Relevant bibliographies by topics / Q-stars

Academic literature on the topic 'Q-stars'

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Published: 14 March 2023

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Journal articles on the topic "Q-stars"

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Lynn, Bryan W. "Q-stars." Nuclear Physics B 321, no. 2 (July 1989): 465–80. http://dx.doi.org/10.1016/0550-3213(89)90352-0.

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Bahcall, Safi, Bryan W. Lynn, and Stephen B. Selipsky. "Are neutron stars Q-stars?" Nuclear Physics B 331, no. 1 (February 1990): 67–79. http://dx.doi.org/10.1016/0550-3213(90)90018-9.

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Bahcall, Safi, Bryan W. Lynn, and Stephen B. Selipsky. "Fermion Q-stars." Nuclear Physics B 325, no. 3 (October 1989): 606–18. http://dx.doi.org/10.1016/0550-3213(89)90498-7.

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Selipsky, Stephen B., Dallas C. Kennedy, and Bryan W. Lynn. "Non-abelian Q-stars." Nuclear Physics B 321, no. 2 (July 1989): 430–38. http://dx.doi.org/10.1016/0550-3213(89)90350-7.

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Becerril, R., A. Bernal, F. S. Guzmán, and U. Nucamendi. "Stability properties of Q-stars." Physics Letters B 657, no. 4-5 (December 2007): 263–68. http://dx.doi.org/10.1016/j.physletb.2007.07.077.

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Su, Ru-Keng, Cheng-Gang Su, and Rong-Shi Pan. "Q-stars at finite temperature." Physics Letters B 278, no. 3 (March 1992): 297–301. http://dx.doi.org/10.1016/0370-2693(92)90196-b.

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Prikas, Athanasios. "Q-stars in 2+1 dimensions." Nuclear Physics B 690, no. 3 (July 2004): 201–29. http://dx.doi.org/10.1016/j.nuclphysb.2004.05.005.

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Geng, Yuan-Yuan, Dong-Nuan Cui, Jiang Zhang, and Bo Zhang. "Exploring the nucleosynthesis region of metal-poor Stars." Proceedings of the International Astronomical Union 4, S252 (April 2008): 339–40. http://dx.doi.org/10.1017/s1743921308023144.

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AbstractThe chemical abundances of the very metal poor double-enhanced stars are excellent information to set new constraints on models of neutron-capture processes at low metallicity. There have been many theoretical studies of s-process nucleosynthesis in low-mass AGB stars. Using the parametric approach based on the radiative s-process nucleosynthesis model, we calculate the following five parameters for a series of metal-poor stars. They are: the mass fraction of 13C pocket q, the overlap factor r, the neutron exposure per interpulse Δτ, and the component coefficients that correspond to relative contribution from the s-process and the r-process. We find that the mass fraction of 13C pocket q deduced for the Pb stars is comparable to the overlap factor r, which is about 10 times larger than normal AGB model; q ~ 0.05; and the neutron exposure per interpulse Δτ for all Pb stars are about 10 times smaller than the ST case (Δτ ~ 7.0mb−1). Although the two fundamental parameters Δτ and q obtained for the Pb stars are very different from the AGB stellar model, the results of the larger value of q and the smaller value of Δτ can also explain the abundance distribution of the Pb stars. This suggest that the q change to larger than that of normal AGB model. Then, this factor will result in the descent of the density of 13C in the nuclear synthesis region directly. So, the neutron exposure Δτ will also decrease to the same extent. Although the neutron number density in the larger initial mass AGB stars (m > 3M⊙) is high, the neutron irradiation time is shorter, obviously the neutron exposure per interpulse in the AGB stars should be smaller. It is noteworthy that the total amount of 13C in metal poor condition is close to the ST case, which is consistent with the primary nature of the neutron source.
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Prikas, Athanasios. "Q-Stars in Anti de Sitter Spacetime." General Relativity and Gravitation 36, no. 8 (August 2004): 1841–69. http://dx.doi.org/10.1023/b:gerg.0000035955.07614.0d.

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Madsen, Jes. "Detecting supersymmetric Q-balls with neutron stars." Physics Letters B 435, no. 1-2 (September 1998): 125–30. http://dx.doi.org/10.1016/s0370-2693(98)00789-8.

