Globular Clusters contain very old metal-poor stars in different evolutionary stages evolved from the same primordial cloud. Signatures of atomic in stellar interiors are studied in the metal-poor GC M30. Furthermore, traces of cluster internal pollution depleting alpha elements e.g. Mg & O are also found through high precision spectroscopy, which favors the existence of multiple stellar populations within a Globular Cluster. In this work, I use spectroscopic observations of 177 sample stars using the multi object spectrograph GIRAFFE and increasing the initial size of 12 of Scheutwinkel (2018) by 13 new UVES spectrograph sample stars of the Globular Cluster M30 ([Fe/H] = -2.3). The abundances of Fe, Ti, Mg & Ba (GIRAFFE) and Fe, Na, Al & Mg (UVES) are derived through the graphical spectrum analysis program SIU with VI broadband photometric stellar input parameters. The underlying line-formation theory is in LTE and uses 1-dimensional hydrostatic plan-parallel MAFAGS atmospheres with mixing length convection. We confirm an Al-Mg anti-correlation (Spearman ϱs= -0.583) and a correlation (Spearman ϱs= 0.641) between Al-Na in RGB stars as a direct result of being the partner elements of the depleted alpha elements Mg & O caused through NeNa, ON and MgAl cycles. We find similar element ratios [X/Fe] as Carretta et al. (2018) & O‘Malley et al. (2018) favoring the prior existence of multiple stellar populations within M30. Furthermore, we detected a signifcant restoration of abundances in the elements Fe, Mg & Ba towards RGB stars. Fe, Mg and Ti are matching the predictions of the diffusion model T5.8 (Richard et al. 2005) reasonably well. For Ba, we have no current atomic diffusion modeling, so the validation of the results is not possible. The trend of Ti is v-shaped presumably due to stronger radiative accelaration effects for this element. Overall our relative abundance trends are consistent with other Globular Cluster studies by Gruyters et al. (2013&2016), Korn et al. (2007) & Lind (2007).

<p>The heating of the solar corona has been investigated during four of decades and several mechanisms able to produce heating have been proposed. It has until now not been possible to produce quantitative estimates that would establish any of these heating mechanism as the most important in the solar corona. In order to investigate which heating mechanism is the most important, a more detailed approach is needed.</p><p>In this thesis, the heating problem is approached ”ab initio”, using well observed facts and including realistic physics in a 3D magneto-hydrodynamic simulation of a small part of the solar atmosphere. The ”engine” of the heating mechanism is the solar photospheric velocity field, that braids the magnetic field into a configuration where energy has to be dissipated. The initial magnetic field is taken from an observation of a typical magnetic active region scaled down to fit inside the computational domain. The driving velocity field is generated by an algorithm that reproduces the statistical and geometrical fingerprints of solar granulation. Using a standard model atmosphere as the thermal initial condition, the simulation goes through a short startup phase, where the initial thermal stratification is quickly forgotten, after which the simulation stabilizes in statistical equilibrium. In this state, the magnetic field is able to dissipate the same amount of energy as is estimated to be lost through radiation, which is the main energy loss mechanism in the solar corona.</p><p>The simulation produces heating that is intermittent on the smallest resolved scales and hot loops similar to those observed through narrow band filters in the ultra violet. Other observed characteristics of the heating are reproduced, as well as a coronal temperature of roughly one million K. Because of the ab initio approach, the amount of heating produced in these simulations represents a lower limit to coronal heating and the conclusion is that such heating of the corona is unavoidable.</p>

<p>Jag har tillverkat ett undervisningsmaterial, i form av en serietidning, som riktar sig mot elever i grundskolans tidigare år och i detta arbete utvärderas undervisningsmaterialet. Med syfte att utvärdera undervisningsmaterialet kartlades elevernas förkunskaper med hjälp av ett frågeformulär innan de fick tillgång till serietidningen. Då eleverna haft tillgång till serietidningen i 12 skoldagar gjordes en eftermätning, med samma frågeformulär som använts vid förmätningen, för att se om eleverna tagit till sig det budskap som materialet vill förmedla. Resultatet visade att alla elever utom 2 presterade bättre på eftermätningen än på förmätningen. På alla frågor utom 3 var det fler elever som svarade korrekt vid eftermätningen än det var vid förmätningen. Att alla elever utom två förbättrade sitt resultat efter att ha haft tillgång till serietidningen tyder på att eleverna har tagit till sig undervisningsmaterialets budskap och att utvärderingen av elevernas kunskaper visar det.</p>

