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Dissertations / Theses on the topic 'Star-forming'

Author: Grafiati
Published: 4 June 2021
Last updated: 7 February 2022

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1

Lee, Pawel. "Structure in star forming regions." Thesis, University of Sheffield, 2016. http://etheses.whiterose.ac.uk/12395/.

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Stars form in clumpy, highly substructured environments. In this thesis I set up N-body simulations of substructured star forming regions and investigate the impact that the substructure has on the survival of the star forming regions. I also present a broad range of methods used in other fields to quantify and identify structure. I discuss their strengths and shortcomings and assess their suitability for use in astronomical contexts. I use the Q and Λ methods to compare the distributions of class I and class II sources in observed star forming regions to learn more about the dynamical evoluti
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2

Gledhill, Timothy Michael. "Optical polarimetry of star forming regions." Thesis, Durham University, 1987. http://etheses.dur.ac.uk/6757/.

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3

Holdship, J. R. "Shock chemistry in star forming environments." Thesis, University College London (University of London), 2017. http://discovery.ucl.ac.uk/10027644/.

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Molecules are abundant in many astrophysical environments. The observation of these molecules and the modelling of the chemistry that leads to their formation is a powerful tool for improving our understanding of the regions in which they are found. In this thesis, a chemical model is developed and applied to astrophysical shocks to understand a number of processes in star forming regions. Shocks often result in discontinuous changes in the temperature and density of the gases they affect. The turbulent fragmentation theory of star formation suggests that such shocks are responsible for the ov
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4

Lacki, Brian Cameron. "Cosmic Rays in Star-Forming Galaxies." The Ohio State University, 2011. http://rave.ohiolink.edu/etdc/view?acc_num=osu1313437011.

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5

Kalari, Venu Madhav. "Disc-accretion in star-forming regions." Thesis, Queen's University Belfast, 2015. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.695381.

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In this thesis, I present new ultraviolet/optical/infrared photometric and spectroscopic observations of pre-main sequence stars (PMS) that have formed either in metal-poor conditions, or in the vicinity of strong ionising radiation. This includes observations of 235 Classical T Tauri stars in the Lagoon Nebula; 63 Classical T Tauril Herbig Ae stars in the Carina Nebula open cluster Trumpler 14; 24 intermediate mass T Tauri stars in the low-Z Sh 2-284 star-forming region; and one Herbig 8[e] PMS candidate in the metal-poor 30 Doradus region. I measure the accretion rates of these PMS stars usi
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6

Contreras, Peña Carlos Eduardo. "Exteme variables in star forming regions." Thesis, University of Hertfordshire, 2015. http://hdl.handle.net/2299/15590.

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The notion that low- to intermediate-mass young stellar objects (YSOs) gain mass at a constant rate during the early stages of their evolution appears to be challenged by observations of YSOs suffering sudden increases of the rate at which they gain mass from their circumstellar discs. Also, this idea that stars spend most of their lifetime with a low accretion rate and gain most of their final mass during short-lived episodes of high accretion bursts, helps to solve some long-standing problems in stellar evolution. The original classification of eruptive variables divides them in two separate
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7

Mineo, Stefano. "X-ray emission from star-forming galaxies." Diss., lmu, 2011. http://nbn-resolving.de/urn:nbn:de:bvb:19-134839.

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8

Maskoliūnas, Marius. "Investigation of star forming regions in Cepheus." Doctoral thesis, Lithuanian Academic Libraries Network (LABT), 2014. http://vddb.library.lt/obj/LT-eLABa-0001:E.02~2014~D_20140203_133341-51153.

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The interstellar matter in the Galaxy is concentrated in a thin layer close to the galactic plane, mostly in spiral arms. Most of the interstellar matter is in a form of atomic and molecular gas and only 1% of its mass is in a form of small (0.01 – 0.1 µm) dust grains which absorb and scatter the light of stars and cause the interstellar extinction. A part of interstellar gas and dust are in a diffuse form and fill the space with density which exponentially decreases with the distance from the galactic plane. However, in the spiral arms gigantic molecular clouds are present which play an out
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9

Juárez, Rodríguez Carmen. "Collapse scenarios in magnetized star-forming regions." Doctoral thesis, Universitat de Barcelona, 2017. http://hdl.handle.net/10803/459253.

