Intel 304

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Why is Light so useful in Astronomy?

• It can tell us many properties of planets and stars: – How warm / hot they are (Surface temperature) – What they’re made of (Chemical Composition) – How they’re moving (Radial Velocity and

Spin) Spectrum of Mars

Interaction of Light and Matter: Four Ways

1. emission – matter releases energy (E) as light 2. absorption – matter takes E from light 3. transmission – matter allows light to pass 4. reflection – matter repels light in another

direction

CONSERVATION OF ENERGY

Emission - Continuous

• Hot, dense objects give off continuous thermal blackbody radiation – Warm objects emit infrared – Hotter

• More light • Shorter wavelengths • e.g. Stars emit visible light!

• IR Spectrum We can measure planet’s surface temperature!

Reflection: Application • When light passes through matter, or reflects off

of matter, some wavelengths may be absorbed

• Resulting spectrum tells us about the matter! – Example: Mars appears red because it’s surface absorbs

more blue light than red (reflects more red light than blue) tells us something about what surface is made of

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Blackbody Activity

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Application to Stars: Thermal Radiation

• Bluer Stars are hotter than redder ones!

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Emission & Absorption • Photons can be absorbed / emitted

by matter: – Photon energy matches “jump” in

energy levels • http://www.astro.uiuc.edu/projects/data/S

pectra/orbitals.html

• Atoms absorb photon & gain energy Absorption-line spectrum

• Atoms emit photon & lose energy Emission-line spectrum

Kirchhoff’s Laws: Kinds of Spectra

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Types of Spectra Activity

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Element Identification

• Fig. 6.8

• Each element has a unique signature because of its energy level structure

Hydrogen

• Only photons whose energies (colors) match the “jump” in electron energy levels can be emitted or absorbed.

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Application : Chemical Composition

• Presence of absorption lines of a particular element indicates the presence of that element in the absorbing material – e.g. atmosphere of a star!

Artificial (Absorption-line) Solar Spectrum:

Laboratory (Emission-line) Spectrum of Iron:

• Outer layers of a star are cooler than the dense inner part (i.e. they are the “cool cloud”)

Application to Stars: Absorption spectra

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• Tails of Comets consist of dust which reflects sunlight, and excited gas which produces an emission-line spectrum.

Application: Emission Spectra

From http://www.astron.pref.gunma.jp/gallery/comet_2001Q4.html

Application : Chemical Composition • Presence of emission

lines of a particular element indicates the presence of that element in the excited gas

From: http://www.pbs.org/wgbh/nova/origins/spectra.html

The Doppler Effect How is light affected by the velocity of a source?

(Alternate views: http://www.fearofphysics.com/Sound/dopwhy2.html

and http://lectureonline.cl.msu.edu/~mmp/applist/doppler/d.htm)

Motion toward observer shortens wavelength (Blue Shift)

Motion away from observer lengthens it (Red Shift)

Faster speed bigger change in λ

The Doppler Effect

Measuring Radial Velocity • Measure Doppler shift of emission or absorption

lines in a spectrum radial velocity of object

• No Motion

• Motion away

• Motion towards

From: http://www.psi.edu/esp/method.html 18

Doppler Effect Activity

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Measuring Radial Velocity

From: http://woodahl.physics.iupui.edu/05-22_anno.jpg

Application: Orbiting Stars • Motions of stars

moving towards & away from us – Binary Stars – Extrasolar planets

• Mizar: – Really 4 stars!

(http://ircamera.as.arizona.edu/NatSci102/NatSci102/lectures/spectroscopy.htm)

More Applications • Spin of Venus

and/or asteroids: – Radar measurements

• Expansion of Universe: – Distant galaxies

moving away from us

Why is Light so Useful?

• Thermal / continuous spectrum temperature • Reflected light properties of reflecting

object • Absorption features composition of

absorbing material (e.g. star, planet atmosphere)

• Emission lines composition of thin gas (e.g. nebula, tail of comet)

• Doppler effect on lines radial velocity, spin!