%% %% This is file `sample.bib', %% generated with the docstrip utility. %% %% The original source files were: %% %% ubcthesis.dtx (with options: `samplebib') %% %% This file was generated from the ubcthesis package. %% -------------------------------------------------------------- %% %% Copyright (C) 2001 %% Michael McNeil Forbes %% mforbes AT %% lns.mit.edu %% %% (Note that the AT symbol cannot be used in a comment in a bibtex file, %% hence the lack of a proper email address above.) %% %% This file may be distributed and/or modified under the %% conditions of the LaTeX Project Public License, either version 1.2 %% of this license or (at your option) any later version. %% The latest version of this license is in %% http://www.latex-project.org/lppl.txt %% and version 1.2 or later is part of all distributions of LaTeX %% version 1999/12/01 or later. %% %% This program is distributed in the hope that it will be useful, %% but WITHOUT ANY WARRANTY; without even the implied warranty of %% MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the %% LaTeX Project Public License for more details. %% %% This program consists of the files ubcthesis.dtx, ubcthesis.ins, and %% the sample figures fig.eps and fig.fig. %% %% This file may be modified and used as a base for your thesis without %% including the licence agreement as long as the content (i.e. textual %% body) of the file is completely rewritten. You must, however, change %% the name of the file. %% %% This file may only be distributed together with a copy of this %% program. You may, however, distribute this program without generated %% files such as this one. %% \ProvidesFile{sample.bib}[2002/12/15 v1.19 ^^J University of British Columbia Sample Thesis] %% These are just some examples of articles and books. Some of the fields %% are not needed, for example the abstract and SLACcitation fields. There %% are many other types of documents. The entry CL:2000 poses a problem %% in the URL field. I am not sure how to get around this right now. @Article{Wandelt:2000ad, author = "Benjamin D. Wandelt and Romeel Dave and Glennys R. Farrar and Patrick C. McGuire and David N. Spergel and Paul J. Steinhardt", title = "Self-interacting dark matter", year = "2000", eprint = "astro-ph/0006344", SLACcitation = "%%CITATION = ASTRO-PH 0006344;%%", abstract = "Spergel and Steinhardt have recently proposed the concept of dark matter with strong self-interactions as a means to address numerous discrepancies between observations of dark matter halos on subgalactic scales and the predictions of the standard collisionless dark matter picture. We review the motivations for this scenario and discuss some recent, successful numerical tests. We also discuss the possibility that the dark matter interacts strongly with ordinary baryonic matter, as well as with itself. We present a new analysis of the experimental constraints and re-evaluate the allowed range of cross-section and mass.", } @Book{LL:1977, author = "L. D. Landau and E. M. Lifshitz", title = "Quantum Mechanics: Non-relativistic theory", publisher = "Pergamon Press", year = "1989, c1977", volume = "3", series = "Course of Theoretical Physics", address = "Oxford; New York", edition = "Third", } @InCollection{Peccei:1989, author = "R. D. Peccei", title = "Special Topics: The Strong {CP} Problem", booktitle = "CP violation", publisher = "World Scientific", year = "1989", editor = "C. Jarlskog", address = "Singapore", month = jan, } @InProceedings{CL:2000, author = "S. A. {Colgate} and H. {Li}", title = "The Magnetic Fields of the Universe and Their Origin", booktitle = "10 pages, 1 figure (figures.png), invited talk at IAU 195 Preprint no. LAUR 00-180.", year = "2000", month = jan, pages = "1418", URL = "{http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=\ 2000astro.ph..1418C&db_key=PRE}", adsnote = "Provided by the NASA Astrophysics Data System", eprint = "astro-ph/0001418", abstract = "Recent rotation measure observations of a dozen or so galaxy clusters have revealed a surprisingly large amount of magnetic fields, whose estimated energy and flux are, on average, {$\sim 10^{58}$} ergs and {$\sim 10^{41}$ G cm$^2$}, respectively. These quantities are so much larger than any coherent sums of individual galaxies within the cluster that an efficient galactic dynamo is required. We associate these fields with single AGNs within the cluster and therefore with all galaxies during their AGN phase. Only the central, massive black hole (BH) has the necessary binding energy, {$\sim 10^{61}$} ergs. Only the accretion disk during the {BH} formation has the winding number, {$\sim 10^{11}$} turns, necessary to make the gain and magnetic flux. We present a model of the BH accretion disk dynamo that might create these magnetic fields, where the helicity of the {$\alpha - \Omega$} dynamo is driven by star-disk collisions. The back reaction of the saturated dynamo forms a force-free field helix that carries the energy and flux of the dynamo and redistributes them within the clusters.", } @Misc{Turner:1999, author = "M. S. Turner", title = "Dark Matter, Dark Energy and Fundamental Physics", howpublished = "astro-ph/9912211", year = "1999", month = dec, abstract = "More than sixty years ago Zwicky made the case that the great clusters of galaxies are held together by the gravitational force of unseen (dark) matter. Today, the case is stronger and more precise: Dark, nonbaryonic matter accounts for {$30\% \pm 7\%$} of the critical mass density, with baryons (most of which are dark) contributing only {$4.5\% \pm 0.5\%$} of the critical density. The large-scale structure that exists in the Universe indicates that the bulk of the nonbaryonic dark matter must be cold (slowly moving particles). The SuperKamiokande detection of neutrino oscillations shows that particle dark matter exists, crossing an important threshold. Over the past few years a case has developed for a dark-energy problem. This dark component contributes about {$80\% \pm 20\%$} of the critical density and is characterized by very negative pressure {$(p_X < -0.6 \rho_X)$}. Consistent with this picture of dark energy and dark matter are measurements of {CMB} anisotropy that indicate that total contribution of matter and energy is within {$10\%$} of the critical density. Fundamental physics beyond the standard model is implicated in both the dark matter and dark energy puzzles: new fundamental particles (e.g., axion or neutralino) and new forms of relativistic energy (e.g., vacuum energy or a light scalar field). A flood of observations will shed light on the dark side of the Universe over the next two decades; as it does it will advance our understanding of the Universe and the laws of physics that govern it.", } @Book{Vilenkin:1994, author = {Alexander Vilenkin and E. P. S. Shellard}, title = {Cosmic Stringas and Other Topological Defects}, publisher = {Cambridge University Press}, year = 1994, address = {Cambridge} } \endinput %% %% End of file `sample.bib'.