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