The world first heard of Sun Yat-sen in 1896 when the British government intervened to save him from deportation to Chine as a refugee. A decade and half later the public read with amazement that this name refugee had lived to be proclaimed the First President of the Republic of China. This men conspirator, a "visionary", socialist dreamer, a fighter for right end Justice became the hero and idol of the Chinese people. Today he is held in greater entres then any living statesmen or any political philosopher of the pet century. The respect mid his memory is paralleled in Chinese history only by the veneration due Confucius. His ultimate position in Chinese history is yet to be determined, but five years after his death he lives in the hearts of the people as the nation's greatest lender and as the outstanding figure of the Chinese Revolution

In this Licentiate thesis I review the properties of the solar atmosphere and the diagnostic value ofdifferent spectral lines in the visible and ultraviolet (UV) along with the millimeter (mm) continua in theelectromagnetic spectrum of the Sun.While the solar atmosphere has been routinely observed in high-resolution from ground-based opti-cal telescopes such as the Swedish Solar Telescope (SST), and more recently in the UV from space tele-scopes such as the Interface Region Imaging Spectrograph (IRIS), radio observations lag behind despitetheir great usefulness. This is likely to change thanks to the Atacama Large Millimeter Array (ALMA)that only started observing the Sun in 2016 with a few limitations, but the first results are promising.ALMA observations probe the solar chromosphere at different heights by tuning into slightly differentfrequencies at potentially milliarcsecond scales if the full array is able to operate with the longest base-lines. This new spectral window onto the Sun is expected to advance various fields of research suchas wave propagation and oscillations in the chromosphere, thermal structure of filaments/prominences,triggering of flares and microflares, and more generally chromospheric and coronal heating, because themm-intensities can be modelled by simply assuming local-thermodynamic equilibrium.In da Silva Santos et al. (2018) we find that coordinated observations from SST, IRIS and ALMA willpermit us to estimate with greater accuracy the full thermodynamical state of the plasma as a functionof optical depth based on experiments with a snapshot of a three-dimensional magnetohydrodynamicsimulation of the Sun’s atmosphere. Particularly, the mm-continuum improves the accuracy of inferredtemperatures in the chromosphere. Here we expand on the Why and How this can be done. The goal isto better constrain the temperature stratification in the solar atmosphere in order to understand chromo-spheric heating.

Solar plage has been the topic of many studies since its initial description in the mid 19th century, but as of yet it has not been understood to the point where we can reproduce all aspects of these active regions in quasi-realistic numerical models. To a large extent, this is caused by an incomplete understanding of the magnetic structure that drives the activity in these areas. Detailed measurements have been done of the magnetic field configuration of plage in the photosphere since the late 20th century, but only a handful of papers have managed to make any measurements at all in the higher situated chromosphere, despite the fact that the magnetic field vector of plage is important in understanding chromospheric magnetic fields in general, as well as the heating processes of the higher atmosphere. In Pietrow et al. (2020) we add to these measurements by introducing what is to our knowledge the first full Stokes inversion of chromospheric plage, which allowed us to estimate the magnetic field vector at an optical depth of logτ = -3.5. The obtained value is |B| = 440 ± 90 G in the plage with an inclination of 10° ± 16° with respect to the local vertical. Our reported magnetic field strength matches with a recent study by Morosin et al. (2020), but is higher by a factor of two or more compared to previous studies that measured the field using other methods. Additionally we measure an average magnetic field strength of |B| = 300 ± 50 G in a fibrillar region close to the plage. In this thesis we explore the difficulties of measuring this magnetic field vector. Since plage exists in a complex environment, we will begin with a general description of the structure and properties of the solar atmosphere and the layers from which it is composed, as well as review the types of active regions that can be found in the solar atmosphere. Our focus then narrows to the chromosphere, the diagnostic properties of spectral lines that are sensitive to this layer (mainly the \cair line), plage regions, and plage chromospheric magnetic fields. Additionally, we touch upon the theory of radiative transfer and how physical characteristics of the atmosphere can be inferred from polarised light. We also give attention to the observing process with the Swedish 1-m Solar Telescope (SST) and the workings of the reduction pipeline and post-reduction methods as well as the process spectropolarimetric inversions. Finally, once we have understood why and how this project has been done, we summarize our findings and compare them to current literature.

The purpose of this study was to write a history of the Price, Utah Sun-Advocate and its predecessors, the six early newspapers which evolved into the present Sun-Advocate, with primary emphasis on the personalities involved, the physical changes and the editorial comment. Major economic, political, and social changes were noted as they occurred in the chronological history.

In several areas around the world, clean water is a precious asset that at anytime, and mainly due to circumstances of weather and climate, can become scarce. Mainly in the dry and remote places, people suffer with lack of water. A solution for this suffering can be a water desalination system, which makes water potable and usable for industry. That solution inherently, brings the problem of power requirement, which is sometimes arduous to accomplish in such remote areas of difficult access and long distances to overcome to build the infrastructure required to operate an electric power plant. Texas and the USA also face this scenario for many regions, for which the government has been creating some programs and driving forward incentives, looking for solutions to support water desalination. Water desalination has future applications for municipalities water-consuming or for arid and remote regions, as well as for industries that rely on heavy water usage, such as natural gas drilling operations, for which millions of gallons are trucked overland to the site and also hauled away afterwards, when the waste water produced must be treated. This thesis created the concept of autonomy for water desalination plants replacing the actual power supply from fossil fuel to a renewable source from wind or sun, giving capacity to them to produce its own electricity to operate as an autonomous unit, as demonstrated in the business case done for the Brownsville water desalination facility.

When the Sun Hits is a feature length film concerned with the delicate relationship between the individual and the whole. A young man named John has fallen into a state of social paralysis since his father's death. He no longer knows how to relate to others and the world around him. Rather than looking to friends and family for support he closes himself off. After the mysterious disappearance of his mother, John blames himself for her leaving. He tries his best to reconnect with his old life, but finds himself making the same mistakes over and over. When his friend Tracy reaches out to him, he bitterly rejects her and once again finds himself alone. It is then that John puts his old life behind him and sets off to make amends with his mother. John has no idea where his mother might be or if she will accept him. Nonetheless, he reaches into the abyss to see if someone is there, waiting for him. The structure of the film is nonlinear as it deviates from traditional narrative form. The intent of this thesis is to serve as a post-film reflection that discusses the relation between my views on cinema and the film I made. The paper will shift between the general themes of the narrative and the film theory working behind it all. It will explore the idea of cinema as an extension of the mind and how this is present in the film. By using specific examples from the film this theory of cinema can be fleshed out and an insight into my process may be gleaned.

Saturn's rings are a complex, dynamic system that can provide unique insight into the structure and features of the planet and surrounding system. We use stellar occultation data of Saturn's rings collected from the Cassini Ultraviolet Imaging Spectrograph to visualize and analyze bending waves present within the rings. Analysis of the propagation of these waves gives insight into the surface mass density of the local ring region and can be used to further our understanding of ring dynamics and ring formation. Our analysis of the Mimas 7:4 bending wave estimated a surface mass density between 30 g cm-2 and 43 g cm-2, corroborating the findings of Spilker et al. (2004) of 47 ± 6.2 g cm-2 and supporting our current understanding of linear wave theory. Our analysis of the Mimas 4:2 bending wave estimated the surface mass density to be between 33 g cm-2 and 47 g cm-2 and was of particular interest since this wave is found in the relatively uncharacterized B ring region.

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