Outline:

1 Introduction

1.1 What we mean by nebular phase
1.2 Possible science
1.3 Overview of physical situation

2 Line profiles

2.1 Basic mapping relations from homologous ejecta
2.2 Example line profiles (uniform sphere, Gaussian distribution, shell, ..)
2.3 Clumping and the Chugai model
2.4 Radiative transfer effects

3 Powering

3.1 Radioactive isotopes and their decay chains
3.2 Transport of decay products
3.3 Non-thermal processes
3.4 Time-dependence
3.5 Other power sources

4 Line formation regimes and analytic methods

4.1 LTE, optically thin
4.2 LTE, optically thin
4.3 NLTE
  4.3.1 Recombination lines
  4.3.2 Cooling lines
4.4 Atomic data and equations/tables for key lines and line ratios

5 Spectral synthesis modelling

5.1 Physical processes 
5.2 NLTE level population equations
5.3 Temperature
5.4 Radiative transfer
5.5 Explosion models, and treatment of mixing
5.6 Survey of published models and their possible application

6 Modelling examples and applications

6.1 Type II SNe
6.2 Type Ib/IIb/Ic SNe
6.3 Type Ia SNe

7 Outlook

public/handbook_of_sn/jerkstrand-plan.txt · Last modified: 2015/11/10 13:34 by Anders Jerkstrand

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