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Dissertations / Theses on the topic "Q-stars"

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Pombo, Alexandre Mira. "Q-ball spectroscopy and construction of boson stars." Master's thesis, Universidade de Aveiro, 2017. http://hdl.handle.net/10773/23513.

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Mestrado em Física
Na ausência de efeitos gravitacionais, a dispersão da equação linear de Klein- Gordon pode ser contrabalan cada pela introdução de auto-interações não-lineares do campo escalar. Quando ocorre o cancelamento de efeitos não lineares e dispersivos, ocorrem pacotes auto-reforçadas de ondas solitárias. Quando um único campo escalar complexo produz soluções solit onicas, eles são conhecidos como Qballs. O tipo mais genérico de Q-balls possui uma rotação e uma carga elétrica e são denominados \gauged, spinning Q-balls". Nesta tese, após uma breve introdução do modelo e algumas propriedades físicas e assintóticas, um método espectroscópico para decompor os vários campos das Q-ball e introduzido e os vários modos obtidos a partir dele são analisados. De modo a analisar estes, algumas quantidades físicas são estudadas e comparadas entre as diferentes soluções de parâmetros de Q-ball. Numa segunda parte, consideraremos a existência de objetos bosónicos na presença de efeitos gravitacionais. A existência de \bolhas" localizadas, aproximadamente estacionárias, do campo gravitacional e eletromagnético clássico - geons foi conjeturada há mais de meio século. Se se insistir em soluções estáticas, as configurações topologicamente triviais no eletro-vácuo são descartadas por teoremas de não-retorno para solitões. Mas os conceitos estacionários e assintoticamente planos de geons encontraram uma solução no vácuo escalar, onde podem existir \bolhas" de campo escalar localizados conhecidos como estrelas do bosões (escalares). Nesta tese, um método de Runge-Kutta de quarta ordem, com uma rotina de shooting, foi implementado para obter o diagrama de fase para obter uma estrela de bosões no estado fundamental, bem como uma unica solução para um estado excitado. Analisamos então o diagrama de fases obtido e algumas quantidades físicas obtidas a partir dele.
In the absence of gravitational e ects, the dispersiveness of the linear Klein-Gordon equation can be counter-balanced by introducing non-linear self-interactions of the scalar eld. When cancellation of non-linear and dispersive e ects occurs, selfreinforcing solitary wave packets emerge. If this solitary wave packets are formed by a single complex scalar eld, a Q-ball is formed. The most generic type of Qballs, known as gauged spinning Q-balls, possess a spinning phase and an electrical charge. In this thesis, after a brief introduction of the model and some physical and asymptotical properties of Q-ball solutions, a spectroscopic method to decompose the several Q-ball elds is introduced, and used to obtained, and analise the latter's. To perform the spectroscopic analises and compare between the possible Q-ball solutions, some physical quantities { namely the electrical charge, Noether charge, energy, gyromagnetic factor and magnetic dipole moment { are retrieved. In a second part, the existence of bosonic objects in the presence of gravitational e ects is going to be considered. The existence of localized, approximately stationary, lumps of the classical gravitational and electromagnetic eld { geons { was conjectured more than half a century ago. If one insists on exact stationarity, topologically trivial con gurations in electro-vacuum are ruled out by no-go theorems for solitons. But stationary, asymptotically at geons found a realization in scalar-vacuum, where everywhere non-singular, localized eld lumps exist, known as (scalar) boson stars. To numerically obtain the boson star solutions, a four order Runge-Kutta method with a shooting routine was implemented. With it, the phase parameter diagram for the fundamental state and single excited state, are obtained. We then analise the obtained phase diagram, study the di erent branches and some physical quantities
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Almergren, Joachim. "Energy and Rotation in Relativistic Astrophysics." Doctoral thesis, SISSA, 2003. http://hdl.handle.net/20.500.11767/4245.

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Moe, Maxwell, and Stefano Rosanne Di. "Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624451.

