Physical emission mechanisms responsible for gamma-ray bursts (GRBs) remain elusive to this day, 50 years after their discovery. Although there are well studied physical models, their power to explain the observed data is a matter of debate. In this thesis, the main focus is the statistical studies of the dierent physical models given the available data from the Fermi Gamma-Ray Space Observatory to make better comparisons between these models as well as ascertaining how well they can explain the available observations so far. To this end, theoretically predicted thermal and non-thermal GRB spectra are investigated. This investigation entails both ending groupings in the catalog data (clustering) and then simulating the expected physical emission processes to test how they would look like in the current data acquiry, processing and tting procedures. Finally, a Bayesian model comparison is performed in a sub-sample of these bursts to quantify the preference of different models by the data. In conclusion, it is found that around one third of all bursts include intervals where the emission is from a photosphere which is non-dissipative.

This means that during these intervals, the emission is either emitted close to the saturation radius or in a flow which is laminar. The results further indicate that dissipation below the photosphere is responsible for the spectral shape in a majority of GRB spectra. It is consequently argued that the dominant emission mechanism during the prompt emission phase in GRBs is thermal emission from the jet photosphere at distance of around 1012 cm from the central engine. A small percentage of the bursts are better explained with a non-thermal generating process such as the synchrotron emission.

Stralningsprocessen som ligger till grund for gamma-blixtarnas initiala hogenergetiskautbrott av gamma-stralning ar fortfarande okand trots att de har observeratsi over 50ar. Aven om det nns valformulerade fysikaliska modeller sa debatterasdet huruvida de olika modellerna kan forklara observationerna. Huvudinriktningen iforeliggande avhandling ar statistiska studier av olika fysikaliska stralningsmodellersom testas mot data fran Fermi Gamma-Ray Space Observatory. Syftet ar attuppna forbattrade jamforelser mellan modellanpassningarna och att utrona hur valmodellerna kan beskriva de tillgangliga observationerna. De modeller som studerasar teoretiska beskrivningar av en termisk och en icke-termisk stralningsprocess. Destatistiska studierna innefattar saval klassicering genom klusteranalys av datakatalogersom dataanalys av simulerad data som ar baserade pa de fysikalisk modellerna.Slutligen gors aven en Bayesiansk modelljamforelseanalys av en delmangd av allaobserverade gammablixtar. Syftet ar att undersoka vilken av modellerna som foredrasav datan. Slutsatsen jag drar av mina undersokningar ar att ungefar en tredjedelav gammablixtarna har perioder da den observerade stralningen kommer franfotosfaren i ett utode dar ingen energidissipering sker. Detta innebar att underdessa perioder kommer stralningen antingen fran omraden nara satureringsradieneller fran ett laminart utode. Mina resultat visar vidare att fotonspektrumen franen en majoritet av blixtarna formas av just energidissipering under fotosfaren. Jagargumenterar darfor for att den dominerande stralningsprocessen under den initiala(eng. prompt) fasen hos gammablixtarna ar termisk stralning fran fotosfareni det relativistiska utodet. Enbart en liten del kan ges en battre forklaring med enicke-termisk model som t.ex. synkrotronstralning.v