Auflistung Astronomy and Geoscience nach Titel
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Jovanović, Milena (Beograd , 2021)[more][less]
Zusammenfassung: The subject of this thesis is a precise determination of the Baryonic Mass Func- tion (BMF) for a representative sample of nearby galaxies, where BMF stands for the distribution of the galaxies’ baryonic masses. Detailed dynamical models were derived for a sample of galaxies based on the publicly available THINGS (The HI Nearby Galaxy Survey) survey, based on the the 21 cm emission line of atomic hydrogen hi. THINGS rotation curves, that reflect dynamical mass, were fitted by the sum of the contributions from the stellar component, neutral atomic gas, and dark matter for 20 THINGS galaxies. The mass of stellar components is measured from the Spitzer photometry in the 3.6 μm band, while the amount of atomic gas is derived directly from the radio observations in THINGS. For the assumed dark matter dis- tribution we used the observationally motivated pseudo-isothermal profile (ISO) and the Navarro-Frenk-White (NFW) profile based on the ΛCDM cosmological model. Dynamical modeling of the total mass was performed with free scaling of the stellar component contribution (mass-to-light ratio, M/L), and also with the same parameter fixed on a value consistent with stellar evolution population models. Con- vergence of the fitting procedure was reached for all the dynamical models with the free mass-to-light ratio, while the modeling with the fixed ratio was successful for 16 objects. The mass of the stellar component, gas, dark matter, baryonic, and total mass, were derived for the sample of galaxies and the aforementioned four sets of dynamical models (two dark matter models with both free and fixed M/L values). The total BMF is constructed by summing the masses of the baryonic compo- nents (stars and gas) for galaxies in the given range of galactic masses. Furthermore, we discuss how typical our Galactic neighborhood and our Galaxy, the Milky Way, as a giant spiral, are in terms of component masses and their place on the global (and local) BMF. URI: http://hdl.handle.net/123456789/5244 Dateien zu dieser Ressource: 1
Doktorska_disertacija_Jovanovic_Milena.pdf ( 14.28Mb ) -
Jurković, Monika (, 2019)[more][less]
Zusammenfassung: The subject of this PhD thesis are Type II Cepheids. Type II Cepheids are pulsating Population II stars with masses of around 0.5 0.6 M⊙. Their mass determines where they are positioned on the Hertzsprung-Russell diagram (HRD), that is, their luminosity and eective temperature. These stars can be found in the Milky Way, the Magellanic Clouds, and in other distant galaxies. They occupy a narrow strip on the HRD which is called the instability strip. Here the radii and luminosity change periodically, and this change can be seen in the light curves. Because of their age, and their position on the HRD, these variables form a separate period-luminosity relation (PL relation). Using the spectral energy distribution models we determined in this thesis the eective temperatures and luminosities, and from evolutionary models the masses and radii, for Type II Cepheids and anomalous Cepheids in the Large and Small Magellanic Clouds. In the thesis, the rst period- luminosity relation was constructed using bolometric magnitude (Mbol). The thesis also presents the reclassication of Type II Cepheids from the Milky Way using the Fourier decomposition of the light curves measured in V lter. The Fourier decomposition was used to calculate the Fourier parameters, which were then used to compare the stars from the Milky Way with the sample of known Type II Cepheids and anomalous Cepheids from the OGLE-III catalogue for the Large Magellanic Cloud. From the 59 stars (taken from the General Catalogue of Variable Stars), 18 turned out to be anomalous Cepheids, 1 anomalous Cepheid pulsating in the rst overtone, 11 classical Cepheids, 2 peculiar W Virginis stars or classical Cepheids, and 7 were found not to be pulsating stars at all. URI: http://hdl.handle.net/123456789/4760 Dateien zu dieser Ressource: 1
Jurkovic_Monika.dok.dis.pdf ( 15.79Mb ) -
Jovanović, Bora (Beograd , 2014)[more][less]
