<p>Varför köper vi idag skandaler? Och varför är det främst den kända kvinnan som attribueras med skandal? Konkurrensen medier emellan ökar konstant enligt medieforskare. Givetvis väcker skandaler uppmärksamhet, vilket handlar om våra tankar och känslor, som dessutom handlar om medias närmanden oss. Detta kan även ha att göra med synen på den exponerade kvinnokroppen. Ena sidan väcker detta mannens sexuella lust och andra sidan väcker det negativ uppmärksamhet. Det blir skandal. Media ger budskap om hur kvinnan ska vara respektabel, och inte bete sig vulgärt. Det är genom artisterna budskapet ges.</p><p>I de undersökta tidskrifterna Hänt bild 2007 och Bildjournalen 1956-57 granskas ur ett genusperspektiv hur kända kvinnor framställs i förhållande till kropp, beteende, kärleksförhållande och karriär. På 1950-talet beskrivs artister främst som respektabla, 2007 har egenskaperna ersatts till vulgaritet. Kvinnokroppen exponeras mer och används med ord som sex, bröst och underliv. Hur kommer det sig? Kan man hitta kopplingar till 1950-talets skildringar av kända kvinnor, då vulgära egenskaper betraktas mindre vulgärt i förhållande till 2007. Vad är likheten och skillnaden i hur kända kvinnor konstrueras i de utvalda tidskrifterna?..</p>

Varför köper vi idag skandaler? Och varför är det främst den kända kvinnan som attribueras med skandal? Konkurrensen medier emellan ökar konstant enligt medieforskare. Givetvis väcker skandaler uppmärksamhet, vilket handlar om våra tankar och känslor, som dessutom handlar om medias närmanden oss. Detta kan även ha att göra med synen på den exponerade kvinnokroppen. Ena sidan väcker detta mannens sexuella lust och andra sidan väcker det negativ uppmärksamhet. Det blir skandal. Media ger budskap om hur kvinnan ska vara respektabel, och inte bete sig vulgärt. Det är genom artisterna budskapet ges. I de undersökta tidskrifterna Hänt bild 2007 och Bildjournalen 1956-57 granskas ur ett genusperspektiv hur kända kvinnor framställs i förhållande till kropp, beteende, kärleksförhållande och karriär. På 1950-talet beskrivs artister främst som respektabla, 2007 har egenskaperna ersatts till vulgaritet. Kvinnokroppen exponeras mer och används med ord som sex, bröst och underliv. Hur kommer det sig? Kan man hitta kopplingar till 1950-talets skildringar av kända kvinnor, då vulgära egenskaper betraktas mindre vulgärt i förhållande till 2007. Vad är likheten och skillnaden i hur kända kvinnor konstrueras i de utvalda tidskrifterna?..

This essay is about how lesbian love is being portrayed in two Swedish novels. The material consists of Karin Boye’s Crisis (1934) and Louise Boije af Gennäs’ Stars without Vertigo (1996). By using theories of heteronormativity, discourse analysis and a historical perspective, the essay aims to explain the similarities and differences in the way that lesbian love is being portrayed in these books. The results are organised through themes by using the methods close reading and comparative method.               The heteronormative discourse is ruled by norms and assumptions about normality in relation to sexuality and gender. The protagonists in both Crisis and Stars without Vertigo are in different ways being confronted with the heteronormative discourse in the Swedish society, Christianity and amongst their family and friends. In Crisis, the main character, Malin struggles to handle her non-heterosexual feelings in relation to her faith, and not to expose her emotions. In 1934 homosexuality was considered a crime in Sweden and at the same time homosexuality was looked upon as a disease, which controls how Malin looks upon her non-heterosexual feelings and keeps her from telling anyone about them. For Sophie, the main character in Stars without Vertigo the society’s values and norms are present, but the social climate for homosexuals is different in comparison to Crisis. The heteronormative discourse concerns her private life, her choice in a spouse/partner and her ability to start a family, since the homosexual community was being considered as something different from the universal heterosexuality and therefore should not have the same rights.               Although the novels where published more than 60 years apart there are some similarities in what kind of words Malin and Sophie are using about non-heterosexuality. Both women choose not to name their non-heterosexuality because any type of word or category is limiting. Thus both Malin and Sophie create their own identity through their sexuality.

