognition problems are of particular interest. Between them we can distinguish: characterizations of graphs with a given spectrum, exact or approximate constructions of graphs with a given spectrum, similarity of graphs and perturbations of graphs. In this dissertation we are primarily interested for the similarity of graphs, where graphs with the same number of vertices and graphs of different orders are considered. Similarity of graphs of equal orders can be established by computation of the spectral distances between them, while for graphs with different number of vertices the measures of similarity are introduced. In that case, graphs under study are usually very large and they are denoted as networks, while the measures of similarity can be spectraly based. Some mathematical results on the Manhattan spectral distance of graphs based on the adjacency matrix, Laplacian and signless Laplacian matrix are given in this dissertation. A new measure of similarity for the vertices of the networks under study is proposed. It is based on the difference of the generating functions for the numbers of closed walks in the vertices of networks. These closed walks are calculated according to the new spectral formula which enumerates the numbers of spanning closed walks in the graphlets of the corresponding graphs. The problem of the characterization of a digraph with respect to the spectrum of AAT , apropos ATA, where A is the adjacency matrix of a digraph, is introduced. The notion of cospectrality is generalized, and so the cospectrality between some particular digraphs with respect to the matrix AAT and multigraphs with respect to the signless Laplacian matrix is considered. URI: http://hdl.handle.net/123456789/4233 Files in this item: 1
Jovanović_Irena.pdf ( 1.138Mb ) -
Lalović, Ana (Beograd , 2016)[more][less]
Abstract: The goal of this thesis is to reduce multidimensional space of galactic properties to the smallest number of dimensions su cient to describe them. For this purpose, the statistical analysis is applied over the parameters that describe fundamental galactic properties on the morphologically representative sample of 2180 galaxies. The sample of galaxies used in this thesis is based on the Arecibo Legacy Fast ALFA (Alfalfa) blind HI survey. The importance of an HI blind survey lies in the fact that galaxies are chosen on the basis of their gas content (HI) solely, thus free of optical selection e ects. From the initial sample counting 10000 galaxies, 2180 of them were chosen, since for this subsample the optical spectroscopy from the Sloan Digital Sky Survey (SDSS) was available and moreover the photometry in the UV (Galaxy Evolution Explorer, GALEX), and optical (SDSS) to the near-infrared (Two Micron All Sky Survey, 2MASS). Parameters are selected according to the previously established correlations between fundamental galactic properties, relying on the previous work. They are extensively tested and confronted between each other to be chosen from the larger parametric space. To select parameters, we rst measured stellar kinematics using publicly available code (pPXF), and tested both empirical and synthetic stellar libraries. In particular, we have measured the velocity dispersion and the higher moments of the line-of-sight velocity distribution function. This is the largest galaxy sample created so far with detailed stellar kinematics measured including higher moments of the line-of-sight velocity distribution function. The sample size allows statistical tests to be applied to the higher moment of the velocity distribution function (h4), with respect to the di erent groups of morphological galaxy types. Various tests agree with the previous indication that elliptical and lenticular galaxies have the same origin. Further, we have measured the line strength indices for several absorption lines (Lick indices), since some of them are good proxies to galaxy ages and metallicity, also the fundamental galactic properties. In the nal statistical analysis, metallicity proves to be of no importance, but the inclusion of galaxy ages in the analysis, the results change signi cantly. The last step in the parameter selection is the modelling of the galaxies' surface brightness pro les with the Sersic pro le, that is performed in this thesis with the Gal t code. The velocity dispersion measured, along with the Sersic index and effective radius of the Sersic pro le takes the role in the dynamical mass calculation, being the fundamental galactic property and hence used in the nal statistical analysis. Finally, we have taken the mass of the gas component and maximal rotational velocity from the radio-spectroscopy and Kron magnitudes (i.e. colours) from the ultraviolet/ optical/nearinfrared photometry (GALEX/SDSS/2MASS databases). After extensive testing, we have chosen the colour calculated from ultraviolet and optical magnitudes (NUV r colour), for the nal statistical analysis. It is worth noting that previous analysis of the galactic properties lack velocity dispersion, as well as the colour with the ultraviolet component, although it is a direct proxy to the speci c star formation rate in the galaxy. This particular colour makes correlations among analysed parameters stronger and proves to be more important than optical colours. Finally, when the proper parametric space of galactic properties is formed (velocity dispersion, colour, luminosity, Petrosian radii R50 and R90, dynamical, HI and stellar masses, maximal rotational velocity and the galaxy ages), the correlation analysis is performed to inspect correlations between parameters. This analysis con rms relations that are already known to hold. Then the principal component analysis is done with the purpose of nding and identifying the smallest number of galactic properties responsible for the nal products of galaxy evolution, as we see today, in the local Universe. The results of the corresponding analysis are the following: there are at least three statistically important, independent components. The rst and the most important component cannot be identi ed with either galactic property, but presents the mixture of several properties: dynamical mass, mass of the stellar and gas component, luminosity and Petrosian radii R50 and R90. Relaying on the previous work, this component may be identi ed with the "size" of the galaxies. The second component, mostly in uenced by the galactic colour, may be identi ed with the "aspect" of the galaxies. The colour was not found to be important in previous work. The galaxy ages can be identi ed with the third principal component. There is a hint on the fourth component, dominated by the maximal rotational velocity that can be identi ed with the speci c angular momentum of galaxies. Although not proven to be statistically important, it may become so in the larger sample of galaxies which will provide the information of the true peak of the galaxies' rotational curves, since the single-beam HI spectra may show the single maximum and this may not be the true maximum. Also, the rotational velocity includes the inclination correction, another questionable parameter in the analysis. To conclude: there are at least three, and possibly four dimensions of the multidimensional galactic space, as we see today. URI: http://hdl.handle.net/123456789/4446 Files in this item: 1
Lalovic_Ana3.pdf ( 11.44Mb ) -
Popović, Č. Luka; Kovačević, Jelena; Ilić, Dragana (Astr. Soc. "Rudjer Bošković"2 , 2008)[more][less]