Review3

Review3 - Review 3 Chapter 16: How do we use the atomic...

Info iconThis preview shows pages 1–2. Sign up to view the full content.

View Full Document Right Arrow Icon
Review 3 Chapter 16: How do we use the atomic emission and absorption spectra to find the composition of a star? How do we determine the rotation period of a star? How do we determine the distance to a star using Stellar Parallax? What is an H-R diagram and what information does it give us? A star when observed through a powerful telescope has a Stellar Parallax of 0.5 arcsecs. What is the distance to the star? One of the Ca spectral lines coming form a distant star is red-shifted by 10 nm. This line of Ca when emitted from a stationary source in our Lab is at 500 nm. Is the star moving away of towards us and what is its speed? Chapter 17: Internal structure of our Sun and its chemical composition. What is the convection zone on the Sun and what are the granules and supergranules? What is the temperature in the Sun’s core? What is the photosphere, chromosphere and corona? What is their temperature and what causes their color? What is the cause of sun-spots why are they dark and why do they occur mostly in pairs and in a band around the sun’s equator? What is the so-called differential rotation of the sun? What is the main cause of the sun’s
Background image of page 1

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Image of page 2
This is the end of the preview. Sign up to access the rest of the document.

Page1 / 2

Review3 - Review 3 Chapter 16: How do we use the atomic...

This preview shows document pages 1 - 2. Sign up to view the full document.

View Full Document Right Arrow Icon
Ask a homework question - tutors are online