Widescreen Test Pattern (16:9)

Slides:



Advertisements
Similar presentations
Chapter 15: The Milky Way Galaxy
Advertisements

LECTURE 21, NOVEMBER 16, 2010 ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT 1ASTR 101-3, FALL 2010.
Measuring Our Rotation Measuring rotation in our galaxy is hard because we are inside it. One method for measuring circular rate of rotation at our radius:
Our Galaxy `. Interstellar dust obscures our view at visible wavelengths along lines of sight that lie in the plane of the galactic disk.
Kozai Migration Yanqin Wu Mike Ramsahai. The distribution of orbital periods P(T) increases from 120 to 2000 days Incomplete for longer periods Clear.
ASTR-1020 Stellar Astronomy Day 26. Galaxy Classes.
Objectives: 1.Explain current theories of how galaxies form, and change over time. 2.Know the characteristics of the milky way galaxy. 3.Compare and contrast.
Spiral Structure of Galaxies An Analytical Model.
Planet Formation Topic: Planet migration Lecture by: C.P. Dullemond.
Rotary Motion Physics Montwood High School. Rotary motion is the motion of a body around an internal axis. –Rotary motion – axis of rotation is inside.
Chapter 15 The Milky Way Galaxy.
1 LEADING PAIRS AND TRAILING SINGLE SPIRAL ARMS: l HST OBSERVATIONS AND SIMULATIONS OF NGC4622 l G. Byrd (Univ. of Alabama), l T. Freeman (Bevill State.
ANGULAR MOMENTUM AND THE STRUCTURE OF DM HALOS Chiara Tonini Special guest: Andrea Lapi Director: Paolo Salucci C.T., A. Lapi & P. Salucci (astro-ph/ ,
The Milky Way Galaxy Astronomy 315 Professor Lee Carkner Lecture 16.
Hubble images a part of the Universe
The Mass of the Galaxy We can use the orbital velocity to deduce the mass of the Galaxy (interior to our orbit): v orb 2 =GM/R. This comes out about 10.
The Milky Way Galaxy 19 April 2005 AST 2010: Chapter 24.
Stellar and Gas Kinematics in the Core and Bar Regions of M100 Emma L. Allard, Johan H. Knapen, University of Hertfordshire, UK Reynier F. Peletier, University.
Physics 106: Mechanics Lecture 01
Universe Eighth Edition Universe Roger A. Freedman William J. Kaufmann III CHAPTER 23 Our Galaxy CHAPTER 23 Our Galaxy.
The Milky Way Galaxy Astronomy 315 Professor Lee Carkner Lecture 17.
Distances. Parallax Near objects appear to move more than far objects against a distant horizon. Trigonometric parallax is used to measure distance to.
Alice Quillen University of Rochester in collaboration with Ivan Minchev Observatoire de Strassbourg Aug, 2009.
Chapter 14: The Milky Way Galaxy The scenario for the formation of galaxies is very reminiscent of the formation process for solar systems. Giant cloud.
The Milky Way Center, Shape Globular cluster system
Levels of organization: Stellar Systems Stellar Clusters Galaxies Galaxy Clusters Galaxy Superclusters The Universe Everyone should know where they live:
The Milky Way Galaxy.
ASTR112 The Galaxy Lecture 6 Prof. John Hearnshaw 10. Galactic spiral structure 11. The galactic nucleus and central bulge 11.1 Infrared observations Galactic.
Lecture 36: Galaxy Formation and Evolution.
Galaxy Characteristics Surface Brightness Alternative to Luminosity I(R) = Flux/area = erg/s/cm 2 /arcsec 2 I(0) – center flux I(R) = at radius R Define.
Galaxies Read Your Textbook: Foundations of Astronomy
Density wave theory The WKB dispersion relation for waves in disks Toomre stability (gravitational stability) of disks 4 possible types of waves in galactic.
Σπειροειδείς γαλαξίες
Advisor: Robin Ciardullo George Jacoby, John Feldmeier, Pat Durrell Kimberly Herrmann July 2 nd, 2005 Penn State Planetary Nebula Studies of Face-On Spiral.
Printed by A New Method for Corotation Determination in Spiral and Barred Galaxies Xiaolei Zhang (US Naval Research Laboratory) Ronald.