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We compile observations of early-type binaries identified via spectroscopy, eclipses, long-baseline interferometry, adaptive optics, common proper motion, etc. Each observational technique is sensitive to companions across a narrow parameter space of orbital periods P and mass ratios q. =. M-comp/M-1. After combining the samples from the various surveys and correcting for their respective selection effects, we find that the properties of companions to O-type and B-type main-sequence (MS) stars differ among three regimes. First, at short orbital periods P less than or similar to 20. days (separations a less than or similar to 0.4 au), the binaries have small eccentricities e... 0.4, favor modest mass ratios < q > less than or similar to 0.5, and exhibit a small excess of twins q. >. 0.95. Second, the companion frequency peaks at intermediate periods log P (days). approximate to. 3.5 (a approximate to 10 au), where the binaries have mass ratios weighted toward small values q. approximate to 0.2-0.3 and follow a Maxwellian " thermal" eccentricity distribution. Finally, companions with long orbital periods log P (days). approximate to 5.5-7.5 (a approximate to 200-5000 au) are outer tertiary components in hierarchical triples and have a mass ratio distribution across q. approximate to 0.1-1.0 that is nearly consistent with random pairings drawn from the initial mass function. We discuss these companion distributions and properties in the context of binary-star formation and evolution. We also reanalyze the binary statistics of solar-type MS primaries, taking into account that 30% +/-. 10% of single-lined spectroscopic binaries likely contain white dwarf companions instead of low-mass stellar secondaries. The mean frequency of stellar companions with q. >. 0.1 and log P (days). <. 8.0 per primary increases from 0.50. +/- 0.04 for solar-type MS primaries to 2.1. +/- 0.3 for O-type MS primaries. We fit joint probability density functions f (M-1, q, P, e) not equal f (M-1) f (q) f (P) f (e) to the corrected distributions, which can be incorporated into binary population synthesis studies.
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Samadov, Hidayat. "Analyzing Reservoir Thermal Behavior By Using Thermal Simulation Model (sector Model In Stars)." Master's thesis, METU, 2011. http://etd.lib.metu.edu.tr/upload/12613336/index.pdf.

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It is observed that the flowing bottom-hole temperature (FBHT) changes as a result of production, injection or shutting the well down. Variations in temperature mainly occur due to geothermal gradient, injected fluid temperature, frictional heating and the Joule-Thomson effect. The latter is the change of temperature because of expansion or compression of a fluid in a flow process involving no heat transfer or work. CMG STARS thermal simulation sector model developed in this study was used to analyze FBHT changes and understand the reasons. Twenty three main and five additional cases that were developed by using this model were simulated and relation of BHT with other parameters was investigated. Indeed the response of temperature to the change of some parameters such as bottom-hole pressure and gas-oil ratio was detected and correlation was tried to set between these elements. Observations showed that generally FBHT increases when GOR decreases and/or flowing bottom-hole pressure (FBHP) increases. This information allows estimating daily gas-oil ratios from continuously measured BHT. Results of simulation were compared with a real case and almost the same responses were seen. The increase in temperature after the start of water and gas injection or due to stopping of neighboring production wells indicated interwell communications. Additional cases were run to determine whether there are BHT changes when initial temperature was kept constant throughout the reservoir. Different iteration numbers and refined grids were used during these runs to analyze iteration errors
however no significant changes were observed due to iteration number differences and refined grids. These latter cases showed clearly that variations of temperature don&rsquo
t occur only due to geothermal gradient, but also pressure and saturation changes. On the whole, BHT can be used to get data ranging from daily gas-oil ratios to interwell connection if analyzed correctly.
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Joseph, Craig L. "Q-nucleosynthesis : implications for stellar evolution /." The Ohio State University, 1985. http://rave.ohiolink.edu/etdc/view?acc_num=osu1487260531956577.

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Murphy, Simon James. "Investigating the A-type stars using Kepler data." Thesis, University of Central Lancashire, 2013. http://clok.uclan.ac.uk/9635/.

