Diss. (sammanfattning) Stockholm : Karol. inst., 2002. / Härtill 5 uppsatser.

Diss. (sammanfattning) Stockholm : Karol. inst., 2003. / Härtill 5 uppsatser.

Diss. (sammanfattning) Linköping : Univ., 2004. / Härtill 6 uppsatser.

Thesis (M.S.)--Ohio University, November, 2008. / Title from PDF t.p. Includes bibliographical references.

Thesis--University of Oklahoma. / Bibliography: leaves 33-36.

Η διδακτορική διατριβή βασίζεται σε οπτικές παρατηρήσεις που πραγματοποιήθηκαν από τα τηλεσκόπια του αστεροσκοπείου του Σκίνακα (το οποίο βρίσκεται στην Κρήτη) και από το τηλεσκόπιο Ισαάκ Νιούτον (που βρίσκεται στη Λα Πάλμα στα Κανάρια νησιά). Από τις παρατηρήσεις αυτές, (οπτικές εικόνες και φάσματα) ανακαλύφθηκαν σε μία περιοχή εβδομήντα τετραγωνικών λεπτών του τόξου της μοίρας, έξι υπολείμματα υπερκαινοφανών αστέρων τα οποία δεν αναγράφονται σε καμία βιβλιογραφία. Τα υπολείμματα αυτά, λόγω της ίδιας περίπου απόστασης που απέχουν, ενδεχομένως να προέρχονται από αλληλεπιδράσεις υπερκαινοφανών αστέρων, οπού η έκρηξη του ενός αστέρα, επιταχύνει την έκρηξη του πλησιέστερου σε αυτόν αστέρα που βρίσκεται στο τελευταίο στάδιο, όταν το ωστικό κύμα διέλθει από αυτόν, δημιουργώντας έτσι μια φυσαλίδα υπολειμμάτων υπερκαινοφανών. Το σημαντικό με αυτή την μελέτη είναι ότι για πρώτη φορά παρατηρήθηκαν στον Γαλαξία μας, στο οπτικό μέρος του φάσματος, μια περιοχή με τόσα υπολείμματα υπερκαινοφανών, παρέχοντάς μας την δυνατότητα να μελετήσουμε τον ρυθμό των εκρήξεων των υπερκαινοφανών με αυτόν της δημιουργίας των υπολειμμάτων τους, και να εξάγουμε συμπεράσματα για τον ρυθμό αστρογένεσης στον Γαλαξία μας. Παράλληλα μελετώντας την ομάδα Μ81, ανιχνεύτηκε για πρώτη φορά στο οπτικό μέρος του φάσματος, σκόνη στην περιοχή μεταξύ των γαλαξιών. Η μελέτη βασίζεται στην σύγκριση του δείκτη χρώματος των γαλαξιών υποβάθρου, των υποψηφίων περιοχών, με τον δείκτη χρώματος γαλαξιών υποβάθρου σε περιοχές που είναι απομακρυσμένες από την ομάδα Μ81, και αποτελούν πεδία ελέγχου. Η συστηματική ερύθρωση που παρουσίαζαν οι γαλαξίες υποβάθρου στις περιοχές πλησίον της ομάδας Μ81 μπορεί να ερμηνευτεί μόνο με την παρουσία μεγάλων ποσοτήτων σκόνης που εμπεριέχονται στο μεσογαλαξιακό χώρο. Η ποσότητα της σκόνης στις περιοχές αυτές υπολογίστηκε ότι είναι περίπου 50 εκατομμύρια ηλιακές μάζες, όσο δηλαδή και η σκόνη που διαθέτει ένας τυπικός σπειροειδής γαλαξίας. Η προέλευση της σκόνης πιθανολογείται ότι οφείλεται σε ένα μέλος της ομάδας (τον γαλαξία Μ82), ο οποίος είναι ένας γαλαξίας με περιοχές έντονης αστρογένεσης και εκτοξεύει μεγάλες ποσότητες σκόνης στο μεσογαλαξιακό χώρο ή στις παλιρροϊκές δυνάμεις που αναπτύχθηκαν κατά την αλληλεπίδραση των γαλαξιών (που έγινε πριν από 200 εκατομμύρια χρόνια) και εκτόξευσαν στον μεσογαλαξιακό χώρο τεράστιες ποσότητες αερίου και μαζί με αυτό και σκόνη. Οι προβλέψεις για την ύπαρξη σκόνης στις περιοχές αυτές, επιβεβαιώθηκε πρόσφατα από τις υπέρυθρες εικόνες που λήφθηκαν από το διαστημικό τηλεσκόπιο Herschel. / This thesis is based on deep optical CCD images which large have been obtained in the light of Hα+[N II], [O III] and [S II]. The resulting mosaic covers an area of 1.4º ´ 1.0º, where filamentary and diffuse emission was discovered, suggesting the existence of more than one supernova remnants (SNRs) in the area. Deep long slit spectra were also taken at eight different regions. Both the flux calibrated images and the spectra show that the emission of the filamentary structures originates from shock-heated gas, while photo-ionization mechanism is responsible for the diffuse emission. In most case, the optical emission is found to be well correlated with the radio at 1420 MHz and 4850 MHz, suggesting their association. The presence of the [O III] 5007 emission line in one of the candidate SNRs suggests shock velocities into the interstellar "clouds" of >100 Km/s, while the absence in the other indicates slower shock velocities. For all candidate remnants the [S II] λλ 6716/6731 ratio indicates electron densities below 270 cm-3, while the Hα emission has been measured to be between 0.6 to 41´10-17 erg s-1 cm-2 arcsec-2. The detected optical emission could be part of a number of supernovae explosions and the possibility that it is within an OB association can not be ruled out. It will then be the first optical discovery of SRNs within a bubble or superbubble in our Galaxy. Further, the study of those areas, also provides information for the star formation history of the Galaxy. Galactic dust constitutes approximately half of the elements more massive than helium produced in stellar nucleosynthesis. Notwithstanding the formation of dust grains in the dense, cool atmospheres of late-type stars, there still remain huge uncertainties concerning the origin and fate of galactic stardust. In this Letter, we identify the intergalactic medium (i.e., the region between gravitationally bound galaxies) as a major sink for galactic dust. We discover a systematic shift in the color of background galaxies viewed through the intergalactic medium of the nearby M81 group. This reddening coincides with atomic, neutral gas previously detected between the group members. The dust–to–H I mass ratio is high (1/20) compared to that of the solar neighborhood (1/120), suggesting that the dust originates from the center of one or more of the galaxies in the group. Indeed, M82, which is known to be ejecting dust and gas in a starburst-driven superwind, is cited as the probable main source.

