Astronomy Picture of the Day. Possible First Pic of Extrasolar Planet

Slides:



Advertisements
Similar presentations
…the study of how light and matter interact
Advertisements

Astronomy Notes to Accompany the Text Astronomy Today, Chaisson, McMillan Jim Mims.
Universe Eighth Edition Universe Roger A. Freedman William J. Kaufmann III CHAPTER 5 The Nature of Light CHAPTER 5 The Nature of Light.
Chapter 4 The Origin and Nature of Light
Astronomy Picture of the Day
Electromagnetic Radiation
Spectroscopy. Spectroscopy is complex - but it can be very useful in helping understand how an object like a Star or active galaxy is producing light,
Spectral lines Photon energy Atomic structure Spectral lines Elements in stars Masses of stars Mass-luminosity relation Reading: sections 16.5, 16.7, 6.2.
PHYS 206 Matter and Light At least 95% of the celestial information we receive is in the form of light. Therefore we need to know what light is and where.
Charles Hakes Fort Lewis College1. Charles Hakes Fort Lewis College2 Chapter 2,9 Stefan’s Law/ Spectroscopy.
Unit 4 Atomic Physics and Spectra. The Electromagnetic Spectrum.
Week 8 Day 1 Announcements
Astronomy Picture of the Day. Why Can We See Each Other? Light emitted from other sources is reflected off of us. We don’t radiate in the visible part.
Test #1, Wednesday, Feb 10 I will post a review for Test 1 in the A101 homepage under the link to “Lectures” this week. I will tell you the topics to review.
Week 6 Day 3 Announcements
The Nature of Light In Astronomy. Herschel’s Infrared experiment Invisible (to our eyes) light immediately beyond the color red is call infrared light.
Astronomy Picture of the Day. Why Can We See Each Other? Light emitted from other sources is reflected off of us. We don’t radiate in the visible part.
© 2004 Pearson Education Inc., publishing as Addison-Wesley Orbital Energy and Escape Velocity orbital energy = kinetic energy + gravitational potential.
Aim: How to distinguish electrons in the excited state DO NOW: PREPARE FOR QUIZ. 10 MIN.
Spectroscopy and Atomic Structure.
Chapter 4 Spectroscopy Chapter 4 opener. Spectroscopy is a powerful observational technique enabling scientists to infer the nature of matter by the way.
Electromagnetic Radiation
Chapter 3 Light and Matter
Blackbody Radiation & Atomic Spectra. “Light” – From gamma-rays to radio waves The vast majority of information we have about astronomical objects comes.
Chapter 4 Spectroscopy.
Properties of Matter Our goals for learning: What is the structure of matter? What are the phases of matter How is energy stored in atoms?
Stars and Galaxies 28.1 A Closer Look at Light Chapter 28.
Guiding Questions 1. How fast does light travel? How can this speed be measured? 2. Why do we think light is a wave? What kind of wave is it? 3. How is.
Spectroscopy “Spectroscopy” : Webster’s definition “Spectro” Radiant energy consisting of component waves which can be dispersed and focused into individual.
Lecture II Light spectra. The Birth of the Quantum Max Planck –The energy contained in radiation is related to the frequency of the radiation by the relationship.
What Can Spectroscopy Tell Us?. Atom or Molecular Fingerprints Every atom or molecule exists in its own unique energy state. This energy state is dependent.
Charles Hakes Fort Lewis College1. Charles Hakes Fort Lewis College2 Chapter 2 Stefan’s Law.
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.
Astronomy Picture of the Day. Review: Kepler's Laws 1. Planets travel aound the sun in elliptical orbits with the sun at one focus of the ellipse. 2.
© 2004 Pearson Education Inc., publishing as Addison-Wesley 6. Light: The Cosmic Messenger.
1 Nature of Light Wave Properties Light is a self- propagating electro- magnetic wave –A time-varying electric field makes a magnetic field –A time-varying.
Atomic Spectra & Doppler Shift. Demos for Optics from last time Optical Board –Lens & mirror –Kepler & Galileo Telescope (inverts/does not) –Eye: normal,
© 2007 Pearson Prentice Hall This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching their.
© 2008 Pearson Education, Inc., publishing as Pearson Addison-Wesley This work is protected by U.S. copyright laws and is provided solely for the use of.
Electromagnetic Radiation (How we get information about the cosmos) Examples of electromagnetic radiation? Light Infrared Ultraviolet Microwaves AM radio.
Aim: How to distinguish electrons in the excited state
What is light? Light can act either like a wave or like a particle Particles of light are called photons.
Spectroscopy and Atomic Structure Ch 04.
Copyright © 2010 Pearson Education, Inc. Lecture Outline Chapter 2 Light and Matter.
Lecture 10: Light & Distance & Matter Astronomy 1143 – Spring 2014.
Chapter 2: Light and Matter Electromagnetic Radiation
Light and Matter Astronomy 315 Professor Lee Carkner Lecture 6.
A Brief Review of “Matter”. Atom nucleus electron e-e- (proton,neutrons) p+p+ n ● 10,000,000 atoms can fit across a period in your textbook. ● The nucleus.
Chapter 4 Spectroscopy The beautiful visible spectrum of the star Procyon is shown here from red to blue, interrupted by hundreds of dark lines caused.
Chapter 4.
Spectroscopy and Atoms
Universe Tenth Edition Chapter 5 The Nature of Light Roger Freedman Robert Geller William Kaufmann III.
Electromagnetic Radiation, Atomic Structure & Spectra.
Starlight What is it? What does it tell us? Write down all notes in RED.
NATS From the Cosmos to Earth Light as a Wave For a wave, its speed: s = l x f But the speed of light is a constant, c. For light: l x f = c The.
Cool, invisible galactic gas (60 K, f peak in low radio frequencies) Dim, young star (600K, f peak in infrared) The Sun’s surface (6000K, f peak in visible)
© 2017 Pearson Education, Inc.
Studying the Sun Notes H- Study of Light Chapter 24
Atoms and Spectra.
Spectroscopy Lecture.
Spectroscopy and Atoms
YOYO: What element is this? How do you know?
Chapter 4.
5.4 Learning from Light Our goals for learning
Continuous, Emission, and Absorption
Light and Matter Chapter 2.
Chapter 3 Review Worksheet
Continuous, Emission, and Absorption
5.4 Learning from Light Our goals for learning
Matter and Particles of Light: Quantum Theory
Presentation transcript:

