Lecture 5 - Ch4

Lecture 5 - Ch4 - 1/18/10 Chapter 4 - Spectroscopy Physics...

Info iconThis preview shows pages 1–3. Sign up to view the full content.

View Full Document Right Arrow Icon
1/18/10 1 Physics 1902 Lecture W.3.a Tools of Astronomy : spectra Chapter 4 - Spectroscopy Why do we want to measure optical spectra How do we measure optical spectra Why measure spectra Spectrum of hot bodies reveals their temperature Shifts in spectral features can reveal motion through Doppler shift Each element has a unique set of spectral lines which allow us to determine the chemical makeup of the sources Detailed studies of atomic transitions can reveal features of the environment such as temperature, pressure, magnetic field Prism with hot lamp Prism Spectrometer Prism with hydrogen source
Background image of page 1

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

View Full DocumentRight Arrow Icon
1/18/10 2 Why do elements have different spectral lines Bohr rules Electrons have certain allowed energy states When an electron moves from one state to another, a photon of energy E = h G is produced where E is the energy-difference between the initial and final electron states Start with hydrogen: simplest atom and the most abundant element in the universe
Background image of page 2
Image of page 3
This is the end of the preview. Sign up to access the rest of the document.

Page1 / 7

Lecture 5 - Ch4 - 1/18/10 Chapter 4 - Spectroscopy Physics...

This preview shows document pages 1 - 3. Sign up to view the full document.

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