Massive OB stars are very influential objects in the ecology of galaxies like our own. Current catalogues of Galactic OB stars are heavily biased towards bright (g < 13) objects, only typically including fainter objects when found in prominent star clusters (Garmany et al., 1982; Reed, 2003; Maíz-Apellániz et al., 2004). Exploitation of the VST Photometric Hα Survey (VPHAS+) allows us to build a robust catalogue of photometrically-selected OB stars across the entire Southern Galactic plane, both within clusters and in the field, down to ~20th magnitude in g. For the first time, a complete accounting of the OB star runaway phenomenon becomes possible. Along with making the primary selection using VPHAS+ colours, I have performed Markov-Chain Monte Carlo fitting of the spectral energy distributions of the selected stars by combining VPHAS+ u, g, r, i with published J, H, K photometry. This gives rough constraints on effective temperature and distance, whilst delivering much more precise reddening parameters A0 and RV - allowing us to build a much richer picture of how extinction and extinction laws vary across the Galactic Plane. My thesis begins with a description of the method of photometric selection of OB star candidates and its validation across a 2 square degree field including the well- known young massive star cluster Westerlund 2 (Mohr-Smith et al., 2015)1. Following on from this I present spectroscopy with AAOmega of 283 candidates identified by our method, which confirms that ~ 94% of the sample are the expected O and early B stars. I then develop this method further and apply it to a Galactic Plane strip of 42 square-degrees that runs from the Carina Arm tangent region to the much studied massive cluster in NGC 3603. A new aspect I attend to in this expansion of method is tightening up the uniform photometric calibration of the data, paying particular attention to the always-challenging u band. This leads to a new and reliable catalogue of 5915 OB stars. As well as increasing the numbers of identified massive stars in this large region of the sky by nearly an order of magnitude, a more complete picture of massive star formation in the Carina Arm has emerged. I have found a broad over-density of O stars around the highly luminous cluster NGC 3603 and have uncovered two new candidate OB clusters/associations. I have also paired up the ionization sources of a number of HII regions catalogued by the RMS survey. It is also shown that the OB star scale- height can serve as a roughly standard ruler, leading to the result that the OB star layer shows the onset of warping at RG ~ 10kpc. My results confirm that this entire region requires a non-standard (3.5 < RV < 4.0) reddening law for distances greater than ~2kpc. The methods developed in this study are ready to roll out across the rest of the VPHAS+ footprint that has been observed to date. This extension will take in a strip ~ ±2 degrees across the entire Southern Galactic mid-plane (a sky area of over 700 square degrees), within which we expect to find the majority of massive OB stars. This will result in the largest catalogue of Galactic OB stars to date.