<p>Vår världsuppfattning har förändrats genom seklerna. Den länge accepterade geocentriska teorin från antikens Grekland var att solen, planeterna och stjärnorna roterade kring jorden. Andra teorier var inte accepterade av varken kyrkan eller vetenskapen. På 1500-talet publicerades Kopernikus heliocentriska teori, som innebar att solen var i centrum och att jorden och de andra planeterna roterar kring den. Vad Kopernikus försökte åstadkomma var en enklare världsbild än grekernas komplicerade epicykelteori. Hans teori ansågs vara kontroversiell, särskilt eftersom den inte gav några särskilt bättre värden på planeternas positioner än den gamla teorin.</p><p>Den som producerade de data som behövdes var Tycho Brahe, som i slutet av 1500-talet gjorde många upprepade observationer av planeternas lägen med hjälp av egenkonstruerade instrument på ön Ven. Efter hans död i början av 1600-talet fortsatte Brahes assistent Johannes Kepler med att utreda planeternas banor, vilket ledde till hans tre berömda lagar om planeternas rörelse. Lagarna var empiriska matematiska samband som således inte kunde förklara vad som styrde planetrörelsen. Utifrån Keplers lagar kunde därefter Isaac Newton förklara planeternas rörelse med hjälp av sin gravitationslag och de tre rörelselagarna. Med hjälp av Newtons formler så kunde man beräkna planeternas lägen på himlavalvet med godtycklig precision, och inte bara det: Newtons gravitationslag kunde på ett helt nytt sätt kombinera vardagens fall av ett äpple i en trädgård med hur planeterna rör sig utifrån en gemensam beskrivning.</p><p>Denna uppsats kommer att ta upp Keplers och Newtons lagar mer detaljerat och även redogöra för den moderna kunskapen kring solsystemets dynamik och uppbyggnad.</p> / <p>The view of how the Earth and the Sun move has changed through the ages. The idea that was “right", from the time of ancient Greece, was that the Earth was at the centre and everything revolved around it even if some facts were unexplained. It was in the middle of the 1500s that Copernicus developed the idea that Sun was in the centre and the Earth revolved around it. His theory was controversial, especially since it did not improve the positions of the planets very much.</p><p>The person who provided the necessary data was Tycho Brahe. In the late 1500s he observed and logged the planetary positions for many years, using his own instruments on the island of Ven. His assistant Johannes Kepler then used the data to infer his three famous laws of planetary motion. Kepler could not explain why the planets moved according to the laws, since the latter were empirical. Isaac Newton could later on derive Kepler’s laws from his own gravitational law and three laws of motion, thereby confirming Kepler’s result. Newton also provided a great synthesis between local physics (the famous apple falling down) and celestial motion.</p><p>This report will discuss the Kepler and Newton laws in more detail, as well as the modern view of the dynamics and structure of the solar system.</p>

The heating of the solar corona has been investigated during four of decades and several mechanisms able to produce heating have been proposed. It has until now not been possible to produce quantitative estimates that would establish any of these heating mechanism as the most important in the solar corona. In order to investigate which heating mechanism is the most important, a more detailed approach is needed. In this thesis, the heating problem is approached ”ab initio”, using well observed facts and including realistic physics in a 3D magneto-hydrodynamic simulation of a small part of the solar atmosphere. The ”engine” of the heating mechanism is the solar photospheric velocity field, that braids the magnetic field into a configuration where energy has to be dissipated. The initial magnetic field is taken from an observation of a typical magnetic active region scaled down to fit inside the computational domain. The driving velocity field is generated by an algorithm that reproduces the statistical and geometrical fingerprints of solar granulation. Using a standard model atmosphere as the thermal initial condition, the simulation goes through a short startup phase, where the initial thermal stratification is quickly forgotten, after which the simulation stabilizes in statistical equilibrium. In this state, the magnetic field is able to dissipate the same amount of energy as is estimated to be lost through radiation, which is the main energy loss mechanism in the solar corona. The simulation produces heating that is intermittent on the smallest resolved scales and hot loops similar to those observed through narrow band filters in the ultra violet. Other observed characteristics of the heating are reproduced, as well as a coronal temperature of roughly one million K. Because of the ab initio approach, the amount of heating produced in these simulations represents a lower limit to coronal heating and the conclusion is that such heating of the corona is unavoidable.