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Turbulence, magnetic fields and gravity driven flows are important for the formation of new stars. Although magnetic fields have been proven to be important in the formation of stars, only a few works have been done combining magnetic field and kinematic information. Such studies are important to analyze both gravity and gas dynamics and be able to compare them with the magnetic field. In this thesis we will combine dust polarization studies with kinematic analysis towards different star-forming regions. We aim to study the physical properties at core scales (<0.1 pc) from molecular line and
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10

Simon, Robert. "Multiline CN observations of star forming regions." [S.l. : s.n.], 1997. http://deposit.ddb.de/cgi-bin/dokserv?idn=955972264.

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11

Revelle, Melissa C. "OBSERVATIONS OF STAR FORMING REGION NGC 1333." Thesis, The University of Arizona, 2009. http://hdl.handle.net/10150/192971.

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12

Groppi, Christopher Emil. "Submillimeter heterodyne spectroscopy of star forming regions." Diss., The University of Arizona, 2003. http://hdl.handle.net/10150/280414.

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The sub-mm wave portion of the electromagnetic spectrum is on the frontier of both scientific and technical research in astrophysics. Being a relatively young field, scientific advancement is driven by advancements in detector technology. In this thesis, I discuss the design, construction, testing and deployment of two sub-mm wave heterodyne array receivers. Polestar is a 4 pixel (2 x 2) heterodyne array built for operation in the 810 GHz atmospheric window. It is in operation at the AST/RO telescope at the South Pole. This receiver has increased imaging speed in this band at AST/RO by a facto
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13

Tideswell, David Mark. "Chemical modelling of extragalactic star forming regions." Thesis, University of Manchester, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.529246.

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14

Abel, Nicholas Paul. "DETERMINING PHYSICAL CONDITIONS IN STAR FORMING REGIONS." UKnowledge, 2005. http://uknowledge.uky.edu/gradschool_diss/428.

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This dissertation is a study of the physical conditions in star-forming regions, and combines observational data and theoretical calculations. We studied the physical conditions of Orions Veil, which is an absorbing screen that lies along the line of sight to the Orion H II region. We computed photoionization models of the Veil. We combined calculations with UV, radio, and optical spectra that resolve the Veil into two velocity components. We derive many physical parameters for each component seen in 21 cm absorption. We find the magnetic field energy dominates turbulent and thermal energies i
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15

Christie, H. "Structure and depletion in star forming clouds." Thesis, University College London (University of London), 2012. http://discovery.ucl.ac.uk/1367071/.

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Observations of star forming molecular clouds reveal clumpiness on all scales, both in the spectra of molecules and thermal continuum emission from the solid component of the interstellar medium, the dust. Recent, high resolution maps have allowed us to probe down to extremely small scales at which we see clumps of radii just several hundredths of a parsec. A good knowledge of the structure of these regions, and of the chemical processes occurring within, is crucial if we want to properly understand the early stages of star formation and the resulting stellar population. However, observations
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16

Pattison, Ian. "High-mass star-forming regions in M33." Thesis, University of Leeds, 2005. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.422023.

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17

Harker, Justin J. "The star forming universe after z=1 /." Diss., Digital Dissertations Database. Restricted to UC campuses, 2008. http://uclibs.org/PID/11984.

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18

Barsony, Mary Anne Scoville Nicholas Zabriskie Scoville Nicholas Zabriskie. "Outflows in high mass star-forming regions /." Diss., Pasadena, Calif. : California Institute of Technology, 1989. http://resolver.caltech.edu/CaltechETD:etd-09102008-084535.