Zusammenfassung: Одређивање разлике динамичког и светског времена и предвиђање промена у брзини Земљине ротације Апстракт Проблем прецизног предвиђања Земљине просторне оријентације је у директној вези са познавањем будућих вредности параметара Земљине ротациеј, помоћу којих се врше трансформације између небеског и терестричког система. Ти параметри су зависни од мноштва астрономских и геофизичких узрока, за чије збирно дејство још увек не постоје одговарајући теоријски модели, који би могли довољно прецизно да описују промене Земљине оријентације. Зато се предикције параметара Земљине ротације мање ослањају на геофизичке теорије, а више на математичка моделирања, која су заснована на разним нумеричким методама. Овај рад је имао за циљ да докаже да је искључиво математичким приступом(без коришћења геофизичких модела и корекција) могуће постићи унапређења у предвиђањима неравномерности скале светског времена UT1. Познато је да тај параметар има најбржу и највећу промену, јер у потпуности пресликава Земљину ротацију са свим њеним неравномерностима. Због чега његове предикције имају најмању тачност. У раду је коришћена оригинална нумеричка метода за извођење апроксимативних функција у облику суме хармоника и експоненцијала(HE). На основу реалних података рађене су предикције за 10 дана, 30 дана и 500 дана у непрекидном периоду од годину и по дана. Додатно, приказани су и, до сада остварени, резултати једне дуговремене предикције која је истим начином урађена раније. Сопствени резултати су упоређивани са одговарајућим резултатима других аутора, који су користили разне друге методе предикције, током реализације међународног пројекта “Earth Orientation Parameters Prediction Comparison Campaign”(EOPPCC). Показало се да HE метод даје сличне резултате као и друге методе када се ради о 10- дневним и 30-дневним предикцијама, али у случају 500 дневних предикција дао је убедљиво најбољи резултат. Да је овај метод заиста погодан за предикције на дужим временским интервалима, приказују и до сада (8 година) остварени резултати једне 10- годишње предикције. Може се закључити да је предикцију величине ΔТ, која се публикује у астрономским годишњацима, могуће знатно унапредити, коришћењем HE метода. Кључне речи: Време, светско време, терестричко време, референтни системи Научна област: Астрономија Ужа научна област: Земљина ротација УДК: 521.933:519:65(043.3) URI: http://hdl.handle.net/123456789/3508 Dateien zu dieser Ressource: 1
jovanovic_bora.pdf ( 11.69Mb ) -
Jurković, Monika (Beograd , 2018)[more][less]
Zusammenfassung: The sub ject of this PhD thesis are Typ e I I Cepheids. Typ e I I Cepheids are pulsating Population I I stars with masses of around 0.5 0.6 M ⊙ . Their mass determines where they are p ositioned on the Hertzsprung-Russell diagram (HRD), that is, their luminosity and e ective temp erature. These stars can b e found in the Milky Way, the Magellanic Clouds, and in other distant galaxies. They o ccupy a narrow strip on the HRD which is called the instability strip. Here the radii and luminosity change p erio dically, and this change can b e seen in the light curves. Because of their age, and their p osition on the HRD, these variables form a separate p erio d-luminosity relation ( P L relation). Using the sp ectral energy distribution mo dels we determined in this thesis the e ective temp eratures and luminosities, and from evolutionary mo dels the masses and radii, for Typ e I I Cepheids and anomalous Cepheids in the Large and Small Magellanic Clouds. In the thesis, the rst p erio d- luminosity relation was constructed using b olometric magnitude ( M b ol ). The thesis also presents the reclassi cation of Typ e I I Cepheids from the Milky Way using the Fourier decomp osition of the light curves measured in V lter. The Fourier decomp osition was used to calculate the Fourier parameters, which were then used to compare the stars from the Milky Way with the sample of known Typ e I I Cepheids and anomalous Cepheids from the OGLE-I I I catalogue for the Large Magellanic Cloud. From the 59 stars (taken from the General Catalogue of Variable Stars), 18 turned out to b e anomalous Cepheids, 1 anomalous Cepheid pulsating in the rst overtone, 11 classical Cepheids, 2 p eculiar W Virginis stars or classical Cepheids, and 7 were found not to b e pulsating stars at all. URI: http://hdl.handle.net/123456789/4751 Dateien zu dieser Ressource: 1
Jurkovic_Monika.dok.dis.pdf ( 15.79Mb ) -
Vučetić, Milica (Beograd , 2017)[more][less]