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Rotation is a key physical process operating in the A stars. We present a method by which rotation periods might be measured with Fourier transforms of Kepler data, potentially removing the requirement of spectroscopic observations to acquire similar information. Angular rotational velocities reach their maximum at about A5, but slowly rotating A stars are also seen and these tend to be chemically peculiar. For Ap stars, rotational braking is understood, but too few progenitors are observed. A review of a rare class of stars, the ‘sn’ stars, leads us to suggest these may contribute to the ‘missing’ Ap progenitors. For Am stars, we find the tidal braking mechanisms proposed in the literature induce mixing that is incompatible with observed abundance anomalies. At the other end of the scale are the λ Boo stars, whose rotation velocities are above average. The two main theories for the origin of their metal underabundances are discussed and it is suggested that both of them imply the λ Boo stars contain a high fraction of pulsators – a suggestion that is backed up by observations in the literature. Many λ Boo stars also have circumstellar material, suggesting they are potential planet hosts. This, and the use of asteroseismology to study their interiors, are two excellent reasons to adopt them as prime targets for detailed investigation with Kepler. Pulsation is a common phenomenon in A stars. The δ Sct stars receive wide attention but the fraction of stars that pulsate at the 50 μmag level is shown to be only 56 per cent. The non-δ Sct stars in the δ Sct instability strip receive far less attention. Some of these stars, without appreciable granulation or stellar winds, are probably the least variable objects on the HR diagram. It is shown that they have the potential to be among the most peculiar Am stars. Their investigation has led to two important conclusions: (1) the presence of γ Dor pulsation in non-δ Sct stars in the δ Sct instability strip may inhibit the development of the expected Am peculiarities; and (2) chemically normal, non-δ Sct stars in the δ Sct instability strip do exist at the μmag level. Fourier transforms are invaluable tools in the field of stellar pulsation. The Kepler Space Telescope is providing data of exquisite precision, and thus more detail is seen in the Fourier transform than ever before. Truly understanding the properties of the data is fundamental to their successful utilisation. Through statistical analysis of noise levels in over 20 000 stars, granulation is concluded to be visible in Fourier transforms of stars cooler than 7500 K. Another property investigated is the Nyquist frequency. We found that periodically modulated sampling on board Kepler allows distinction between real pulsation frequencies and Nyquist aliases, even when those real frequencies exceed the Nyquist frequency of the data. This discovery opens up study of many hundreds of stars previously thought to have insurmountable Nyquist ambiguities in their data.
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Brookes, Diane Patricia. "Interferometric radio observations of the interactive winds of massive stars." Thesis, University of Birmingham, 2016. http://etheses.bham.ac.uk//id/eprint/6749/.

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Massive stars have very strong stellar winds which interact with their environment. This work has involved the study of these interactive winds at radio and other wavelengths. Radio observations have been made of the massive runaway star BD+43◦ 3654 and its bow shock which is interacting with the inter-stellar medium. These observations, together with archive data at other wavelengths, have revealed stratified dust and turbulent gas in this interaction zone. Further radio studies have been undertaken of the interaction zones of the colliding winds of massive binary systems. Observations of the colliding wind binary WR 147 at 5GHz have revealed a curved collision zone, suggestive of simple interactive models. Measurements of the flux from the Wolf-Rayet component of this massive binary system has allowed a mass-loss rate to be derived and though the companion O-star is not detected, an upper flux limit has allowed upper limits on the mass-loss rate and limits on the terminal velocity to be inferred. Also revealed is a curious ’bridge’ feature previously observed in WR 147 which occurs between the two binary components. One mechanism is suggested to explain this anomalous feature, the ionising flux of one binary component, the O-star, may be ionising the wind of the other, the WR component. Modelling of the ionisation structure of the stellar winds has been undertaken to verify that this may be occurring. Radio observations of massive stars made at low-frequency have produced detections of WR 147 and the brighter colliding wind binary, WR 146. These detections have allowed modelling of the non-thermal emission in order to deduce where the non-thermal absorption turn-over occurs in these systems. The resultant modelling has illustrated that these colliding wind regions are complex, with multiple absorption regions best describing their nature.
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Claas, Ralf Frederik [Verfasser], zu Heringdorf Dagmar [Akademischer Betreuer] Meyer, and Holger [Akademischer Betreuer] Stark. "Regulation der Sphingosinkinase-1 durch G alpha q / Ralf Frederik Claas. Gutachter: Holger Stark ; Dagmar Meyer zu Heringdorf. Betreuer: Dagmar Meyer zu Heringdorf." Frankfurt am Main : Univ.-Bibliothek Frankfurt am Main, 2012. http://d-nb.info/1044093684/34.

