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Rozprawy doktorskie na temat „Spectral line formation Congresses”

Autor: Grafiati

Data publikacji: 29 lipca 2024

Data aktualizacji: 31 lipca 2025

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1

Gibb, Andrew Gordon. "Spectral line observations of two contrasting molecular clouds : Lynds 1630 and G34.3+0.2." Thesis, University of Kent, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.239827.

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2

Bedikoglou, Isidore. "A study of spectral line surveys for four regions related to star formation." Thesis, University of Manchester, 2009. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.514420.

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Star formation is a process that has been studied extensively during the last decades. With the advent of advanced instruments our knowledge has expanded beyond the point of general descriptions. From simple models of gravitational contraction of spherical clouds we have managed to give more detailed descriptions about the inner processes and the chemistry within the environment of proto stars and young stellar objects. Still there are several issues that have not been fully understood, such as the formation of stars with very large masses, the exact mechanism that generates strong bipolar out

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3

Lo, Wing-Chi Nadia Physics Faculty of Science UNSW. "A multi-molecular line study of an entire giant molecular cloud." Awarded by:University of New South Wales. Physics, 2009. http://handle.unsw.edu.au/1959.4/44587.

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A unified theory of star formation remains one of the major unsolved issues in astrophysics. Presented here are the results of multi-molecular lines mapping of the entire giant molecular cloud G333, comprised sites of low- and high-mass star forming regions in various evolution stages of star formation. The result shows the spatial distribution of CS, HCO+, HCN and HNC are similar on large scales, while N2H+ seems to trace preferentially the very densest regions, possibly due to the chemical difference, that N2H+ is sensitive to temperature and readily destroyed by CO. Two analysis methods wer

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4

Li, Shanghuo, Junzhi Wang, Zhi-Yu Zhang, et al. "Millimetre spectral line mapping observations towards four massive star-forming H ii regions." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/623847.

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We present spectral line mapping observations towards four massive star-forming regions Cepheus A, DR21S, S76E and G34.26+0.15 - with the IRAM 30-m telescope at the 2 and 3 mm bands. In total, 396 spectral lines from 51 molecules, one helium recombination line, 10 hydrogen recombination lines and 16 unidentified lines were detected in these four sources. An emission line of nitrosyl cyanide (ONCN, 14(0), 14-13(0), (13)) was detected in G34.26+0.15, as the first detection in massive star-forming regions. We found that c-C3H2 and NH2D show enhancement in shocked regions, as suggested by the evid

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5

Martinez, Osorio Yeisson Fabian. "Atomic Processes in Stellar Atmospheres : Inelastic Collisions and Effects on Late-type Spectra." Doctoral thesis, Uppsala universitet, Teoretisk astrofysik, 2015. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-249168.

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Chemical abundances as measured from stellar spectral lines are often subject to uncertainties due to lack of accurate data for inelastic collisions, which is needed for non-local thermodynamic equilibrium (non-LTE) modelling. For cool stars, understanding of collision processes with electrons and hydrogen atoms is required to achieve high precision measurements. In this thesis, I have investigated the role of these collisions on the non-LTE formation of Li and Mg spectral lines in late-type stars. In the case of Li, electron impact excitation processes were calculated using the R-matrix with

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6

Hindson, Luke Paul. "The G305 star forming complex : a panoramic view of the environment and star formation." Thesis, University of Hertfordshire, 2012. http://hdl.handle.net/2299/9197.

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This thesis presents molecular line and radio continuum observations of the giant molecular cloud (GMC) complex known as G305. The energy input from high-mass stars in the form of powerful winds and ionising radiation is one of the primary feedback mechanisms in GMCs. This feedback is thought to play a dual role both dispersing and destroying the natal environment but also sweeping up and compressing molecular gas and potentially triggering new episodes of star formation. Despite their importance to the evolution of GMCs and galaxies as a whole, the physical processes behind the formation and

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7

Pacheco-Vazquez, Susana. "Unbiased Spectral Survey towards the intermediate-mass Class 0 protostar Cep E-mm." Thesis, Grenoble, 2012. http://www.theses.fr/2012GRENY066/document.

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Les protoétoiles de masse intermédiaire (IM) (2 ≤ M* ≤ 8 Msun) sont le lien entre les étoiles de faible et haute masse car elles couvrent également un intervalle intermédiaire de luminosités, de densités et de températures [Fuente et al., 2012]. Même si les « IM-YSOs » jouent un rôle important dans l'étude de la formation des étoiles, on a très peu de connaissances sur la formation et l'évolution des premières étapes des protoétoiles de masse intermédiaire. Les études systématiques spectrales sont un outil puissant pour caractériser la composition chimique d'un objet astrophysique, et la seule

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8

Collet, Remo. "On the Chemical Composition of Metal-Poor Stars : Impact of Stellar Granulation and Departures from Local Thermodynamic Equilibrium on the Formation of Spectral Lines." Doctoral thesis, Uppsala University, Department of Astronomy and Space Physics, 2006. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-7121.