A105 Stars and Galaxies  This week’s units: 70, 71, 72, 73  News Quiz Today  Milky Way homework due Thursday  3 observing events Today’s APODAPOD.
Black Holes. The intense gravitational field left when a giant star collapses.
 Students will be able to determine the size and shape of our galaxy.  Students will be able to distinguish the different kinds of variable stars. 
Galaxy Rotation: How we know AS413 10/28/2014 D. Clemens.
Galaxies are collections of stars (between 200 billion and 400 billion) that all rotate (orbit) around a massive central point.
Finish Momentum Start Spinning Around
What governs stellar orbits of disk stars: For the most part, we can treat all the “other” stars as being uniformly spread out Don’t worry about effects.
A Rotation Pattern with Two Inner LB Resonances
Dynamics of Uniform Circular Motion
Spiral arms in the milky way galaxy and cosmic rays
1 The Milky Way Galaxy We live on the quiet outskirts of a galaxy of approximately 100 Billion stars. This galaxy, the Milky Way, is roughly disk-shaped.
Asteroseismology A brief Introduction
Today in Astronomy 328: the Milky Way Image: wide-angle photo and overlay key of the Sagittarius region of the Milky Way, showing vividly the effect of.
Rotation curves and spiral arms in galaxies - observations and theory
Spiral Density waves initiate star formation. A molecular cloud passing through the Sagittarius spiral arm Gas outflows from super supernova or O/B star.
Harry Kroto ifa.hawaii.edu Harry Kroto 2004
Copyright © 2010 Pearson Education, Inc. Clicker Questions Chapter 14 The Milky Way Galaxy.
Circular Motion and Other Applications of Newton’s Laws
M51, the Whirlpool Galaxy. Lord Rosse discovered the spiral structure in M51 in 1850 The explanation of this beautiful form has been one of the outstanding.
The Milky Way Galaxy 02/03/2005. The Milky Way Summary of major visible components and structure The Galactic Rotation Dark Matter and efforts to detect.
Galaxies: Our Galaxy: the Milky Way. . The Structure of the Milky Way Galactic Plane Galactic Center The actual structure of our Milky Way is very hard.
Universe Tenth Edition
Milky Way: Galactic Structure and Dynamics Milky Way has spiral structure Galactic Bulge surrounds the Center Powerful radio source Sagittarius A at Center.
Our Galaxy Chapter Twenty-Five. Guiding Questions 1.What is our Galaxy? How do astronomers know where we are located within it? 2.What is the shape and.
Rotation of the Galaxy. Determining the rotation when we are inside the disk rotating ourselves To determine the rotation curve of the Galaxy, we will.
Simulations for the nearby Seyfert 2 galaxy NGC 4945 Lien-Hsuan Lin 1,2, Chi Yuan 2, C.C. D. Yen 3, and S. Muller 2 1 Department of Physics, National Taiwan.
The Milky Way Galaxy. What are each of these?
Printed by A New Method for Corotation Determination in Spiral and Barred Galaxies Xiaolei Zhang (US Naval Research Laboratory) Ronald.
News flash ALMA observes a protoplanetary disk around the young star HL Tauri. This is the first time we can DIRECTLY actually observe a planetary system.
Structure of the Milky Way
Chapter 14 Spiral Galaxy.
Galaxies.
Gas Flow Induced by a Strong Bar Potential: Straight Dust Lanes Connecting to a Nuclear Starburst Ring David Yen Department of Mathematics, Fu-Jen Catholic.
The scenario for the formation of galaxies is very reminiscent of the formation process for solar systems. Giant cloud of gas and dust, shrinks under its.
The scenario for the formation of galaxies is very reminiscent of the formation process for solar systems. Giant cloud of gas and dust, shrinks under its.
Presentation transcript:

Widescreen Test Pattern (16:9) Aspect Ratio Test (Should appear circular) 4x3 16x9

Spiral Structure in Galaxies 12th March 2010 Suprit Singh (Talk for the course: Galactic Dynamics)

Overview Wave Mechanics of Differentially rotating disks Kinematic Density Waves Dispersion Relation Local Stability of Disks Spiral Structure Basics Lin-Shu Hypothesis Geometry The Winding Problem Pattern Speed

Spiral Structure: Basics

The Lin-Shu Hypothesis Lin and Shu suggested that the spiral arms can be thought of in terms of density waves: compressions and rarefactions in the distribution of stars. Coupling this with Lindblad's ideas and the hypothesis that spiral patterns are long lived lead to the Lin-Shu hypothesis that spiral structure is just a stationary density wave. Unfortunately, Lin & Shu were only half right: spiral patterns are density waves, but they're definately not stationary!

Geometry We can characterize spiral structure in terms of rotational symmetry. If I(R,f) is the observed intensity distribution in a disk then if I(R, f+2p/m) = I(R,f) (i.e. a rotation by 2p/m radians leaves the galaxy looking the same) then the galaxy (and spiral pattern) is said to have m-fold symmetry and m arms (m > 0). Most galaxies have m = 2 and the predominance of two-armed galaxies is something that any good theory of spiral structure should be able to explain.

The Winding Problem I The pitch angle at some radius R is defined as the angle between a tangent to the spiral arm and the circle R = constant. It's useful to define a function describing a mathematical curve which runs along the center of an arm. If we have m arms we can write this as The function f(R; t) is known as the shape function and allows us to define a radial wavenumber

The Winding Problem II The pitch angle is then and for galaxy with flat rotation curve W(R)R = 200km/s at R = 5 kpc and after 10 Gyr the pitch angle would be 0.14. This is much smaller than any observed galaxy and is known as the winding problem.

The Pattern Speed In the Lin-Shu hypothesis, the sprial arms are a density wave pattern that rotates rigidly. We can then always move to a rotating frame with some angular frequency Wp in which the pattern remains stationary. This pattern speed is not the same as the rotational frequency of the disk. The radius at which Wp = W (R) is known as the corotation radius. At smaller radii, W (R) > Wp . Observationally, dust lanes are seen to lie on the inside of arms as defined by bright stars. If this reflects a time lag between the point of maximum compression of gas and the formation of stars it suggests that gas is flowing into arms from the inside. Since most arms are trailing this implies that the gas is rotating faster than the spiral pattern. Therefore, spiral patterns (at least those in grand design spirals) must be inside corotation. Measuring the pattern speed is, in general, difficult (its a pattern, not a physical object) and relies on the assumption that there is in fact a well-defined pattern speed.

Wave Mechanics of Differentially rotating disks II

Kinematic Density Waves Any particle orbitting in an axissymmetric galaxy will execute a periodic orbit with some well defined period Tr. During this time, the azimuthal angle will increase by some amount Df (not necessarily equal to 2p). The corresponding radial and aziumthal frequencies are Wr = 2p/Tr and Wf = 2p/Tf We can consider the orbit in a frame which rotates with frequency Wp. In this frame, the azimuthal position of the particle if fp=f- Wpt then in one radial period Dfp = Df - Wp Tr . Choose Wp such that orbit is closed.

The Lin-Shu Theory

Tight Winding Approximation

Potential of the Spiral Pattern I

Potential of the Spiral Pattern II

Dispersion Relation I

Dispersion Relation II

Dispersion Relation III

Dispersion Relation IV

Dispersion Relation V

Dispersion Relation VI

Dispersion Relation VII (??) Not yet! Lets first see why WKB works? Dispersion Relation VII (??) Not yet! Pattern rotates at constant speed: it is a growing mode of oscillations The waves propagate in a part of the galaxy bordered by resonances and/or turning-points which deflect waves. That part acts as a resonant cavity for waves. Waves grow in the stellar disk but saturate due to the transfer of wave energy to gas disk. Waves grow between the Inner Lindblad Resonance and Corotational Res. CR region acts as an amplifier of waves due to over-reflection Density waves may exist in this ‘resonant cavity’ Two ILRs, one inner and one outer One OLR. Condition for ILR

Dispersion Relation VII (Finally!!)

Local Stability of Disks (Toomre)

That’s all Folks. Thanks for your kind attention* References : Binney and Tremaine. Galactic Dynamics 2nd Edition Bertin and Lin. Spiral Structure in Galaxies My friend Google for Images/Videos That’s all Folks. Thanks for your kind attention* *after a ‘Galactic’ amount of spiraling 