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19

Visser, Anja Eveline. "Star forming cores in dark molecular clouds." Thesis, University of Cambridge, 2001. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.620970.

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20

Cunningham, Nichol. "Molecular outflows in massive star forming regions." Thesis, University of Leeds, 2015. http://etheses.whiterose.ac.uk/11180/.

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This thesis presents millimetre continuum and molecular line observations exploring the properties of molecular outflows towards massive star forming regions. Massive stars produce some of the most energetic phenomena in the Galaxy, yet we still do not have a comprehensive understanding of how they actually form. Outflows are known to play a key role in this formation process and their properties, particularly how they change depending on the mass, luminosity and evolution of the driving source can shed light on how massive stars actually form. This thesis presents observations at both high (S
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21

Fukue, Tsubasa. "Polarimetric Study of Star/Planet-Forming Regions." 京都大学 (Kyoto University), 2009. http://hdl.handle.net/2433/124422.

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22

Suraphong, Yuma. "Intrinsic Structure of Star-Forming BzK Galaxies." 京都大学 (Kyoto University), 2011. http://hdl.handle.net/2433/152030.

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23

Smith, Penelope Ann. "The molecular content of star-forming galaxies." Thesis, University of Edinburgh, 1992. http://hdl.handle.net/1842/27428.

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An exciting development in observational astronomy over the last 15 years has been the opening up of the submillimetre and millimetre atmospheric windows, to the extent that observations of external galaxies are now possible. This thesis presents the results of a millimetre/submillimetre-wave study of several nearby, infrared-bright, vigorously star-forming galaxies, in an attempt to investigate their molecular hydrogen content. In particular, it seeks to evaluate the relative merits of the two most commonly adopted molecular hydrogen 'tracers' - millimetre-wave transitions of the CO molecule
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24

Randriamanakoto, Rojovola Zara-Nomena. "Super star cluster candidates in the star-forming regions of luminous infrared galaxies." Master's thesis, University of Cape Town, 2010. http://hdl.handle.net/11427/11807.

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Includes abstract.<br>Includes bibliographical references (leaves 86-90).<br>We report on a study of super star cluster (SSC) candidates in the star-forming regions of a representative sample of local luminous infrared galaxies (LIRGs) using KS-band near-infrared (NIR) adaptive optics imaging with GEMINI/ALTAIR and VLT/NACO instruments. The evolution of the cosmic star formation rate (CSFR) indicates its rapid decline in the local Universe.
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25

Marquart, Thomas. "Star-forming Dwarf Galaxies : Internal motions and evolution." Doctoral thesis, Uppsala universitet, Observationell astrofysik, 2012. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-181481.

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The study of dwarf galaxies is important in order to better understand the physics of the young universe and how larger galaxies form and evolve. In this work we focus on Blue Compact Galaxies (BCGs) which havemuch enhanced star formation (starbursts), causing blue colours and strong emission line spectra. Investigating of the inner motions of BCGs provides a means for determining masses and understanding what triggered the current starburst. We have used the Very Large Telescope to perform challenging observations of the stellar motions in several BCGs, as seen in the near-infrared Ca-triplet
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26

Rundle, David. "Molecular line transfer calculations in star forming regions." Thesis, University of Exeter, 2010. http://hdl.handle.net/10036/111934.

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This thesis describes the development, benchmarking and application of a non-LTE, co-moving frame Monte Carlo molecular line radiative transfer module for TORUS. Careful attention has been paid to the convergence, acceleration and optimisation of the code. I present the results of the application of the code to various benchmarking scenarios, including a collapsing cloud, a circumstellar disc and a very optically thick cloud of interstellar water. Benchmarking is an essential step in verifying the accuracy and efficiency of the code which is vital if it is to be used to analyse real data. In a
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27

Furness, James. "Observations of young high mass star forming regions." Thesis, University of Sheffield, 2009. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.515251.