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<p>The information about the chemical compositions of stars is encoded in their spectra. Accurate determinations of these compositions are crucial for our understanding of stellar nucleosynthesis and Galactic chemical evolution. The determination of elemental abundances in stars requires models for the stellar atmospheres and the processes of line formation. Nearly all spectroscopic analyses of late-type stars carried out today are based on one-dimensional (1D), hydrostatic model atmospheres and on the assumption of local thermodynamic equilibrium (LTE). This approach can lead to large systema

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9

Benredjem, Djamel. "Etude théorique du déplacement des raies spectrales par effet de polarisation dans les plasmas denses : cas des raies de l'hélium hydrogenoïde." Paris 6, 1986. http://www.theses.fr/1986PA066016.

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Le déplacement des raies de l'hélium hydrogenoïde émises dans les plasmas denses a été calculé en considérant l'effet des électrons libres et celui des ions perturbateurs sur l'émetteur. Le premier, déterminé par une méthode de potentiel auto-consistant, induit un déplacement vers le rouge alors que le second, calcule par perturbation, décale les raies vers le bleu. Deux méthodes de calcul de cette grandeur ont été développées : l'une permet d'évaluer le déplacement comme moment spectral du profil complet; l'autre, plus simple, séparé les deux contributions et peut s'appliquer à des états très

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10

García, Pérez Ana Elia. "On the Abundances of Li, Be and O in Metal-Poor Stars in the Galaxy." Doctoral thesis, Uppsala University, The Uppsala Astronomical Observatory, 2005. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-4814.

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<p>Stellar atmospheres constitute excellent environments to study the chemical evolution of our Galaxy. The chemical composition of these atmospheres reflects the composition of the gas from where these stars were born. As the Galaxy evolves, the composition of the gas changes from being primordial (Big-Bang nucleosynthesis) to being enriched in heavy elements (stellar and interstellar nucleosynthesis). The abundances of fragile chemical elements can be affected by stellar mixing processes. Precise lithium, beryllium and oxygen abundance determinations in old stars are presented in this thesis

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11

Rozario, Hoimonti Immaculata. "Spectroscopic study of acetylene and hydrogen cyanide." Thesis, Lethbridge, Alta. : University of Lethbridge, Dept. of Physics and Astronomy, c2012, 2012. http://hdl.handle.net/10133/3415.

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High-resolution molecular spectroscopy has been used to study acetylene line parameters and emission spectra of hydrogen cyanide. All acetylene spectra were recorded in our laboratory at the University of Lethbridge using a 3-channel tuneable diode laser spectrometer. N2-broadened line widths and N2-pressure induced line shifts have been measured for transitions in the v1+v3 band of acetylene at seven temperatures in the range 213–333K to obtain the temperature dependences of broadening and shift coefficients. The Voigt and hard-collision line profile models were used to retrieve the line para

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12

Djeffal, Malik Abdeflam. "Bruits et vibrations des moteurs électriques asynchrones." Rouen, 1997. http://www.theses.fr/1997ROUES031.

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Cette étude sur les vibrations des moteurs asynchrones monophasés à phase auxiliaire a pour but principal de réduire le bruit émis. Une compréhension des phénomènes d'origine électromagnétique, mécanique ou aérodynamique est nécessaire. Le détail connu relatif aux mesures du bruit et des vibrations est rappelé. Les vibrations électromagnétiques sont celles qui sont au centre de nos préoccupations et que l'on cherche à réduire. Cependant les vibrations mécaniques ne doivent pas être négligées. Les équations de la mécanique permettent de décrire les vibrations de translation, en plus des vibrati

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13

Cabrit, Sylvie. "Ejection de matiere dans les objets protostellaires et les etoiles jeunes de faible masse." Paris 6, 1989. http://www.theses.fr/1989PA066082.

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Une etude de 2 diagnostics de perte de masse dans les objets stellaires et on developpe un programme qui calcule la formation des raies rotationnelles de co en geometrie axiale. Les contraintes posees par les resultats sur la structure a grande echelle des jets sont discutees. Les raies interdites dans les etoiles jeunes de faible masse sont ensuite etudiees. Plusieurs modeles capables d'expliquer les profils observes sont discutes

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14

Scott, Patrick C. "CO Spectral Line Formation in the Sun: Convective Simulation, Line Profiles and Isotopic Abundance Measures." Thesis, 2004. http://hdl.handle.net/1885/42581.

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CO spectral line formation in the Sun was modelled using realistic, ab initio, timedependent 3D radiative-hydrodynamical model atmospheres. Three `phases' of 3D model atmospheres were utilised. In Phase 1, strong CO lines formed in very high atmospheric layers were modelled using the established model (Asplund et al. 2000b). This produced less than perfect agreement with observed line asymmetries measured in the ATMOS disc-centre solar atlas. The velocity, temperature and density fields were then manually altered during Phase 2 in order to ascertain the reasons for the disagreement with observ

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15

Sutherland, Ralph S. "Interstellar shock fluorescence." Phd thesis, 1993. http://hdl.handle.net/1885/138720.

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16

Fabbian, Damian. "Chemical compositions of stars in the light of non-LTE spectral line formation : the evolution of carbon and oxygen in the Galaxy." Phd thesis, 2008. http://hdl.handle.net/1885/151594.

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