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ABSTRACT A documentation and analysis of the impact of new technologies on the design and layout of The Star, particularly desktop publishing hardware and software, digital photography and the Internet. A broad outline of the production and editorial technology employed prior to the introduction of fourth wave in 1995 is provided to contextualise the research. A systematic visual analysis of selected pages from the 1920s to present as well as interviews with key members of staff from The Star, who have experienced the evolution of the paper first-hand, provide the primary source of information for the study. To prevent the paper from becoming too anecdotal, the organisational approach to the study of the media and theory of visual culture provide the theoretical framework. The research concludes that new technology itself has not drastically affected the design and layout of The Star over the past decade, but rather stimulated change within the organisational environment, which gradually did affected the visual appearance of the paper.

Presented in this thesis are measurements of W boson production in high energy pp collisions and ep deep inelastic scattering that take place at RHIC and HERA facilities, respectively. These measurements explore the inner structure of the nucleons, in particular, probing the distributions of the light flavor sea which consists of up, down and strange quarks. The W+/W− cross-section ratio, RW , in pp collisions is sensitive to the asymmetry in the ¯d and ¯u flavors in the nucleon sea. This ratio was first measured with the STAR detector at RHIC with the data collected in 2009 and again with the data collected from 2011 to 2013, featuring pp collisions of a center-of-mass energy of √s = 500/510 GeV and an integrated luminosity of ∼ 350 pb−1. The study considered in this thesis further improves the precision of this measurement by analyzing an additional data set collected in 2017 which corresponds to an integrated luminosity of ∼ 350 pb−1. The experimental results are compared to theory predictions generated with various global PDF fits. The measurement performed at HERA searches for the strange quark content in the nucleon via charm production in charged current deep inelastic scattering. This is the first measurement of its kind, using the HERA II data collected with the ZEUS detector. This data set corresponds to e±p collisions at a center-of-mass energy of √s = 318 GeV with an integrated luminosity of 358 pb−1. The results are consistent with expectations from the Standard Model, albeit with large experimental uncertainties arising from the limited statistics. / Physics

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Star formation is a complex hierarchical process that witnesses the transfer of mass among a range of scales from large diffuse molecular clouds to crowded clumps and finally down to prestellar cores. The final stage of this process has prestellar cores actively accreting matter while undergoing gravitational collapse on their way to becoming main sequence stars. This thesis presents multi wavelength submillimeter observations of the Perseus molecular cloud using 160 μm, 250 μm, 350 μm, and 500 μm maps of thermal dust emission from the Herschel space observatory. Additionally C18O J = 3 → 2 spectral line emission is observed in four star forming clumps within Perseus using the James Clerk Maxwell Telescope. Spectral line emission allows for the separation of material along the line of sight. Prestellar core mass is derived from observational maps using various source finding algorithms. The mass is overestimated when compared to prestellar core mass found from spectral line data. This overestimation can be mitigated with careful selection of source finding algorithm and background removal. Further, the prestellar core mass derived from spectral line data was the closest match to the initial stellar mass function over dust maps. However, both the spectral line masses and dust map masses do not agree with the IMF confirming a star forming efficiency factor in the evolutionary step between prestellar core and main sequence star. Lastly, a filamentary analysis finds that high mass stars preferentially form in crowded regions close to, or contained within, filament structure. / Thesis / Master of Science (MSc) / Star formation is a complex hierarchical process that witnesses the transfer of mass among a range of scales from large diffuse molecular clouds to crowded clumps and finally down to prestellar cores. The final stage of this process has prestellar cores actively accreting matter while undergoing gravitational collapse on their way to becoming main sequence stars. This thesis presents multi wavelength submillimeter observations of the Perseus molecular cloud using 160 μm, 250 μm, 350 μm, and 500 μm maps of thermal dust emission from the Herschel space observatory. Additionally carbon monoxide spectral line emission is observed in four star forming clumps within Perseus using the James Clerk Maxwell Telescope. Spectral line emission allows for the separation of material along the line of sight. Prestellar core mass is derived from observational maps using various source finding algorithms. The mass is overestimated when compared to prestellar core mass found from spectral line data. This overestimation can be mitigated with careful selection of source finding algorithm and background removal. Further, the prestellar core mass derived from spectral line data was the closest match to the initial stellar mass function over dust maps. However, both the spectral line masses and dust map masses do not agree with the IMF confirming a star forming efficiency factor in the evolutionary step between prestellar core and main sequence star. Lastly, a filamentary analysis finds that high mass stars preferentially form in crowded regions close to, or contained within, filament structure.