Massive stars live fast and die young. They shine furiously for a few million years, during which time they synthesize most of the heavy elements in the universe in their cores. They end by blowing themselves up in a powerful explosion known as a supernova (SN). During this process, the core collapses to a neutron star or a black hole, while the outer layers are expelled with velocities of thousands of kilometers per second. The resulting fireworks often outshine the entire host galaxy for many weeks. The explosion energy is eventually radiated away, but powering of the newborn nebula continues by radioactive isotopes synthesized in the explosion. The ejecta are now quite transparent, and we can see the material produced in the deep interiors of the star. To interpret the observations, detailed spectral modeling is needed. This thesis aims to develop and apply state-of-the-art computational tools for interpreting and modeling SN observations in the nebular phase. This requires calculation of the physical conditions throughout the nebula, including non-thermal processes from the radioactivity, thermal and statistical equilibrium, as well as radiative transport. The inclusion of multiline radiative transfer, which we compute with a Monte Carlo technique, represents one of the major advancements presented in this thesis. On February 23 1987, the first SN observable by the naked eye since 1604 exploded, SN 1987A. Its proximity has allowed unprecedented observations, which in turn have lead to significant advancements in our understanding of SN explosions. As a first application of our model, we analyze the 44Tipowered phase (t &amp; 5 years) of SN 1987A. We find that a magnetic field is present in the nebula, trapping the positrons that provide the energy input, and resulting in strong iron lines in the spectrum. We determine the 44Ti mass to 1.5(+0.5−0.5)*10−4 M⊙. From the near-infrared spectrum at an age of 19 years, we identify strong emission lines from explosively synthesized metals such as silicon, calcium, and iron. We use integral-field spectroscopy to construct three-dimensional maps of the ejecta, showing a morphology suggesting an asymmetric explosion. The model is then applied to the close-by and well-observed Type IIP SN 2004et, analyzing its ultraviolet to mid-infrared evolution. Based on its Mg I] 4571 Å, Na I 5890, 5896 Å, [O I] 6300, 6364 Å, and [Ne II] 12.81 mm nebular emission lines, we determine its progenitor mass to be around 15 M⊙. We confirm that silicate dust, SiO, and CO have formed in the ejecta. Finally, the major optical emission lines in a sample of Type IIP SNe areanalyzed.We find that most spectral regions in Type IIP SNe are dominated by emission from the massive hydrogen envelope, which explains the relatively small variation seen in the sample. We also show that the similar line profiles seen from all elements suggest extensive mixing occurring in most hydrogenrich SNe. / At the time of the doctoral defense, the following papers were unpublished and had a status as follows: Paper 3: Manuscript. Paper 4: Accepted.

There exists many astronomical objects that vary in brightness. Objects such as variable stars like the Cepheids that periodically expands and contracts their outer layers, or the active galactic nuclei (AGN) where accretion of matter into a black hole generates a often varying brightness. Several candidates for being such variable objects have been identified as a result of the Vanishing and Appearing Stuff during a Century of Observations (VASCO) project. These candidates were then narrowed down to a handful that showed variability towards the infrared part of the spectrum. This bachelor’s thesis then aims to look further into these candidates using various databases and catalogues taking data from several sky surveys (SDSS, 2MASS etc). This is done to get better overview of the objects lightcurve over a bigger part of the spectrum, to establish whether the variability is real or a result from errors and to form a hypothesis of what kind of objects they could be. The result obtained from the data from the surveys points towards all the objects being real variable objects. The hypothesis is that all the objects are AGN’s that vary in brightness. / Det existerar många olika astronomiska objekt som varierar i ljusstyrka. Allt från variabla stjärnor som Cepheiderna som periodvis expanderar och kontraherar dess yttre skikt, till aktiva galaxkärnor där ackretion av materia in i ett svart hål genererar en ofta varierande ljusstyrka. Ett flertal kandidater för just sådana varierande objekt har identifierats som ett resultat av VASCO projektet. Dessa kandidater har sedan skalats ner till en handfull mängd kandidater som visade variation mot den infraröda delen av spektrumet. Detta kandidatarbete siktar på att vidare undersöka dessa kandidater genom att använda diverse astronomiska databaser och kataloger för att få data från flera kartläggningsprojekt (t.ex. SDSS, 2MASS etc). Detta är gjort för att få en bättre överblick över objektens ljuskurvor över en större del av spektrumet, att fastställa ifall objekten är riktiga variabla objekt eller uppstått på grund av diverse fel, samt att framställa en hypotes för vad det är för typ av objekt de kan vara. Resultaten från undersökningarna pekar på att alla objekten är riktiga variabla objekt. Hypotesen är att alla av objekten är aktiva galaxkärnor som varierar i ljusstyrka.

