Spiral Galaxy - Canis Venitici We can only see about 1/6 (ca 6000ly) of the way to the Galctic Centre due to scattering by gas and dust in the disk.

Slides:



Advertisements
Similar presentations
Galaxy Classification
Advertisements

The Birth of Stars Chapter Twenty. Interstellar gas and dust pervade the Galaxy Interstellar gas and dust, which make up the interstellar medium, are.
Chapter 19: Between the Stars: Gas and Dust in Space.
© 2010 Pearson Education, Inc. The Milky Way. © 2010 Pearson Education, Inc. Dusty gas clouds obscure our view because they absorb visible light. This.
The Interstellar Medium (ISM): The Birth of Stars.
The Interstellar Medium Astronomy 315 Professor Lee Carkner Lecture 19.
First Hour Test –Wednesday 16 February –Bring two No. 2 pencils –An eraser (“Do you feel lucky?”) –A photo ID –Something to write on Review Session –Tuesday.
Taking the fingerprints of stars, galaxies, and interstellar gas clouds Absorption and emission from atoms, ions, and molecules.
IQ Radio, x-ray and infrared radiation are all examples of: A. Magic
An external galaxy; a spiral like our own.. Which way does it rotate?
Chapter 11: The Interstellar Medium Region in the Constellation Orion named the Orion Nebula which is the closest star formation region to us. Jets and.
Chapter 15: Chapter 15: The Milky Way Galaxy. Lesson Plan Idea of Gallaxies Idea of Gallaxies Parson’s observations Parson’s observations Hubble’s observations.
Galaxy  A large collection of stars  Galaxies contain star groups  Galaxies only contain 1% of matter in the universe  The remaining 99% of matter.
Susan CartwrightOur Evolving Universe1 Atoms and Starlight n Why do the stars shine? l l planets shine by reflected sunlight—but what generates the Sun’s.
Star Properties studied so far… Period Mass Eccentricity Red shift Velocity Temperature (Wiens Law) Composition – which elements and how much of each Color.
Interstellar Dust and Gas. In 1783 William Herschel began a survey of the heavens using an 18 ¾ inch reflector of his own construction. His goal was to.
Stars & Gas: Building Blocks of the Galaxy Stars as Black Body Radiators Hertzsprung-Russell diagram: Luminosity vs. Temperature Radiation over a `continuous'
The Big Stuff Galaxies The Universe and The Big Bang.
The Birth of Stars -part I Chapter Twenty. Announcements I need from you a LIST on questions every end of the class near the door so I can KNOW what you.
Chapter 4 Spectroscopy.
Chapter 18 The Interstellar Medium. 18.1Interstellar Matter 18.2Emission Nebulae 18.3Dark Dust Clouds Centimeter Radiation 18.5Interstellar Molecules.
THIS PRESENTAION HAS BEEN RATED BY THE CLASSIFICATION AND RATING ADMINISTRATION TG-13 TEACHERS’ GUIDANCE STRONGLY ADVISED Some Material May Be Unintelligible.
Galaxies Chapter 16. Topics Types of galaxies Dark Matter Distances to galaxies Speed of galaxies Expansion of the universe and Hubble’s law.
The Launch Pad Tuesday, 8/31/10 What will be the ultimate fate of our Sun?
{ On the Shoulders of Giants Organization of the universe.
Photoelectron Spectrometers Survey of the Universe Harry Kroto 2004.
Note that the following lectures include animations and PowerPoint effects such as fly-ins and transitions that require you to be in PowerPoint's Slide.
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.
Physical properties. Review Question What are the three ways we have of determining a stars temperature?
ASTR112 Astrophysics: the Galaxy Prof. John Hearnshaw 2003 semester 1 Room 804, Rutherford Building Department of Physics and Astronomy
The Interstellar Medium and Star Formation Material between the stars – gas and dust.