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28

Duval, Florent. "Lyman-alpha radiative transfer in Star-forming galaxies." Doctoral thesis, Stockholms universitet, Institutionen för astronomi, 2015. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-111550.

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This thesis focuses on the intrinsically strongest spectral signature of star-forming galaxies: the Lyman alpha recombination line of the hydrogen atom (hereafter Lya). Located at the wavelength of 1215.67 Å in the restframe far-ultraviolet spectra of star-forming galaxies, the Lya line proves to be a vital tracer and a powerful emission-line window to discover and to study the remote young star-forming galaxies of the early the Universe. Although intrinsically very strong, the Lya line is also a resonant line. As a consequence, the transport of Lya photons inside the interstellar medium (ISM)
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29

Wilding, Timothy Colin. "Probing the star-forming history of external galaxies." Thesis, University of Cambridge, 1993. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.318465.

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30

Kumari, Nimisha. "Spatially-resolved studies of nearby star-forming galaxies." Thesis, University of Cambridge, 2018. https://www.repository.cam.ac.uk/handle/1810/283605.

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Spatially-resolved studies of nearby star-forming galaxies are essential to understand various physical and chemical phenomena at play in the interstellar medium in the galaxies, and consequently to obtain a comprehensive picture of galaxy formation and evolution. In this thesis, I perform spatially-resolved analyses of chemical abundances and star-formation in nearby star-forming galaxies - blue compact dwarf galaxies (BCDs) and spiral galaxies. I map various properties of H II regions and the surrounding gas within three BCDs, using integral field spectroscopic (IFS) data from the Gemini Mul
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31

Hermanowicz, Maciej Tomasz. "Populations of star forming regions in nearby galaxies." Thesis, University of Cambridge, 2014. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.648576.

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32

Lorenzoni, Silvio. "Star-forming galaxies in the epoch of reionization." Thesis, University of Oxford, 2012. http://ora.ox.ac.uk/objects/uuid:0ad7e1e3-cba3-4cef-9ccc-db3bb9278d02.

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This work presents a search for galaxies at 6.5 < z < 9.8 based on the Lyman-break technique, using the latest HST WFC3 near-infrared data covering ∼ 150 arcmin^2 of the GOODS-South field. With these data, it is possible to find sufficient z ≈ 7−9 galaxies to fit both φ∗ and M∗ of the UV Schechter luminosity function. There is evidence for evolution in this luminosity function from z = 6−7 to z = 8−9, in the sense that there are fewer UV-bright galaxies at z ≈ 8 − 9, consistent with an evolution mainly in M∗. The candidate z ≈ 7 − 9 galaxies detected have insufficient ionizing flux to reionize
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33

Craigon, Alison M. "The morphology and kinematics of star forming regions." Thesis, University of Strathclyde, 2016. http://digitool.lib.strath.ac.uk:80/R/?func=dbin-jump-full&object_id=27550.

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To develop a complete picture of the early stages of star and planet formation, it is necessary to understand the molecular clouds from which they form. The physical properties of these clouds and the interactions between their gas and solid constituents are not well known. This thesis presents an observational study of the morphology and kinematics of carbon monoxide(CO) gas in molecular clouds. It forms part of a wider project to produce the first coupled gas-solid maps of a broad sample of starless and star forming clouds. Nine molecular clouds were observed with the James Clerk Maxwell Tel
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34

Martin, Clare E. "Alfvén waves in low-mass star-forming regions." Thesis, University of St Andrews, 1999. http://hdl.handle.net/10023/14190.

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Low-mass star-forming regions have a lifetime which is greater than their dynamical time and must therefore be, in an average sense, in mechanical equilibrium. The work presented here proposes that an equilibrium exists between the self-gravity, gas pressure, and the magnetic field and the waves it supports. Specifically the equilibrium in the direction perpendicular to the ordered magnetic field is given by the Lorentz force, while that parallel to the field is given by an Alfvén wave pressure force. The work detailed in this thesis models a low-mass star-forming region as a one-dimensional
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35

Tafere, Melaku S. "Gas flows and feedback in star-forming galaxies." Master's thesis, Faculty of Science, 2018. http://hdl.handle.net/11427/30016.

