DOC PREVIEW
TAMU ASTR 101 - Light: The Cosmic Messenger
Type Lecture Note
Pages 2

This preview shows page 1 out of 2 pages.

Save
View full document
View full document
Premium Document
Do you want full access? Go Premium and unlock all 2 pages.
Access to all documents
Download any document
Ad free experience
Premium Document
Do you want full access? Go Premium and unlock all 2 pages.
Access to all documents
Download any document
Ad free experience

Unformatted text preview:

ASTR 101 Lecture 8 Outline of Last Lecture I. Gravitational Potential EnergyII. Conservation of EnergyIII. The Force of GravityOutline of Current Lecture I. Light: The Cosmic MessengerII. Learning from Lighta. Chemical Fingerprintsb. Thermal RadiationCurrent LectureChapter 5Light: The Cosmic MessengerWavelength and Frequency- Wavelength x Frequency = speed of light = constant- l x f = c- l = wavelength, f = frequency, c = 3.00 x 108m/s = speed of light5.2 Learning from LightWhat are the three basic types of spectra?- Emission line spectrum- Continuous spectrum- Absorption line spectrum- spectra of astrophysical objects are usually combinations of these three basic typesHow does light tell us what things are made of?Chemical Fingerprints- Each type of atom has a unique set of energy levels- Each transition corresponds to a unique photon energy, frequency, and wavelength- Because those atoms can absorb photons with those same energies, upward transitions produce a pattern of absorption lines at the same wavelengths- Each type of atom has a unique spectral fingerprint- Observing the fingerprints in a spectrum tells us which kinds of atoms are presentThermal Radiation- Nearly all large or dense objects emit thermal radiation, including stars, planets, and you- An object's thermal radiation spectrum depends on only one property: its temperatureProperties of Thermal Radiation1. Hotter objects emit more light at all frequencies per unit area2. Hotter objects emit photons with a higher average energy17814524077Interpreting an actual spectrum- By carefully studying the features in a spectrum, we can learn a great deal about the object that created it.- Between blue and green on the spectrum: reflected sunlight. Continuous spectrum of visible light is like the Sun's except that some of the blue light has been absorbed - the object must look red- Thermal radiation: infrared spectrum peaks a wavelength corresponding to a temperature of 225K.- Carbon dioxide: absorption lines are the fingerprints of CO2 in the atmosphereMeasuring the Doppler Effect shif- Doppler shif tells us ONLY about the part of an object's motion toward or away from


View Full Document

TAMU ASTR 101 - Light: The Cosmic Messenger

Type: Lecture Note
Pages: 2
Documents in this Course
Lecture14

Lecture14

56 pages

Lecture17

Lecture17

35 pages

lecture3

lecture3

65 pages

Lecture02

Lecture02

40 pages

Lecture16

Lecture16

35 pages

Lecture27

Lecture27

69 pages

Lecture03

Lecture03

26 pages

astronomy

astronomy

90 pages

Lecture23

Lecture23

47 pages

Lecture15

Lecture15

45 pages

Lecture24

Lecture24

64 pages

Lecture25

Lecture25

22 pages

Lecture22

Lecture22

48 pages

Lecture02

Lecture02

25 pages

Lecture03

Lecture03

32 pages

Lecture05

Lecture05

28 pages

Lecture19

Lecture19

72 pages

Load more
Download Light: The Cosmic Messenger
Our administrator received your request to download this document. We will send you the file to your email shortly.
Loading Unlocking...
Login

Join to view Light: The Cosmic Messenger and access 3M+ class-specific study document.

or
We will never post anything without your permission.
Don't have an account?
Sign Up

Join to view Light: The Cosmic Messenger 2 2 and access 3M+ class-specific study document.

or

By creating an account you agree to our Privacy Policy and Terms Of Use

Already a member?