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Müller, Stefanie. "Improving the Usability of a Q&A Platform : A design process based on the principles of Lean UX – adapted to a given start-up environment." Thesis, Tekniska Högskolan, Högskolan i Jönköping, JTH, Datateknik och informatik, 2019. http://urn.kb.se/resolve?urn=urn:nbn:se:hj:diva-45309.

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This Bachelor thesis is about digital tools for event organisers. The platforms offered by companies serve as digital backchannels that among other things facilitate interactions between audience and stage, for example during live Q&A sessions. This work focuses on the tasks and challenges of moderators on site and aims to develop a system that will optimise their workflows. Therefore, a tool is developed that allows moderators to conduct a Q&A session independently without having to rely on the assistance of an event organiser operating a desktop based platform simultaneously. The analysis addresses the moderator's role and tasks. It turns out that the functions of the platform relevant to the moderator can be combined in a mobile interface that is linked to it. Using a semi- structured expert interview, the feedback from clients of the start-up "Happenn" is gathered, which use the already existing platform of the company. Their platform "Happenn Live" serves as case study for this thesis. On the basis of the findings of the methods adapted to Lean UX, a solution approach in the form of a redesign of the platform and a corresponding mobile application for moderators is conceptualised. The structure and visual design of the platform follows the general design standards for desktop- and mobile-based interfaces. In this way, an improved usability can be achieved by making the platform more user-friendly for the user.
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Felicetti, Roberto. "Field Current Control for the Damping of Rotor Oscillations and for the Alternative Start of Synchronous Machines : Further Innovative Applications of Field Current Active Control besides UMP-Compensation." Thesis, Uppsala universitet, Institutionen för teknikvetenskaper, 2018. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-353669.

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The possibility to save energy in synchronous machines operation by dismissing d-axis damping bars and surrogating them with active excitation current control in sectored field winding is proved. In particular a way to recover the energy of rotor oscillations during power regulation is shown by means of a studycase generator whereas a self-starting machine is analytically and numerically designed in view of its next construction and test. Principal design requirements and limits for both applications are presented and discussed.
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Books on the topic "Q-stars"

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Luke, Crampton, ed. Q encyclopedia of rock stars. London: Dorling Kindersley, 1996.

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Inc, Game Counselor. Game Counselor's Answer Book for Nintendo Players. Redmond, USA: Microsoft Pr, 1991.

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Inc, Game Counsellor, ed. The Game Counsellor's answer book for Nintendo Game players: Hundredsof questions -and answers - about more than 250 popular Nintendo Games. Redmond, Washington: Microsoft Press, 1991.

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Awesome Super Nintendo Secrets 2. Lahaina, USA: Sandwich Islands Publishing, 1993.

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Crampton, Luke, and Daffyd Rees. Q Rock Stars Encyclopedia. Edition Olms, 1999.

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Thomson, Sarah L. Extreme Stars! Q&A (Smithsonian Q & A (Children's Paperback)). Collins, 2006.

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Thomson, Sarah L. Extreme Stars! Q&A (Smithsonian Q & A (Children's Paperback)). Collins, 2006.

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Extreme Stars! Q&A (Smithsonian Q & A (Children's Cloth)). Collins, 2006.

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Thomson, Sarah L. Extreme Stars! Q&A (Smithsonian Q & A (Children's Cloth)). Collins, 2006.

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Tracer, Grey. Q Stars and Neighbors: Meet Ace and K. Independently Published, 2017.

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Book chapters on the topic "Q-stars"

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Lynn, B. W. "Q-Stars." In Phase Structure of Strongly Interacting Matter, 204–15. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-642-87821-3_7.

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Aidelman, Yael, Carlos Escudero, Franco Ronchetti, Facundo Quiroga, and Laura Lanzarini. "Reddening-Free Q Indices to Identify Be Star Candidates." In Communications in Computer and Information Science, 111–23. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-61218-4_8.

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Deutsch, Nurit Novis, and Maria Klingenberg. "Who Relates to the Divine as Feminine? Transnational Consensus and Outliers Among Young Adults." In The Diversity Of Worldviews Among Young Adults, 133–51. Cham: Springer International Publishing, 2022. http://dx.doi.org/10.1007/978-3-030-94691-3_7.

