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Relaxation Time Today in Astronomy 142: the Milky Way’s disk More on stars as a gas: stellar relaxation time, equilibrium Differential rotation of the stars in the disk The local standard of rest Rotation curves and the distribution of mass The rotation curve of the Galaxy Figure: spiral structure in the first Galactic quadrant, deduced from CO observations. (Clemens, Sanders, Scoville 1988) 21 March 2013 Astronomy 142, Spring 2013 1 Stellar encounters: relaxation time of a stellar cluster In order to behave like a gas, as we assumed last time, stars have to collide elastically enough times for their random kinetic energy to be shared in a thermal fashion. But stellar encounters, even distant ones, are rare on human time scales. How long does it take a cluster of stars to thermalize? One characteristic time: the time between stellar elastic encounters, called the relaxation time. If a gravitationally bound cluster is a lot older than its relaxation time, then the stars will be describable as a gas (the star system has temperature, pressure, etc.). 21 March 2013 Astronomy 142, Spring 2013 2 Stellar encounters: relaxation time of a stellar cluster (continued) Suppose a star has a gravitational “sphere of influence” with radius r (>>R, the radius of the star), and moves at speed v between encounters, with its sphere of influence sweeping out a cylinder as it does: v V= π r2 vt r vt If the number density of stars (stars per unit volume) is n, then there will be exactly one star in the cylinder if 2 1 nV= nπ r vtcc =⇒=1 t Relaxation time nrvπ 2 21 March 2013 Astronomy 142, Spring 2013 3 Stellar encounters: relaxation time of a stellar cluster (continued) What is the appropriate radius, r? Choose that for which the gravitational potential energy is equal in magnitude to the average stellar kinetic energy. Gm231 v =2 ⇒= mv tc r 2 4πGmn22 Done in more detail (Astronomy 232-level): for a spherical cluster with a “core” radius R, it can be shown that v3 1 t = . c 22 4πGmnln( 2Rr) Not that far from our rough estimate, as the logarithm is a very slow function. 21 March 2013 Astronomy 142, Spring 2013 4 Stellar encounters: relaxation time of a stellar cluster (continued) In this week’s homework, you will show among other things that for such a cluster of N stars, with core radius R and typical stellar mass m, GN( −−11) m Gm2 GN( ) m2 v2 = and = 24R rR Assume N >> 1 and substitute these into the expression for relaxation time: 2RN tc ≅ v N 24ln 2 The time t x = 2 Rv is called the crossing time; it’s the time it takes a star moving at the mean speed v to traverse the core of the cluster (diameter 2R) if it doesn’t collide. 21 March 2013 Astronomy 142, Spring 2013 5 Thermal equilibrium A handy way for bookkeeping random motions in thermal equilibrium is the virial theorem: In an isolated system of particles that exert forces on each other describable by scalar potentials, the system’s moment of inertia I, total kinetic energy K, total potential energy U and total mechanical energy E are related by 22 d I dt=2. K +=+ U K E In many cases (see, e.g., this week’s recitation), d22 I dt = 0, for which K, U and E are related by 1 K=−=− UE. 2 It is often easy to calculate U and the systematic-motion part of K; thus we can get the random-motion part of K. 21 March 2013 Astronomy 142, Spring 2013 6 Thermal equilibrium (continued) For example: suppose a uniform-density star cluster – N stars of mass m, Nm = M – has radius R and rotates like a solid body at angular speed Ω. What is the random speed v of a typical star in this cluster? Obviously d 22 I dt = 0, since the cluster’s structure is constant, so 122 11 K=∑ mvii + I Ω=− U 2i 22 N 12 13GM2 mv2+ MR 22 Ω= 2 25 25 R 32GM vR= −Ω22 55R 21 March 2013 Astronomy 142, Spring 2013 7 Thermal equilibrium (continued) We will resist the temptation to prove the virial theorem here; though the proof isn’t difficult, it’s long and complicated. It will be proven for you in PHY 235 and AST 232. If you can’t wait, see FA, pp. 78-80. Caveats: The virial theorem applies only to thermal equilibrium or steady-state motion. Thus, before every use, one should check to see whether the system on which one’s using it has been around long enough to be in thermal equilibrium. Long enough means the system has been together for a time much longer than the relaxation time. 21 March 2013 Astronomy 142, Spring 2013 8 Rotation of the stellar population Averaging over the random motions, one can detect differential