I investigate the observational signatures of the formation of dark matter cores in dwarf galaxies. I adopt the paradigm where the energy from star formation feedback is injected into the orbits of dark matter particles, forming a constant density core consistent with observations of dwarf galaxies. Using physically motivated constraints I show there is ample feedback energy available given the average stellar mass of dwarf galaxies to form cores in $10^{8}$--$10^{11}$\thinspace M$_{\odot}$ halos, and predict the maximum core size as a function of stellar mass. I describe how observational features of the old stellar content of dwarf galaxies are due to this core formation paradigm. As both dark matter and stars are collisionless fluids, the stars responsible for the feedback form in the centres of dwarf galaxies and have their orbits grown by subsequent star formation. This will naturally lead to age and metallicity gradients, with the younger and more metal rich stellar population near the dwarf centres. This process also prevents the destruction of globular clusters by driving them out of the dwarf nucleus --- the decrease in central dark matter density reduces the strength of dynamical friction --- and increases the likelihood of being stripped onto the stellar halos of larger galaxies. It also offers a model for forming multiple populations in globular clusters, with the only assumption being that the source of the polluted gas resides within the dwarf progenitor. As the orbit of a globular cluster grows, it will experience multiple accretion events with each pass through the gas-rich galaxy centre. The simple accretion model exhibits two traits revealed from observations --- a short accretion timescale and a sensitive dependence on mass --- without requiring an exotic initial stellar mass function or the initial globular cluster mass function to be 10--25 times larger than at present. / Dissertation / Doctor of Philosophy (PhD)

if (){then ();} else {();} uses eight microphones to record sounds from the room for the entire duration of the exhibition. All sounds are archived and then called upon in seemingly random intervals and played from twenty-four speakers set up in the room. The recordings are then layered allowing the past and present to exist simultaneously, creating an interaction with the passage of time. Using analogue methods, mathematics, electronics, and coding languages I am interested in creating interactive sound environments inviting participants to help create the work. Playing with aural phenomena, I focus on basic methods of producing and processing sound to stimulate human interaction and play.

This project aims to obtain and interpret the measurements of the mean longitudinal magnetic field of the chemically peculiar star V1148 Ori. To achieve this aim 12 spectropolarimetric observations obtained by the CFHT using the spectropolarimeter ESPaDOnS were used. The method used to extract the magnetic field signatures from the spectra is called least-squares deconvolution. This method yields line-averaged profiles with a high signal-to-noise ratio. These mean line profiles are necessary to compute the mean longitudinal field. Results of the mean longitudinal field measurements were plotted as a function of the rotational phase, and to this, a sinusoidal function describing a dipolar field was fitted. The dipolar field parameters were computed for two different stellar radii. Inconsistent values for the stellar radii were obtained from the literature, and therefore we calculated two values for each of the parameters. For the surface polar field strength, we found BR1 = 17.38±0.30 kG and BR2 = 12.81±0.22 kG. The calculations involving one of the stellar radii gave results more consistent with previous findings. However, the discrepancy in parameter values could not be accounted for by the small uncertainties. So no definite conclusions can be drawn about the dipolar field parameters. Our fit aligns well with our longitudinal field measurements, no clear indication of any significant deviation from our model assumption, which suggests that the mean longitudinal field is consistent with a large-scale dipolar-like structure.

(Field Trip Activities in Prague Focusing on the Star Game Reserve and Their Application and Use in the Teaching of Biology) The subject of this diploma thesis are organizational forms of teaching with a focus on excursion activities in science classes at the 2nd level of primary school and in the corresponding years of lower grammar school. The work is clearly divided into several parts. The first part deals with general information about the excursion activity as a whole. It deals with the division of individual excursions, their preparation and course. Subsequently, the possibilities of educational programs in Prague and the surrounding area are characterized, which are prepared from various institutions. Furthermore, the work specifically focuses on the Prague forest in the field of the Star game reserve, because in the last part of the text is made an educational walk connecting the history and nature of this place. An integral part of the work is a questionnaire survey dealing with the use of excursions in science teaching.

Labour in our current dispensation can be understood by critically examining their embeddedness in their geographical spaces and their spatial connection to those geographical spaces. Meanwhile, it has been highly contested by famous economic geographers like Andrew Herod and Don Mitchell, who argues that although labour shapes their economic and political spaces, they do not do this by choice and, as such, their power to make structural changes had been overemphasised. Therefore, a further study into other structures in which labour works and live can help reveal the extent of their influence on structures of any kind. Mainly, working conditions are essential for workers, and this study contests their power of influence on them. Notably, working conditions are formulated by the employers basing their decisions on their societal values, morals, and other factors. In order to understand the interplay of these components in influencing the decision of employers on working conditions, ethical leadership at the workplace is necessary to be studied to uncover how employers' ethical stances influence the working conditions of their workers. Particularly, ethical leadership is a complex structure involving a leadership style and ethics that affect employers' decision-making process. This qualitative paper used purposive and snowball non-probability sampling techniques to select participants from Holiday Club Åre and Ski Star Åre. The results from this study show that ethical leadership influences working conditions and it existed within the two workplaces even during the pandemic; however, it is unevenly exhibited, and the reason for such disparities can be attributed to the personalistic characteristics of the managers. Namely, ethical leadership and good working conditions lead to a higher level of job satisfaction and trust in leadership, higher productivity, behaviour emulation and reduction in counterproductive behaviour at the workplace. Workers were also found to have a marginal structural impact on their working conditions because of their low bargaining power despite the support of their labour agency. / <p>2022-01-22</p>