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In this MSc thesis, I investigated the kinematics of Hα emission from the hot ionized and NaD absorption from cool neutral gas in a sample of 40 nearby Luminous Infrared Galaxies (LIRGs: LIR ≥1011L) from Supernovae and starbursts in the infrared, SUNBIRD survey imaged with the Southern African Large Telescope (SALT). This project can be seen in two major areas. The first is analyzing the emission and absorption spectra, in this case from the hot ionized gas and cool gas respectively. Two routines were used for the profile fitting, to get the centroid wavelength of both the emission and absorpt
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36

Randriamampandry, Solohery Mampionona. "Stellar masses of star forming galaxies in clusters." University of the Western Cape, 2010. http://hdl.handle.net/11394/3028.

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Magister Scientiae - MSc<br>We determine the stellar mass of star forming galaxies in the X-ray luminous cluster MS 0451.6-0305 at z ∼ 0.54. The stellar masses are estimated from fitting model spectral energy distributions (SEDs) to deep, optical UBRIz observations obtained from WIYN 3.5m telescope and public NIR K-band image from Palomar Observatory telescope. The model SEDs are based on the stellar population synthesis (SPS) model of Bruzual & Charlot (2003) and Conroy et al. (2009) that span a wide range of age, star formation history, Initial Mass Function (IMF), metallicity and dust conte
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37

Asboth, Viktoria. "Studying dusty star-forming galaxies with Herschel-SPIRE." Thesis, University of British Columbia, 2015. http://hdl.handle.net/2429/55041.

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Observations suggest that almost half of the total light emitted by stars in the Universe is absorbed by dust, and the emission is re-radiated at far-infrared and submillimeter wavelengths. Dusty star-forming galaxies play a significant role in the stellar mass build-up at high redshift, but their contribution to the cosmic star formation rate density at z > 4 is still unknown, due to the currently limited availability of statistically significant high-redshift dusty galaxy samples. In this thesis we analyze data from two large area surveys, the HerMES Large Mode Survey (HeLMS) and the Hersche
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38

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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39

Draper, Peter Walter. "CCD polarimetry as a probe of regions of recent star-formation." Thesis, Durham University, 1988. http://etheses.dur.ac.uk/6597/.

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Chapter 1 of this thesis details the incorporation of a Charged Coupled Device (CCD) detector system with the Durham Imaging Polarimeter. The details include the physical characteristics of the device and the electronics and software associated with the device control and data storage. The introduction of the CCD detector system haa made necessary the inclusion of a super-achromatic half-wave plate in the polarimeter which has an inherent variability in its optic axis. Chapter 2of this work describes fully how suitable corrections for this effect can be made, and derives "first order" results.
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40

Gómez, Ruiz Arturo [Verfasser]. "Molecular Outflows in Star Forming Regions / Arturo Gómez Ruiz." Bonn : Universitäts- und Landesbibliothek Bonn, 2014. http://d-nb.info/1052582044/34.

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41

Meger, Nicole. "BzKs in GOODS-N : z~2 star forming galaxies." Thesis, University of British Columbia, 2008. http://hdl.handle.net/2429/7581.

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This thesis presents new deep near-infrared imaging data in one of the most well studied regions of the sky, the Great Observatories Origins Deep Survey's northern field (GOODS-N). In particular, we have produced a science grade Ks-band (2.2 μm) source catalogue with a depth of KS(AB) = 23.8 magnitudes. With our K-selected sample, we use the BzK two-colour se lection criterion to find galaxies lying at redshifts between 1.4 and 2.5. We investigate the redshift distribution of these BzKs using spectroscopic redshifts as well as a new photometric redshift catalogue and find respectively, 13% and
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42

Schmeja, Stefan. "Properties of turbulent star forming clusters: models versus observations." Phd thesis, [S.l.] : [s.n.], 2006. http://deposit.ddb.de/cgi-bin/dokserv?idn=980518660.