Barns föreställningar kring naturens olika fenomen är många. Ett fenomen som alla barn upplever varje dag är övergången från dag till natt och tvärtom. För att kunna ge barn förklaringar om hur saker och ting sker och hänger samman, är det viktigt att lyssna på deras föreställningar för att sedan bygga vidare på dessa. För att ta reda på barns föreställningar kring fenomenet dag och natt, har enskilda semistrukturerade intervjuer genomförts med elever i årskurs tre. Resultaten visar att eleverna hade förståelse för att solen, månen, jorden och andra planeter är i ständig rotation. Hur dessa objekt roterar ute i rymden varierade i svaren hos eleverna. Slutsatsen av detta arbete blir att elevernas föreställningar kring fenomenet dag och natt kan kopplas samman med de vetenskapliga förklaringarna samt att de hade förståelse för att olika objekt i rymden ständigt roterar på olika sätt. / Children's conceptions are several about different natural phenomenon. One phenomenon that every child comes in contact with every day is the transition from day to night and vice versa. To be able to give children explanations about thing that happens and how they are connected to each other, it is important to listen to what conceptions they have and then explain on the basis from their conceptions. Individual semi constructed interviews have been made with pupils in 3rd grade to find out what conceptions they have. The results show that the pupils were certain that the sun, the moon, the earth and other planets are rotating out in space varied. The conclusion of this work is that the pupils conceptions about the phenomenon day and night can be connected with the scientific explanations and that they also had understanding about how different objects are rotating in space.

The asymptotic giant branch (AGB) is the last stage of stellar evolution for stars with masses between 0.8-8 M(sun). This phase is characterised by an intense mass loss, which builds up a circumstellar envelope of dust and gas(CSE). It is through this process that the AGB stars contribute to the chemical evolution of galaxies. In addition, a rich and varied chemistry is active within the CSEs.Observations of circumstellar H2O are of particular interest, as it is expected to be one of the most abundant molecules in the inner envelopes of M-type AGB stars (with C/O&lt;1). The first part of this thesis concerns the modelling of water vapour emission lines from CSEs around M-type AGB stars. Using satellite observations and detailed radiative transfer models, H2O abundances in these stars are determined and compared with theoretical chemical models. The importance of resolved H2O line profiles and excitation through different vibrationally excited states are also demonstrated.The second part of the thesis has its focus on the detached shells of dust and gas observed around a handful of carbon AGB stars (with C/O&gt;1), believed to be an effect of highly time-variable mass loss during a thermal pulse. The detached shells around three sources were observed in stellar light scattered by dust and gas in the shells using ground-based and space telescopes. The observations allow a separation of the scattering agents, and reveal information on the detached shells in unprecedented detail. / At the time of the doctoral defense, the following papers were unpublished and had a status as follows: Paper 2: Submitted. Paper 4: In progress.

Jag har tillverkat ett undervisningsmaterial, i form av en serietidning, som riktar sig mot elever i grundskolans tidigare år och i detta arbete utvärderas undervisningsmaterialet. Med syfte att utvärdera undervisningsmaterialet kartlades elevernas förkunskaper med hjälp av ett frågeformulär innan de fick tillgång till serietidningen. Då eleverna haft tillgång till serietidningen i 12 skoldagar gjordes en eftermätning, med samma frågeformulär som använts vid förmätningen, för att se om eleverna tagit till sig det budskap som materialet vill förmedla. Resultatet visade att alla elever utom 2 presterade bättre på eftermätningen än på förmätningen. På alla frågor utom 3 var det fler elever som svarade korrekt vid eftermätningen än det var vid förmätningen. Att alla elever utom två förbättrade sitt resultat efter att ha haft tillgång till serietidningen tyder på att eleverna har tagit till sig undervisningsmaterialets budskap och att utvärderingen av elevernas kunskaper visar det.

