Next:
Contents
Radiative Transfer Modelling of Star Formation Regions
Robin R. Phillips
Abstract
Acknowledgements
Contents
Star Formation
The Birth, Life and Death of Stars
The Stages of Star Formation
From Molecular Cloud to Clump
From Clump to Protostar
From Protostar to the Main Sequence
Classification of Protostellar Objects
Summary of Thesis Contents
Observing Star Formation Regions
The Theory Of Spectral Line Generation From Molecules
Einstein Coefficients
Temperature Definitions
Radio Telescopes and their use
The James Clerk Maxwell Telescope
Methods for Reducing Telescope Data
Correcting the Temperature Scale
Rotation Diagrams
Radiative Transfer Modelling
The radiative transfer equation
The Source Function
The LVG Approximation
The Monte Carlo Method
The Feautrier Method
The STENHOLM Method
Solving the Radiative Transfer Equation Along a Line of Sight
A Generalised 2-D Radiative Transfer Program
Introduction
Generalising the STENHOLM program to run for Non-linear Molecules
New features
Source of the Einstein Coefficients
Setting up the model cloud
Re-labelling the Data Arrays
Using the Modified STEN Program
Initial setup
Starting the program
Option 1
Option 2
Option 3
Option 4
Output options
Input files
datakey.sten (13)
.stendefaults (10)
Data.list (17)
run.*** (18)
Other files
An Example Using the Modified STEN Program
The
geometry
routine for the ASTRA Program
Introduction
The model shape
Calculating the lines of sight
Calculating the ring relative velocities
The
givevel
subroutine
Relative velocity between two points on a line of sight
The
midfind
subroutine
Setting up the model cloud
Ring parameter calculations
The Lambda Iteration
The Emissivity Function
Solving the Radiative Transfer Equation
Statistical Equilibrium
Calculating the level populations
Solving the Matrix Equation
Convergence Check
Calculating the Line Profiles
Define the line of sight from the telescope through the cloud
The
geometry2
subroutine
Gridded convolution
Calculating the Optimum Velocity Window
Calculating the final output
Outputting the Results
A Modification to Allow Modelling of Dust
The Tcl/Tk interface
Using the Tcl/Tk Interface
Input/Output Files for the ASTRA Program
.stendefaults (n/a)
datakey.sten (n/a)
MODELDATA.DAT (1)
SHELL.DAT (8)
run.** (19)
COEFDATA.*** (2)
FREQ.*** (3)
G.*** (4)
OBJECTDATA.*** (14)
TELEDATA.*** (15)
MOLECDATA.*** (16)
stendump.txt (7)
datastore.tmp (18)
data.***
runshells.***
rundata.***
run##.***
lastcloud.***
makemodel.***
comments.txt
mcs Files
Documentation for the Helper Programs
Testing the ASTRA program
Testing the geometry section
A Subjective Test Using the Dust Model
Testing by Comparison with the Spherically Symmetric Case
The optically thick LTE case
The LVG case
A Detailed Comparison with a 1-D Model
Solid Body Rotation
Testing for non-Spherically Symmetric Cases
Keplerian Rotation
Test Summary
Simulated Observations of Rotating Clouds
Solid Body Rotation vs Keplerian Rotation
Dependency of Line Shape on Viewing Angle
The Observability of Rotation Features
Observing Using the JCMT
The Potential Usefulness of Proposed Large Telescopes
Effects of the Viewing Angle of the Disk
Limitations of the 'standard test model'
Modelling L1544
Required number of disks/cylinders
A prolate model
An oblate model
Modelling Summary
Bibliography
Index
About this document ...
Next:
Contents
1999-04-12