Zusammenfassung: In this dissertation we discuss in uence of H emission from supernova remnants (SNRs) on H derived star formation rates (SFRs). We present the detection of 16 optical SNR candidates in a part of nearby spiral galaxy IC342, and two more poten- tial SNRs in NGC 185 galaxy. The candidates were detected by applying [S ii]/H ratio criterion on observations made with the 2 m telescope at Rozhen National Astronomical Observatory in Bulgaria. Also, in this dissertation we present the most up-to-date list of nearby galaxies with optically detected SNRs. When deri- ving H star formation rates, assumption is that the radiation is coming from the ionized gas surrounding hot and young stars { Hii regions. In this case, emission from SNRs contaminates H ux used to derive SFR. We found that the contribu- tion of SNRs' ux to the total H ux, for 18 galaxies in our sample of galaxies with optical SNRs, is 5 5%. Due to the observational selection effects, the SNR contamination of SFRs derived herein represents only a lower limit. M83 is the galaxy with the most detected optical SNRs and in this galaxy SNRs account for 9 per cent of the total H emission. We expect that fraction similar to this would be close to the real contribution of SNR emission to the total H emission in spiral galaxies. Using two dwarf galaxies as an example, Holmberg IX and NGC 185, we show that the contamination of H ux by SNRs, or other sources, can be much larger, up to ten times higher than total H ux coming from Hii regions of the observed galaxy. URI: http://hdl.handle.net/123456789/4501 Dateien zu dieser Ressource: 1
Milica_disertacija_21.03.2017.pdf ( 26.28Mb ) -
Vučetić, Milica (Beograd , 2017)[more][less]
Zusammenfassung: In this dissertation we discuss in uence of H emission from supernova remnants (SNRs) on H derived star formation rates (SFRs). We present the detection of 16 optical SNR candidates in a part of nearby spiral galaxy IC342, and two more poten- tial SNRs in NGC 185 galaxy. The candidates were detected by applying [S ii]/H ratio criterion on observations made with the 2 m telescope at Rozhen National Astronomical Observatory in Bulgaria. Also, in this dissertation we present the most up-to-date list of nearby galaxies with optically detected SNRs. When deri- ving H star formation rates, assumption is that the radiation is coming from the ionized gas surrounding hot and young stars { Hii regions. In this case, emission from SNRs contaminates H ux used to derive SFR. We found that the contribu- tion of SNRs' ux to the total H ux, for 18 galaxies in our sample of galaxies with optical SNRs, is 5 5%. Due to the observational selection effects, the SNR contamination of SFRs derived herein represents only a lower limit. M83 is the galaxy with the most detected optical SNRs and in this galaxy SNRs account for 9 per cent of the total H emission. We expect that fraction similar to this would be close to the real contribution of SNR emission to the total H emission in spiral galaxies. Using two dwarf galaxies as an example, Holmberg IX and NGC 185, we show that the contamination of H ux by SNRs, or other sources, can be much larger, up to ten times higher than total H ux coming from Hii regions of the observed galaxy. URI: http://hdl.handle.net/123456789/4507 Dateien zu dieser Ressource: 1
Milica_disertacija_21.03.2017.pdf ( 26.28Mb ) -
Milogradov-Turin, Jelena (Belgrade)[more][less]
URI: http://hdl.handle.net/123456789/126 Dateien zu dieser Ressource: 1
phdJelenaMilogradovTurin.pdf ( 115.3Mb ) -
Ševarlić, Branislav (Belgrade)[more][less]
URI: http://hdl.handle.net/123456789/141 Dateien zu dieser Ressource: 1
phdBranislavMSevarlic.pdf ( 5.662Mb ) -
Teleki, Đorđe (Belgrade , 1964)[more][less]
URI: http://hdl.handle.net/123456789/228 Dateien zu dieser Ressource: 1
phdDjordjeTeleki.pdf ( 4.541Mb ) -
Šegan, Stevo (Belgrade , 1987)[more][less]
URI: http://hdl.handle.net/123456789/360 Dateien zu dieser Ressource: 1
phdStevoSegan.pdf ( 8.557Mb ) -
Đurović, Dragutin (Belgrade)[more][less]
URI: http://hdl.handle.net/123456789/324 Dateien zu dieser Ressource: 1
phdDragutinDjurovic.pdf ( 4.035Mb ) -
Ninković, Slobodan (Belgrade)[more][less]
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Kuzmanoski, Mike (Belgrade)[more][less]
URI: http://hdl.handle.net/123456789/128 Dateien zu dieser Ressource: 1
phdMikeKuzmanoski.pdf ( 14.21Mb ) -
Đurašević, Gojko (Belgrade)[more][less]
URI: http://hdl.handle.net/123456789/124 Dateien zu dieser Ressource: 1
phdGojkoDjurasevic.pdf ( 34.72Mb ) -
Atanacković-Vukmanović, Olga (Belgrade)[more][less]
URI: http://hdl.handle.net/123456789/129 Dateien zu dieser Ressource: 1
phdOlgaAtanackovic.pdf ( 24.18Mb ) -
Angelov, Trajče (Belgrade , 1980)[more][less]
URI: http://hdl.handle.net/123456789/364 Dateien zu dieser Ressource: 1
phdTrajceAngelov.pdf ( 4.280Mb ) -
Oskanjan, Vasilije (Belgrade)[more][less]
URI: http://hdl.handle.net/123456789/131 Dateien zu dieser Ressource: 1
phdVasilijeOskanjan.pdf ( 41.32Mb ) -
Radović, Viktor (Beograd , 2017)[more][less]