2030 NASA Jet Propulsion Laboratory will place an interferometer, which will workas a radio telescope, on the far side of the Moon. The interferometer uses thinpolyamide films as antennas, which are rolled out by a rover (an autonomousvehicle). The thesis covers concept generation of the propulsion and steering systemof the rover.The interferometer is to be placed on the far side of the Moon in order to ensure, asfar as possible, that it is not effected by radiation from Earth. The interferometerconsists of several polyamide films, approximately 100 meters long and one meterwide. The films are to be connected in the middle in order to form a star pattern offilm. Since the rover is to roll out these films on the surface of the Moon, it will driveback and forth to the lander to pick up the rolls. The focus in the project has been todevelop a reliable and stable system as possible so that the rover can accomplish itsmission without malfunctions. The purpose with the interferometer is to map thehydrogen gas clouds which were formed during universe’s youth (Platt, 2008).The outcome of this project is a concept indicating what the most optimal design ofwheel mount, of motor mount, of wheel and steering design may be in order to steerthe rover. The method to generate concepts used is known Fredy Olsson’s method.This is a method that has been developed at Lunds University and it has been widelyused in engineering education at Halmstad University.The four concepts developed and contributes to the whole concept for propulsion andsteering system of the rover. The four concepts developed are an all six steering, allof the six wheels can be controlled individually. Each wheel is split, or divided intwo. The motor is angle mounted and the wheel is semi-open with a slope that makesthe Moon dust fall out if it comes inside.Inspiration from previous rovers which are or have been on the Moon and Mars hasbeen useful in generating concepts. Previously used concepts are stable and reliable,which are important factors in this project. Previous theses have come to theconclusion that the chassis of the rover should be the one similar to the one used onMars Science Laboratory Curiosity and Mars Exploration Rover’s Spirit andOpportunity.The Halmstad University projects in collaboration with NASA began at HalmstadUniversity in 2013, and previous projects have developed the chassis, energy systemand the deployment mechanism of the rover. This year’s project takes intoconsideration the results from previous years since a concept of a complete roverultimately is going to be presented to NASA Jet Propulsion Laboratory.The thesis is done in collaboration with NASA Jet Propulsion Laboratory inCalifornia, USA. NASA Jet Propulsion Laboratory is the leading U.S. center forrobotic exploration of the solar system. / NASA Jet Propulsion Laboratory ska 2030 placera en interferometer på månensbaksida, interferometern ska fungera som ett radioteleskop. Interferometern användersig av tunna polyamidfilmer som antenner. Dessa ska rullas ut på månens yta av enrover (ett obemannat fordon). Rapporten behandlar framtagning av koncept förstyrning och framdrivning av denna rover.Interferometern ska placeras på månens baksida för att man i så stor mån som möjligtvill undkomma strålningsstörningar från Jorden. Interferometern ska bestå av flertaletpolyamidfilmer, ca 100 meter långa och en meter breda. Filmerna skasammankopplas i en kontrollenhet som finns i mitten av det stjärnformade mönsterfilmerna läggs i. Då rovern ska placera ut dessa filmer på månens yta, ska den skaköra från och till landaren för att hämta upp rullarna. Fokus i projektet har varit attgöra ett så pålitligt stabilt system som möjligt för att rovern ska klara av att slutförasitt uppdrag utan driftstörningar. Med interferometern vill man sedan kartläggavätgasmoln som bildades i universums ungdom (Platt, 2008).Resultatet av projektet är ett koncept som visar roverns framdrivnings- ochstyrsystem, hjulupphängning, motorplacering samt hur hjuldesignen kan se ut. FredyOlssons metoder har använts för att ta fram koncept som uppfyller krav och önskemåldå denna metod har använts tidigare under utbildningen.De fyra koncept som bidrar till ett koncept för hela styr- och framdrivningssystem ärstyrning och framdrivning på roverns alla sex hjul, hjulen är designade på så vis att deär delade i två. Motorn är vinkelmonterad. Roverns hjul är semi-öppna med en kantsom är högre än det djup hjulet sjunker ner i månytan., med en sluttning inuti för attsand och damm ska rinna ut.Inspiration har kommit från tidigare rovrar som varit/är aktiva på månen och Mars dådet är beprövade koncept som visat sig vara stabila och pålitliga. Tidigareexamensarbeten har kommit fram till att det chassi som ska användas är snarlikt detsom använts på Mars Science Laboratory Curiosity och Mars Exploration Rover’sSpirit och Opportunity.Projektet började på Högskolan i Halmstad 2013 och tidigare projekt har tittat påbland annat chassit, energisystem och utplaceringsenheten. Årets projekt har tagithänsyn till resultat från tidigare år, för att ett koncept på en hel rover slutligen skakunna visas upp för NASA Jet Propulsion Laboratory.Examensarbetet är genomfört i samarbete med NASA:s Jet Propulsion Laboratory iKalifornien, USA, vilka är USA:s center för robotisk utforskning av solsystemet.

A variety of precision observations suggest that the present universe is dominated by some unknown components, the so-called dark matter and dark energy. The distribution and properties of these components are the focus of modern cosmology and we are only beginning to understand them. Gravitational lensing, the bending of light in the gravitational field of a massive object, is one of the predictions of the general theory of relativity. It has become an ever more important tool for investigating the dark universe, especially with recent and coming advances in observational data. This thesis studies gravitational lensing effects on scales ranging over ten orders of magnitude to probe very different aspects of the dark universe. Implementing a matter distribution following the predictions of recent simulations, we show that microlensing by a large population of massive compact halo objects (MACHOs) is unlikely to be the source of the observed long-term variability in quasars. We study the feasibility of detecting the so far elusive galactic dark matter substructures, the so-called “missing satellites”, via millilensing in galaxies close to the line-of-sight to distant light sources. Finally, we utilise massive galaxy clusters, some of the largest structures known in the universe, as gravitational telescopes in order to detect distant supernovae, thereby gaining insight into the expansion history of the universe. We also show, how such observations can be used to put constraints on the dark matter component of these galaxy clusters. / At the time of the doctoral defense, the following paper was unpublished and had a status as follows: Paper 6: Submitted.