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AbstractA Q-analysis generally favors large inter-group differences, whereas consensual statements that are shared by most participants tend to receive less attention, as do unusual views, which characterize small groups of participants. In this chapter, we start by exploring consensus statements and offer some thoughts on their meaning. We then consider views that are outside of the individual horizons of most participants. We identified these views through statements towards which most of the samples tended to be indifferent or neutral.Against the backdrop of these transnational statement preferences, we proceed to discuss irrelevant statements through the lens of “religious outliers”; individuals for whom the statements in question were, in fact, highly relevant and important. We then attempt to characterize these “types” through sets of statements, which were not part of any national prototype, and analyze the subjectivities of those who endorse them, by presenting holistic analyses of their interview narratives. Jointly, these analyses help us assess to what extent we can set aside the idea of national-cultural boundaries in favor of other levels of FQS statement analysis – the transnational and the idiosyncratic.
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"Q." In Shooting Stars of the Small Screen, 269–70. University of Texas Press, 2009. http://dx.doi.org/10.7560/718494-020.

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Fahlstedt, Kim Khavar. "Charlie Chan’s Last Mystery, or the Transcultural Disappearance of Warner Oland." In Nordic Film Cultures and Cinemas of Elsewhere, 42–52. Edinburgh University Press, 2019. http://dx.doi.org/10.3366/edinburgh/9781474438056.003.0003.

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This chapter investigates the transnational film persona of Warner Oland. Alongside Anna Q. Nilsson and Greta Garbo, Oland was one of Sweden’s first, and internationally most beloved, Hollywood film stars. During the 1920s and 30s, Oland gained global popularity for roles as Orientalist characters such as Dr. Fu Manchu and Charlie Chan. This case study probes into the last two years of Oland’s life, in which his fame rose to a career high while he was also struggling in his personal life from years of alcohol abuse. It investigates how a range of fleeting conceptualizations of national and ethnic identifiers, such as “Swedishness” and Orientalism, were utilized as heuristic tools to make sense of Oland's public disintegration. In the present study, Oland’s racialized and ethnic personae were reproduced and renegotiated within three geographical locations (Hollywood, Europe, and China) of that period’s transnational film culture.
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Chuang, Ching-Ho. "Allmächtig oder hochmütig? Q in Star Trek." In Superbia – Hochmut und Stolz in Kultur und Literatur, 183–212. Psychosozial-Verlag, 2014. http://dx.doi.org/10.30820/9783837969047-183.

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"q-Analogs of Multiple Harmonic (Star) Sums." In Series on Number Theory and Its Applications, 279–304. WORLD SCIENTIFIC, 2016. http://dx.doi.org/10.1142/9789814689403_0009.

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"q-Analogs of Multiple Zeta (Star) Values." In Series on Number Theory and Its Applications, 365–417. WORLD SCIENTIFIC, 2016. http://dx.doi.org/10.1142/9789814689403_0012.

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Briscoe, J. "The Language and Style of the Fragmentary Republican Historians." In Aspects of the Language of Latin Prose. British Academy, 2005. http://dx.doi.org/10.5871/bacad/9780197263327.003.0003.

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This chapter starts by describing the nature of the evidence of the language and style of the fragmentary republican historians. It also refers to a number of usages which are absent, or virtually absent, from Cicero and Caesar: some of these are found in Latin – primarily, of course, in poetry – of a time before that of the historian concerned, while others occur for the first time in the author in question. The chapter specifically discusses archaisms and neologisms. It also reports the successors of Cato I. The verbatim fragments of L. Cassius Hemina, Q. Fabius Maximus Servilianus, L. Calpurnius Piso, C. Fannius and Cn. Gellius, L. Coelius Antipater, Sempronius Asellio, Q. Claudius Quadrigarius, Valerius Antias, L. Cornelius Sisenna, and C. Licinius Macer are then explored. The surviving longer fragments, with a few exceptions, exhibit a simple sentence structure, with a minimum of subordination.
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Dyer, Dr Karen. "1. Exam Skills for Success in Tort Law." In Concentrate Questions and Answers Tort Law, 1–4. Oxford University Press, 2019. http://dx.doi.org/10.1093/he/9780198745297.003.0001.

