Astro 1050 Mon. Oct. 14, 2002
Homework #5
What fundamental property
of a star
varies along the main sequence?
Masses of Binary stars
Masses of Binary stars
Masses of Binary stars
Measuring a and P of
binaries
Masses and the HR Diagram
The Mass-Luminosity
Relationship
Eclipsing Binary Stars
Starting Ch.9:
Interstellar Medium
Emission nebulae
Reflection nebulae – The
Pleiades
Dark Nebula
Spectral Measurements
Measurements at other
Wavelengths
Collapse of
Molecular Clouds
What will a forming star
look like in HR diagram?
How does mass affect
collapse?
Observations of collapse
More details of stellar
structure and energy generation
The CNO Cycle
Heavy Element Fusion
Models of Stellar
Structure
Numerical Stellar Models
Why don’t stars collapse?
Why do we get steady
fusion rates?
Mass-Luminosity
relationship
Lifetime on Main Sequence
How about a 0.5 solar
mass star?
How about a 0.5 solar
mass star?
Width of Main Sequence –
and Stellar Aging
Orion Nebula: A
Star-Forming Region
Protoplanetary Disks in
the Orion Nebula
Herbig-Haro objects: The
angular momentum problem
Herbig-Haro 34 in Orion
Motion of Herbig-Haro 34
in Orion