Zusammenfassung: The main goal of this dissertation is improvement of an approach for identi- cation of the members of asteroid families, based on the hierarchical clustering method. An additional step is introduced in order to reduce a so-called chaining e ect. The introduced algorithm consists of four main steps. In the rst step, the hierarchical clustering method is applied to the initial catalogue of proper elements in order to obtain a preliminary list of family members. In the second step, using available physical properties, and based upon the de ned criteria, the interlopers are identi ed. In the third step, objects identi ed as interlopers in the second step, are excluded from the initial catalogue of proper orbital elements, producing a modi ed catalogue. Finally, in the fourth step, the HCM analysis is performed again, but this time using the modi ed catalogue of proper elements. It is shown that in this way a number of potential interlopers among family members is signi cantly reduced. Moreover, an on-line based portal (Asteroids Families Portal; AFP) to apply this procedure is developed, and is freely available to all interested researchers. The second goal of the dissertation is to determine the limitations of the backward integration method, used for estimation of ages of young asteroid families. This aim is achieved through numerical simulations of the evolution of a ctitious family. By determining instants of secular angles i $ clustering, a linear relationship is found between the depth of a clustering and the age of a family. According to the obtained results, the backward integration method could be successfully applied to families not older than 18 Myrs. URI: http://hdl.handle.net/123456789/4504 Dateien zu dieser Ressource: 1
Radovic_teza.pdf ( 22.32Mb ) -
Tsirvoulis, Georgios (Beograd , 2019)[more][less]
Zusammenfassung: Asteroid families are populations of asteroids in the Main Belt that share a common origin, that is they are the fragments of energetic collisions between two asteroids. Their study over the years has produced a number of important results concerning the collisional and dynamical evolution of the Main Belt, the physical properties of the primordial bodies of the Solar System and the physics of energetic collisions, to name a few. The contribution of the present thesis can be summarized into two main topics: The first is the discovery of a new mechanism that leads to significant perturbations on the orbits of asteroids, and consequently on the evolution of asteroid families affected by it, and the second is the discovery of a couple of new families, each with its own peculiarities. The first part of this thesis was initially motivated by the irregular shape of the (1726) Hoffmeister asteroid family. In an effort to explain this peculiarity we carried out a thorough dynamical analysis of its past evolution and found out that none of the mechanisms known to affect the orbits of asteroids could explain it. Investigating further we discovered that the linear nodal secular resonance with the most massive asteroid (1) Ceres, is the mechanism responsible for the anisotropic inclination distribution of Hoffmeister family members. Having established the importance of the nodal secular resonance with Ceres, we sought to expand on the subject with the study of all linear secular resonances, nodal and periapsidal, involving not only (1) Ceres, but (4) Vesta, the second most massive asteroid, as well. To do so we utilized numerical integrations of test particles across the whole Main Belt, and evaluated the impact of these resonances on their orbits. Furthermore we identified all asteroid families crossed by one or more of these resonances. Two of these cases, the families of (1251) Seinajoki and (1128) Astrid were then studied in more detail, confirming the importance of the previously ignored secular resonances with massive asteroids. The second part details the discovery of two new asteroid families. The first one, that of (326) Tamara family, was motivated by the unexpectedly high number of dark asteroids in the Phocaea region, a part of the inner Main Belt which is expected to consist mostly of bright ones. Using all available physical data we were able to show that most of the dark asteroids therein belong to a single dynamical family, which we then further analyzed finding that it is 264 ± 43 Myrs old and that it could have a significant contribution to the influx of small dark asteroids toward the Near Earth region. The second discovered family, that of (633) Zelima, is a small cluster, sub-family of the large (221) Eos family. After identifying its members, we derived the age of the Zelima family, which turned out to be only about 3.66 Myrs. URI: http://hdl.handle.net/123456789/4752 Dateien zu dieser Ressource: 1
Tsirvoulis_Georgios.pdf ( 76.51Mb ) -
Urošević, Dejan (Belgrade)[more][less]
URI: http://hdl.handle.net/123456789/122 Dateien zu dieser Ressource: 1
phdDejanUrosevic.pdf ( 7.815Mb )