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Abstract
In this thesis, the field star Initial Mass Function (IMF) and chemical evolution parameters for the Milky Way (MW) are derived using a forward modelling technique in combination with Bayesian statistics. Starting from a local MM disc model, observations of stellar samples in the Solar Neighbourhood are synthesised and compared to the corresponding volume-complete observational samples of Hipparcos stars. The resulting IMF, derived from observations in the range from 0.5 to 8Msun, is a two-slope broken power law with powers of -1.49 +- 0.08 and -3.02 +- 0.06 for the low-mass slope and the high-mass slope, respectively, with a break at 1.39 +- 0.05Msun. In order to constrain the IMF for stars more massive than 8Msun, a fast and flexible chemical enrichment code, Chempy, was developed, which is also able to reproduce spatial and stellar population selections of observational samples. The inferred high-mass slope for stellar masses above 6Msun is -2.28 +- 0.09, accounting for the systematic effects of different yield sets from the literature. This shows that constraints from chemical modelling, similarly to hydrodynamical simulations of the Galaxy, demand a Salpeter high-mass index. This is hard to recover from star count analysis given the rareness of high-mass stars.
Dokumententyp: | Dissertation |
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Erstgutachter: | Just, Prof. Dr. Andreas |
Ort der Veröffentlichung: | Heidelberg |
Tag der Prüfung: | 8 Dezember 2015 |
Erstellungsdatum: | 17 Dez. 2015 13:45 |
Erscheinungsjahr: | 2015 |
Institute/Einrichtungen: | Zentrale und Sonstige Einrichtungen > Zentrum für Astronomie der Universität Heidelberg (ZAH) > ZAH: Astronomisches Rechen-Institut |
DDC-Sachgruppe: | 520 Astronomie |
Normierte Schlagwörter: | Milky Way, Chemical evolution modelling, Bayesian statistics |