Astronomy Picture of the Day

Possible First Pic of Extrasolar Planet

Question The color of visible light is determined by its ____. A)brightness B) amplitude C)speed D)wavelength

Question If the wavelength of light increases, while the speed remains constant, the frequency must ____. A)increase also B) decrease C)remain unchanged

Question If the wavelength of light increases, while the speed remains constant, the frequency must ____. A)increase also B) decrease C)remain unchanged c =  f 

Question The bending of light that occurs when moving between media of different densities is called ___. A)reflection B) refraction C)diffraction D)distortion

Question The bending of light that occurs when moving between media of different densities is called ___. A)reflection B) refraction C)diffraction D)distortion “The change of direction of light as it passes from one medium to another is associated with a change in velocity and wavelength. The energy of the light is unchanged as it passes from one media to another. When visible light in air enters a medium such as glass, the velocity of light decreases to 75% of its velocity in air and in other materials the decrease can be even more substantial.”

ff c = 1 nm = m, 1 Angstrom = m The Electromagnetic Spectrum

Spectroscopy and Atoms How do you make a spectrum?

When you bend light, bending angle depends on wavelength, or color. Refraction of light (Prism demo)‏

What does the spectrum of an astronomical object's radiation look like? Many objects (e.g. stars) have roughly a "Black-body" spectrum: Brightness Frequency also known as the Planck spectrum or Planck curve.

Questions How is temperature related to the amount of energy radiated? How is temperature related to the color of the object? (Blackbody Demo)‏

"cold" dust "hot" stars "cool" star Sun frequency increases, wavelength decreases The wavelength of peak emission tells us the temperature of the object!

Types of Spectra 1. "Continuous" spectrum - a luminous solid or liquid, or a sufficiently dense gas, emits light of all wavelengths and produces a continuous spectrum 2. "Emission" spectrum - a low-density, hot gas emits light whose spectrum consists of a series of bright emission lines that are characteristic of the composition of the gas. 1."Absorption” Spectrum - a cool, thin gas absorbs certain wavelengths from a continuous spectrum, leaving dark absorption lines in their place, superimposed on the continuous spectrum.

Pattern of lines is a fingerprint of the element

For a given element, emission and absorption lines occur at the same wavelengths. Helium discovered in Sun’s spectrum before being found on Earth! Sodium emission and absorption spectra

The Particle Nature of Light Light interacts with matter as individual packets of energy, called photons. c photon energy is proportional to frequency: E  f (or E  1 1 example: ultraviolet photons are more harmful than visible photons.

The Nature of Atoms The Bohr model of the Hydrogen atom: _ + proton electron "ground state" _ + an "excited state" Text Website Video Clips

When an atom absorbs a photon, it moves to a higher energy state briefly When it jumps back to lower energy state, it emits photon(s) in a random direction, conserving the total energy of the system! (video clips)‏

Other elements Helium Carbon neutron proton Each element has its own allowed energy levels yielding a unique spectral fingerprint.

Questions? How Many Types of Spectra? What Causes spectra? Text Website Tutorial

Spectrum of the Sun Absorption spectrum What causes emission/absorption of light at specific wavelengths?