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Each Concentrate revision guide is packed with essential information, key cases, revision tips, exam Q&As, and more. Concentrates show you what to expect in a law exam, what examiners are looking for, and how to achieve extra marks. This chapter discusses ways to achieve a good grade for a law exam. The basis for a good grade in tort law is a detailed understanding of the law of tort and developing a systematic approach to using one's knowledge of law to answer examination questions. The preparations for success include attending all lectures and seminars/tutorials; reviewing previous exam papers; start revising early; and being aware of the date, time, and venue of the exam.
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Conference papers on the topic "Q-stars"

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Verbin, Y., Arttu Rajantie, Carlo Contaldi, Paul Dauncey, and Horace Stoica. "Sigma Model Q-balls and Q-Stars." In PARTICLES, STRINGS, AND COSMOLOGY. AIP, 2007. http://dx.doi.org/10.1063/1.2823779.

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VERBIN, Y. "SOLITONIC AND NON-SOLITONIC Q-STARS." In Proceedings of the MG11 Meeting on General Relativity. World Scientific Publishing Company, 2008. http://dx.doi.org/10.1142/9789812834300_0396.

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Seleznev, A. F., and A. A. Malofeeva. "A search of unresolved binaries in open clusters by the photometry data in visible and infrared." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.194.

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The general idea is to find the photometric diagram where the unresolved binary stars are well detached from the singlestars, even for small values of the component mass ratio q. We use the diagram (H-W2)-W1—W2-(BP-K) to estimate thebinary and multiple star ratio and the distribution of q for the Pleiades in the primary component mass interval between0.5 and 1.8 solar masses. A large number of binaries with secondary components being brown dwarfs or stars with theremnants of protostellar discs providing slight infrared excess are among the low-mass stars with the mass of the primarycomponent lower than 0.5 solar masses.
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Mustonen, M. T., J. Suhonen, Livius Trache, Alexei Smirnov, and Sabin Stoica. "Beyond low beta-decay Q values." In EXOTIC NUCLEI AND NUCLEAR∕PARTICLE ASTROPHYSICS (III): From Nuclei to Stars. AIP, 2010. http://dx.doi.org/10.1063/1.3527233.

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Bock, J., N. Bangemann, and S. Paepke. "Which breast scar is the breast-Q star?" In 41. Jahrestagung der Deutschen Gesellschaft für Senologie e.V. – Gemeinsam gegen Brustkrebs: optimale Behandlung für jede Patientin. Georg Thieme Verlag, 2022. http://dx.doi.org/10.1055/s-0042-1748350.

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Frey, Robert, and Bruno Thedrez. "Interpretation of Intracavity Instabilities in Terms of Dynamic Stark Effect." In Optical Bistability. Washington, D.C.: Optica Publishing Group, 1988. http://dx.doi.org/10.1364/obi.1988.we.7.

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Xiong, Wei, and Ana V. Stankovic. "Program start fluorescent ballast with clamped-Q resonant filament heating circuit." In 2014 IEEE Industry Applications Society Annual Meeting. IEEE, 2014. http://dx.doi.org/10.1109/ias.2014.6978433.

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Cherepashchuk, A. M., T. S. Khruzina, and A. I. Bogomazov. "Parameters of Sco X-1." In ASTRONOMY AT THE EPOCH OF MULTIMESSENGER STUDIES. Proceedings of the VAK-2021 conference, Aug 23–28, 2021. Crossref, 2022. http://dx.doi.org/10.51194/vak2021.2022.1.1.039.

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We modelled optical light curves of Sco X-1 obtained by the Kepler K2 mission. We calculated the ratio of the mass of therelativistic object to the mass of the optical star q = M x /M v = 3.6 (3.5 − 3.8) and the orbital inclination i = 30 ◦ (25 ◦ − 34 ◦ ).
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Andriollo, M., G. Bettanini, G. Martinelli, A. Morini, and A. Tortella. "Analysis of Double Star Permanent Magnet Synchronous Generators by a General Decoupled d-q Model." In 2007 IEEE International Electric Machines & Drives Conference. IEEE, 2007. http://dx.doi.org/10.1109/iemdc.2007.383544.

