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Table of contents
1 Introduction
1.1 Historical background
1.2 Stellar evolution theory
1.2.1 The spectral types of stars and Hertzsprung–Russell diagram
1.2.2 CNO cycle
1.2.3 The triple-alpha process
1.2.4 Carbon, neon and oxygen burning
1.2.5 Si burning
1.2.6 Photodisintegration and core collapse
1.3 Supernovae
1.3.1 SN classification
1.3.2 Thermonuclear Type Ia SNe
1.3.3 Core-collapse SNe
1.3.3.1 Mass loss
1.3.3.2 Red supergiants
1.3.3.3 Type II-P/L SNe
1.3.3.4 Type IIb SNe
1.3.3.5 Type Ibc SNe
1.3.4 Other rare SNe types and proposed models
1.3.4.1 SNe Type Ibn
1.3.4.2 SNe Type IIc
1.3.4.3 Peculiar Type II SNe
1.3.4.4 SN impostors
1.3.4.5 Super-luminous SNe
1.3.4.6 Pair-instability SNe
1.3.4.7 GRB-associated Type Ic-BL SNe
1.4 The need to better understand the diversity of CCSNe
2 Supernova modelling
2.1 1-D stellar evolution with MESA
2.1.1 13–25M model grid
2.2 Massive star explosions
2.2.1 Introduction
2.2.2 Numerical simulations with V1D
2.2.2.1 Explosive nucleosynthesis
2.2.2.2 Fallback
2.2.2.3 Mixing
2.3 SN radiation modelling: approaches and codes
2.3.1 STELLA
2.3.2 SEDONA
2.3.3 ARTIS
2.3.4 PHOENIX
2.3.5 CMFGEN
2.4 Radioactive decay power from unstable istopes
3 Observational properties
3.1 Type II-P SNe
3.1.1 Light curves
3.1.2 Color evolution
3.1.3 MV at plateau – MV at nebular phase relation
3.1.4 MV at plateau – expansion rate relation
3.1.5 Spectral evolution
3.2 Type II-L
3.3 Stripped-envelope SNe
4 SN 2008bk — a low-luminosity Type II-P supernova
4.1 Introduction
4.2 Observational data
4.3 Numerical setup
4.3.1 Pre-SN evolution
4.3.2 Piston-driven explosions
4.3.3 Radiative-transfer modelling
4.4 Properties of our best-match model to the observations of SN 2008bk
4.4.1 Ejecta temperature and ionization
4.4.2 Photometric properties
4.4.3 Spectroscopic properties
4.4.4 Ba II lines and the structure seen in H
4.4.5 Additional remarks
4.5 Sensitivity to progenitor and explosion properties
4.5.1 Radius
4.5.2 Mass
4.5.3 Mixing
4.6 Conclusions
4.7 Line identifications for model X at early and late times in the photospheric phase
5 Low-luminosity Type II-P SNe
5.1 Modelling
5.1.1 Pre-SN evolution with MESA
5.1.2 Piston-driven explosion with V1D
5.1.3 Radiative-transfer modelling with CMFGEN
5.2 Bolometric and multi-band light curves
5.2.1 Results from simulations
5.2.2 Comparison to observations
5.3 Spectra
5.3.1 Results from simulations
5.3.2 Comparison to observations and spectral line identifications
5.4 Comparison to other work
5.5 Conclusions
6 Kinetic energy variation
6.1 Model YE1 and comparison to SN 2005cs
6.2 Model YE2 and comparison to SN 2012ec
6.3 Model YE3 and comparison to SN 1999em
6.4 Conclusions
Conclusions
Acknowledgements
Appendix A Observational data
A.1 A sample of low-luminosity Type II SNe
A.1.1 SN 1994N
A.1.2 SN 1997D
A.1.3 SN 1999br
A.1.4 SN 1999eu
A.1.5 SNe 1999gn, 2006ov and 2008in
A.1.6 SN 2001dc
A.1.7 SN 2002gd
A.1.8 SN 2003Z
A.1.9 SN 2004eg
A.1.10 SN 2005cs
A.1.11 SN 2008bk
A.1.12 SN 2009N
A.1.13 SN 2009md
A.1.14 SN 2010id
A.1.15 SN 2013am
A.1.16 Other candidates in low-luminosity SNe II-P
A.1.16.1 SN 1991G
A.1.16.2 SN 2003ie
A.1.16.3 SN 2014bi
A.1.17 Archetypical Type II-P SN 1999em
A.2 A sample of core-collapse SNe
Appendix B Contributions of indiviudal ions to model spectra
B.1 Models m12, m25 and m27
Bibliography