rotation in the disk of the galaxy, from the radial velocities of nearby stars. The rotation is differential in the sense that different radii have different angular velocities. • The angular velocity decreases monotonically as radius from the Galactic center increases. Measurement of average stellar motions along the line of sight and perpendicular to the line of sight can be used to determine the local angular velocity. Unfortunately, motions perpendicular to the line of sight (proper motions) are currently hard to measure for enough stars, and stars that are far away. 21 March 2013 Astronomy 142, Spring 2013 9 Rotation of the stellar population, and Oort’s constants vr Oort’s constants, defined: vt d Sun rdΩ 1 d 2 A=−=−Ω Br vt 22dr r dr ( ) vr whence Ω=AB − In terms of the average radial velocities and average proper motions: = = + vrt Adsin 2 v Adcos 2 Bd In the absence of proper motions (vt), B is usually obtained less directly from the statistics of random motions, with the result 1−=AB / 1.6. 21 March 2013 Astronomy 142, Spring 2013 10 Oort’s constants (continued) The measurement of the Oort A constants thus requires good , km/sec radial velocity measurements (v ), d r / r proper motions (v ), and distances v t A (d) over a wide range of distance. These days one can’t measure very well for stars very far away, but this will improve drastically with the upcoming B ESA Gaia mission. , km/sec d / t Figures: vr /d (upper) and vt /d v 2A (lower) for classical Cepheid variable stars. From FA. 21 March 2013 Astronomy 142, Spring 2013 11 The local standard of rest From A and B we get the average rotational motion of the Sun’s orbit, called the local standard of rest (LSR): Ω=(9.8 ± 0.9) × 10−16 radians s-1 =±=±-1 vrφ 254 16 km s 8.4 0.6 kpc P =(200 ±× 20) 106 years The solar system actually moves slightly with respect to the LSR, at about 7 km/s. From the motion of the LSR, the Galaxy within r = 8.4 kpc can be weighed: vr2 φ 11 MM= =±×(1.3 0.2) 10 . G (Reid et al. 2009.) 21 March 2013 Astronomy 142, Spring 2013 12 Rotation curves The average orbits in the disk of the Galaxy seem to be circular, centered on the Galactic center. A measurement of average angular velocity at any radius allows a determination of the mass within that radius of the Galactic center. Done as a function of radius: rotation curve • Enables determination of enclosed mass, and in turn the density, as a function of r. Interstellar gas has far smaller random motions than stars, is widespread, and detectable throughout the galaxy; atomic (e.g. H I 21 cm) and molecular (e.g. CO 2.6 mm) lines are the best to use for determination of the Galactic rotation curve. 21 March 2013 Astronomy 142, Spring 2013 13 Example rotation curves 1. Point mass, M: Keplerian motion GMm mv2 GM F = = ⇒=vr() v decreases with 2 r rrincreasing r 2. Constant density, spherically symmetric: 4π Mr( ) = ρ r3 3 0 2 Gm Gm4π 3 mv Mr( ) = ρ0r = rr223 r 4πρG Solid-body rotation ⇒=vr() r 0 3 v increases linearly with increasing r 21 March 2013 Astronomy 142, Spring 2013 14 Example rotation curves (continued) 3. Spherical symmetry, 1 / r 2 density distribution: 2 r0 ρρ= 00(r : core radius of galaxy) r2 rr M( r) = ρ( r′) 44 π r ′′22 dr= πρ r dr ′ ∫∫0000 2 =4πρ00rr ∝ r GmM( r) Gm mv2 = 4πρ rr2 = 2200 rr r vr( ) = 4πρ G r2 = constant Flat rotation curve 00 As we will see, many rotation curves of disk galaxies, including ours, look like this one. 21 March 2013 Astronomy 142, Spring 2013 15 Measurement of Galaxy’s rotation curve from H I and CO line profiles Wavelength or frequency shift and radial velocity: the Doppler effect. λλ− ∆∆λνv 0 ==−=r λλν000c Along a given line of sight through the plane, maximum radial velocity must come from orbit tangent to line of sight: motion parallel to line of sight, cosφ = 1. • Thus distance and rotational motion of tangent points very well determined. there is a distance ambiguity: for lines of sight toward the inner galaxy (first and fourth quadrant), there are two locations with the same radial velocity. 21 March 2013 Astronomy 142, Spring 2013 16 Interpretation of H I line profiles Sun 21 cm 1,3 line r 1 intensity 4 2 5 r2 2 3 0 4 Radial velocity (vr ) 5 21 March 2013 Astronomy 142, Spring 2013 17 Measurement of Galaxy’s rotation curve from H I and CO line profiles (continued) Resolution of the ambiguity usually involves information other than velocities: association or lack thereof with visible-wavelength nebulosity (less extinguished = nearer).
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