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Buyalo, M. S., I. M. Gadzhiyev, N. D. Il'inskaya, A. A. Usikova, V. N. Nevedomskiy, A. Yu Egorov, and E. L. Portnoi. "Mode-locking and Q-switching in 1.06 μm two-sectional QW lasers due to stark effect." In 2016 International Conference Laser Optics (LO). IEEE, 2016. http://dx.doi.org/10.1109/lo.2016.7549717.

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Reports on the topic "Q-stars"

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Hochron, D. R., B. W. Lynn, and S. B. Selipsky. An upper bound on Q-star masses. Office of Scientific and Technical Information (OSTI), June 1992. http://dx.doi.org/10.2172/94554.

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Farahbod, A. M., and J. F. Cassidy. An overview of seismic attenuation in the Eastern Canadian Arctic and the Hudson Bay Complex, Manitoba, Newfoundland and Labrador, Nunavut, Ontario, and Quebec. Natural Resources Canada/CMSS/Information Management, 2022. http://dx.doi.org/10.4095/330396.

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In this study we investigated coda-wave attenuation (QC) from the eastern Canadian Arctic in Nunavut and the Hudson Bay complex including portions of northern Manitoba, Ontario, Quebec and Labrador. We used earthquake recordings from 15 broadband and 3 short period seismograph stations of the Canadian National Seismic Network (CNSN) and 29 broadband stations of the POLARIS network across the region. Our dataset is comprised of 637 earthquakes recorded between 1985 and 2021 with magnitudes ranging from 1.3 to 6.1, depths from 0 to 20 km and epicentral distances of 5 to 100 km. This gives a total of 246 high signal-to-noise (S/N) traces (S/N[lesser/equal]5.0) useful for QC calculation (with a maximum ellipse parameter, a2, of 100) across the region. Coda windows were selected to start at tc = 2tS (two times the travel time of the direct S wave), and were filtered at center frequencies of 2, 4, 8, 12 and 16 Hz. Our study reveals a consistent pattern. We find that in the northern section of the study area, the highest Q0 values (e.g., Q0 of 110 and 112) are at station POIN and station RES, respectively, which are located in the older Archean province. The lowest Q0 values that we find (e.g., Q0 of 55 and 61) are at station AKVQ and IVKQ respectively, located in northern Quebec. Smaller Q0 values for stations in the south are explained by the younger age of the rocks and proximity to the main fault systems. An average for all the data results in a Q relationship of QC = 82f1.08 for the frequency band of 2 to 16 Hz for the entire region.
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Farahbod, A. M., and J. F. Cassidy. An overview of seismic attenuation in the Northern Appalachians Seismic Zone, New Brunswick and Nova Scotia. Natural Resources Canada/CMSS/Information Management, 2022. http://dx.doi.org/10.4095/329702.

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In this study we investigated coda-wave attenuation (QC) from the northern Appalachian region of eastern Canada in the two provinces of New Brunswick and Nova Scotia. We used earthquake recordings from 8 broadband and 2 short period seismograph stations of the Canadian National Seismograph Network (CNSN) across the region. Our dataset is comprised of 476 earthquakes recorded between 1983 and 2021 with magnitudes ranging from 1.5 to 4.1, depths from 0 to 20 km (with the vast majority being &amp;lt;10 km) and epicentral distances of 5 to 100 km. This gives a total of 261 high signalto- noise (S/N) traces (S/N greater than or equal to 5.0) useful for QC calculation (with a maximum ellipse parameter, a2, of 100) across the region. Coda windows were selected to start at tc = 2tS (two times the travel time of the direct S wave), and were filtered at center frequencies of 2, 4, 8, 12 and 16 Hz. Our study reveals a consistent pattern. We find that in the northern New Brunswick, the lowest Q0 values (e.g., Q0 of 61) are at station KLN which is the closest station to the epicenter of the 1982 Miramichi earthquake (M 5.8). The highest Q0 values that we find (e.g., Q0 of 178) are at station GGN, located in the southern New Brunswick. Smaller Q0 values for stations in the north (closer to the Charlevoix-Kamouraska seismic zone or Miramichi source area) is explained by Jin and Aki's (1988) finding that Q0 is lower in the vicinity of large earthquakes. An average for all the data results in a Q relationship of QC = 99f0.96 for the frequency band of 2 to 16 Hz for the entire region.
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