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43

Elston, Richard Joseph. "Search for rapidly star-forming galaxies at high redshift." Diss., The University of Arizona, 1988. http://hdl.handle.net/10150/184574.

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We have conducted three surveys to try and locate distant star forming galaxies. The most general survey used deep 2μ images with optical CCD photometry to locate objects with peculiar SEDs. Using the IR data we should be able to locate rapidly star forming galaxies to z = 25. With a 3σ detection limit of 18.5 at K we have found no objects with z > 5 but we have found several blue objects at z < 4 in 16min² of sky. This suggests tha there is no extremely luminous early phase of galaxy formation. We have found several blue objects at z < 4 in 10min² of sky. Of particular interest is an object w
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44

Afonso, José Manuel Lourenço Coutinho. "On the star-forming properties of faint radio sources." Thesis, Imperial College London, 2002. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.271584.

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45

Davies, Luke Jonathan Mark. "A multi-wavelength study of early star-forming galaxies." Thesis, University of Bristol, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.539761.

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46

Rane, Akshaya. "Physical Conditions in a Galactic Star forming region W22." UKnowledge, 2011. http://uknowledge.uky.edu/gradschool_theses/158.

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This document describes study of an active star forming region in our galaxy (the Milky Way) known as W22. Physical conditions in these regions can help us in understanding star formation processes in the universe and hence the structure and evolution of the universe. Zeeman effect measurements in 18 cm OH absorption line were carried out in order to estimate the line of sight magnetic field strength in the molecular cloud associated with this star forming region. Other physical parameters such as hydrogen column density, optical depth, critical magnetic field were also determined from these m
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47

Parkes, I. M. "A search for star-forming galaxies at high redshift." Thesis, University of Edinburgh, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.660361.

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This thesis describes the first search for star formation in primeval galaxies (PGs) at redshifts <I>z</I> ≥ 7. Our method was to undertake deep near-infrared imaging in the J window (~ 1.0 - 1.5<I>μ</I>m) using four narrowband filters of 2% FWHM. Over an area of sky of 3.0<SUP>?1</SUP>, no emission line object was found to a sensitivity limit of ≈ 10<SUP>-18</SUP> Wm<SUP>-2</SUP>. Interpreting this limit in terms of a limit on Lyα emission, it has been possible to place the first constraints on star formation at redshifts 7≤ <I>z</I> ≤ 9. The search is also sensitive to other emission lines a
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48

Giannetti, Andrea <1986&gt. "The evolution of massive clumps in star forming regions." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2014. http://amsdottorato.unibo.it/6216/.

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In this thesis two related arguments are investigated: - The first stages of the process of massive star formation, investigating the physical conditions and -properties of massive clumps in different evolutionary stages, and their CO depletion; - The influence that high-mass stars have on the nearby material and on the activity of star formation. I characterise the gas and dust temperature, mass and density of a sample of massive clumps, and analyse the variation of these properties from quiescent clumps, without any sign of active star formation, to clumps likely hosting a zero-age mai
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49

Noble, Allison. "Dusty star-forming galaxies within high-redshift galaxy clusters." Thesis, McGill University, 2014. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=123107.

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We present a multi-wavelength perspective of star-forming galaxies within high-redshift galaxy clusters. The clusters derive from the Red-sequence Cluster Survey (RCS) and the Spitzer Adaptation of the Red-sequence Cluster Survey (SpARCS), and possess ample spectroscopic coverage, yielding numerous confirmed cluster members. This thesis consists of a collection of distinct but related works, focusing on environmental effects within the dense regions of clusters---some of the rarest structures in the Universe. We exploit the high sensitivities of cutting-edge infrared and submillimeter teles
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Ruffle, Deborah Patricia. "The physical and chemical evolution of star forming regions." Thesis, University College London (University of London), 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.300792.

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