abstract: It is estimated that wind induced soil transports more than 500 x 106 metric tons of fugitive dust annually. Soil erosion has negative effects on human health, the productivity of farms, and the quality of surface waters. A variety of different polymer stabilizers are available on the market for fugitive dust control. Most of these polymer stabilizers are expensive synthetic polymer products. Their adverse effects and expense usually limits their use. Biopolymers provide a potential alternative to synthetic polymers. They can provide dust abatement by encapsulating soil particles and creating a binding network throughout the treated area. This research into the effectiveness of biopolymers for fugitive dust control involved three phases. Phase I included proof of concept tests. Phase II included carrying out the tests in a wind tunnel. Phase III consisted of conducting the experiments in the field. Proof of concept tests showed that biopolymers have the potential to reduce soil erosion and fugitive dust transport. Wind tunnel tests on two candidate biopolymers, xanthan and chitosan, showed that there is a proportional relationship between biopolymer application rates and threshold wind velocities. The wind tunnel tests also showed that xanthan gum is more successful in the field than chitosan. The field tests showed that xanthan gum was effective at controlling soil erosion. However, the chitosan field data was inconsistent with the xanthan data and field data on bare soil. / Dissertation/Thesis / Ph.D. Civil and Environmental Engineering 2011

Les explosions de mélanges de gaz inflammables/solides combustibles ne sont pas bien comprises en raison de la complexité des transferts thermiques, des mécanismes de cinétiques et des interactions entre la turbulence /combustion. L'objectif principal de ce travail est d'étudier la sévérité des explosions des nanoparticules de carbone noir/méthane afin de comprendre l'influence de l'insertion des nanoparticules sur les explosions de gaz. Des tests ont été effectués sur ces mélanges dans un tube de propagation de la flamme et dans une sphère d'explosion standard de 20 L. L'influence de la turbulence initiale et de la taille de particule élémentaire du noir de carbone a également été étudiée. Il semble que l'insertion de nanoparticules de noir de carbone augmente d'environ 10% la sévérité de l’explosion pour les mélanges pauvres en méthane. Par conséquent, il semble que les nanoparticules ont un impact sur la sévérité de l'explosion même pour les systèmes à basse turbulence, contrairement aux systèmes impliquant des poudres de taille micrométrique qui nécessitent une dispersion à des niveaux élevés de turbulence. L'augmentation de la vitesse maximale de montée en pression est plus élevée pour des poudres avec un petit diamètre de particule, notamment en raison des phénomènes de fragmentation. En outre, un modèle numérique de propagation de front de flamme associé à un mélange gaz/noir de carbone a été développé pour examiner l'influence du noir de carbone sur la propagation de la flamme. Les résultats du modèle numérique suggèrent que la contribution de la chaleur radiative favorise l'accélération de la flamme. Ces résultats sont en accord avec les résultats expérimentaux de sévérité de l'explosion pour certains mélanges hybrides / Flammable gas/solid hybrid mixture explosions are not well understood because of the interaction of the thermal transfer process, the combustion kinetics mechanisms and the interactions between turbulence and combustion. The main objective on this work is to study the explosion severity and flame burning velocities of carbon black nanoparticles/methane to better understand the influence of added nanopowders in gas explosions. Tests have been performed in a flame propagation tube and in the standard 20 L explosion sphere. The influence of carbon black particles on the explosions severity and in the front flame propagation has been appreciated by comparing the results obtained for pure gas mixtures. It appeared that the carbon black nanoparticles insertion increases around 10% the explosion severity for lean methane mixtures. Therefore, it seems that nanoparticles has an impact on the severity of the explosion even for quiescent systems, contrary to systems involving micro-sized powders that requires a dispersion at high turbulence levels. The increment on the maximum rate of pressure rise is higher for powders with lower elementary particle diameter, which is notably due to the fragmentation phenomena. A flame propagation numerical model associated to a gas/carbon black mixture has been developed to examine the influence of carbon blacks on the flame propagation. The results of the numerical model suggest that the radiative heat contribution promotes the flame acceleration. This result is consistent with the experimental increase on the explosion severity for some hybrid mixtures

Title: Sputtering of dust grains and its consequences for space processes Author: Marek Vyšinka Department: Department of Surface and Plasma Science Supervisor: prof. RNDr. Jana Šafránková, DrSc., Department of Surface and Plasma Science Abstract: A great part of matter in a space has a form of dust grains, tiny pieces of rocks with the dimensions of hundreds nanometers to hundreds micrometers. In this environment dust grains undergo collisions with energetic particles (electron, ions, UV photons) that leads to their charging and modification. The presented thesis studies ion-dust interactions and is focussed on dust grain modification through ion implantation and its destruction via sputtering process. Two compu- ter models are presented - first for computing the ion implantation profile in the grain and second, for the shape of the sputtered grain lying on the surface of a bigger object. The resulting shape of the grain is compared with that obtained experimentally. Important results of the thesis are measured sputtering yields for spherical SiO2 grains at several surface potentials obtained by simultaneous ion and electron bombardments. Keywords: ions, dust grains, sputtering, sputtering yield, implantation profile 1