What's in our galaxy?.
Star Formation (Compare: Solar System Formation).
PHYS Black Holes If the mass of the core is more than about 3 solar masses the neutron degeneracy is overwhelmed and the core goes on collapsing.
Harry Kroto 2004 Sodium Flame Test. © at: commons.wikimedia.org/wiki/File:Flametest--Na...commons.wikimedia.org/wiki/File:Flametest--Na...
The Interstellar Medium. Red, White, and Blue : Nebulae.
AST101 Lecture 20 The Parts of the Galaxy. Shape of the Galaxy.
AIM: Galaxies and the Universe Do Now: Compare the North Star (Polaris) with the Sun.
ASTR112 The Galaxy Lecture 2 Prof. John Hearnshaw 2. Constituents of the Galaxy 3. Structure of the Galaxy 4. The system of galactic coordinates 5. Stellar.
Lecture 6: Weighing Galaxies --Dark Matter Astronomy 5: The Formation and Evolution of the Universe Sandra M. Faber Spring Quarter 2007 UC Santa Cruz.
Stars are formed from _______ ___ and ____ coming together due to _______. All stars begin with the _______ ______. What happens then depends on the ____.
ASTR112 The Galaxy Lecture 9 Prof. John Hearnshaw 12. The interstellar medium: gas 12.3 H I clouds (and IS absorption lines) 12.4 Dense molecular clouds.
Galaxies Milky Way and Beyond.
H Atom 21 cm Line. Is the Milky Way a Spiral Galaxy like this one?
AST101 Lecture 20 Our Galaxy Dissected. Shape of the Galaxy.
Stellar NurseriesStages of Star Birth. The interstellar medium The space between the stars is not empty.
{ To Infinity and Beyond… The Classification of Stars and Galaxies.
The Big Bang.  Cosmology – The study of the structure and evolution of the universe.  Big Bang Theory – The universe was very hot and small. Billions.
Star Formation The stuff between the stars Nebulae Giant molecular clouds Collapse of clouds Protostars Reading
Formation of the Solar System and The Universe. Our Solar System Sun is the center of a huge rotating system of: Sun is the center of a huge rotating.
The Interstellar Medium and Star Formation
Stars and Galaxies.
The Interstellar Medium and Star Formation
Galaxies and Formation
“Forbidden Transitions”
Queen Magazine Harry Kroto 2004.
Spiral Arms.
WHERE STARS ARE BORN.
Title: 30.1 Galaxies and The Universe
The Discovery of the Interstellar Medium (ISM)
Chapter 11 The Cone Nebula
The ISM and Stellar Birth
Doppler Shifts of Interstellar NaD lines
Nebula.
Region in the Constellation Orion named the Orion Nebula which is the closest star formation region to us. Jets and disks appear to be part of the star.
Queen Magazine Harry Kroto 2004.
Prepare your scantron:
Rayleigh scattering. Rayleigh scattering Harry Kroto 2004.
Harry Kroto 2004.
The Discovery of the Interstellar Medium (ISM)
Presentation transcript:

Spiral Galaxy - Canis Venitici

We can only see about 1/6 (ca 6000ly) of the way to the Galctic Centre due to scattering by gas and dust in the disk

Diffuse Nebula

Attenuation due to scattering by interstellar gas and dust clouds

ν →ν → Rotating binary star system with one dark companion Diffuse interstellar cloud Absorption against the hot background emission exhibits a varying Doppler Shift Absorption of an atom in interstellar cloud unshifted Absorption line of an atom in the cool atmosphere in the spectrum of a star

Multiple Clouds in the Line of Sight Na D Lines Ca Line

Doppler Shifts in Interstellar lines  /  =  / = v/c

Rosette Nebula

Scattering by interstellar Gas and Dust

Hartman 1904 K Ti Fe Ca Na T (100K) BinaryDiffuse cloud

Multiple Clouds in the Line of Sight

Harry Kroto 2004

Feedback: Privacy Policy Feedback
Do Not Sell My Personal Information
About project: SlidePlayer Terms of Service

© 2024 SlidePlayer.com Inc. All rights reserved.