Aim. In this project, theoretical models of dust driven winds of asymptotic giant branch (AGB) stars with effective temperatures within a range of 2400 − 3200 [K] and relative carbon-to-oxygen abundance C/O &gt; 1 are studied. The aim is to understand if and how a detailed description of the grain size in winds of carbon rich AGB stars affects the wind formation and wind driving processes. Method. The computations were performed with a well tested FORTRAN code by calculating a grid of 60 models with different stellar parameters using grain size-dependent opacities. The results were then compared with models where the small particle approximation (SPA) had been used. Conclusions. The results indicate a certain dependency on grain size of the wind properties. The results from the computations of the majority of the models show no significant diferences however, especially not for the mass loss rates. Thus earlier computations performed using the SPA need not necessarily to be rejected.

This paper studies how peer assessment is used as a strategy to improve young learners' results in Swedish as a school subject. Nine teachers are interviewed about their use of the method on 7-12-year-old pupils. Comparisons are made between the interviews and Swedish and international discussion on peer assessment. There are similarities between the practice of the teachers and what is said in the litterature about the method and its advantages and drawbacks. The teachers tend to emphasize the social aspects more, though. They also point to adjustments necessary to make the method function in groups of different kinds. Of feedback methods, they seem to prefer "Two stars and a wish" to others.

The spectroscopic determination of stellar properties is important for subsequent studies of exoplanet atmospheres. In this thesis, HARPS data for 6 exoplanet-hosting, late-type stars is processed to achieve an average signal-to-noise ratio of ~105. Together with line data, the SME tool is used to synthesize spectra and interpolate model photospheres with which chi-square minimization is performed. Fundamental parameters are derived to an overall precision of 191 K in effective temperature, 0.88 dex in surface gravity and 0.21 dex in metallicity. For 5 of the stars, the parameters are thereafter used to compute specific intensities across the stellar discs. Primary improvements could be made in regards to the stellar models, i.a. through the update of atomic properties and inclusion of magnetic fields. The numerical derivation can also be handled more carefully by excluding parameter-insensitive spectral regions. / Den spektroskopiska bestämningen av stjärnegenskaper är viktig för efterföljande studier av exoplaneters atmosfärer. I denna avhandling bearbetas HARPS-data från 6 stjärnor av sen typ som hyser exoplaneter för att uppnå en genomsnittlig signal-till-bruskvot på ~105. Tillsammans med linjedata, används SME-programvaran för att syntetisera spektra och interpolera modellfotosfärer med vilka chi-kvadratminimering genomförs. Fundamentala parametrar härleds till en medelprecision på 191 K i effektiv temperatur, 0.88 dex i ytgravitation och 0.21 dex i metallicitet. För 5 av stjärnorna används parametrarna till att därefter beräkna specifika intensiteter över stjärnornas projicerade ytor. Huvudsakliga förbättringar kan göras med avseende på stjärnmodellerna, bl.a. genom uppdatering av atomära egenskaper och inkludering av magnetiska fält. Den numeriska härledningen kan också hanteras med högre noggrannhet genom att avsiktligt exkludera parameterokänsliga spektralregioner.