AY202a Galaxies & Dynamics Lecture 7: Jeans’ Law, Virial Theorem Structure of E Galaxies Jean’s Law

Star/Galaxy Formation is most simply defined as the process of going from hydrostatic equilibrium to gravitational collapse. There are a host of complicating factors --- left for a graduate course: Rotation Cooling Magnetic Fields Fragmentation …………… The Simple Model

Mc Assume a spherical, isothermal gas cloud that starts near Rc hydrostatic ρo Rc equlibrium: T 2K + U = 0 c (constant density) Spherical Gas Cloud Rc U = ∫ -4πG M(r) ρ(r) r dr 0 3 GM 2 ~ − c Potential 5 R c Energy

Mc = Cloud Mass Rc = Cloud Radius M ρ = constant density = c 0 3 4/3 π Rc The Kinetic Energy, K, is just K = 3/2 N k T where N is the total number of particles,

N = MC /(µ mH) where µ is the mean molecular weight and

mH is the mass of Hydrogen The condition for collapse from the Virial theorem (more later) is 2 K < |U| So collapse occurs if

2 3 MC kT 3G MC < µ mH 5 RC and substituting for the cloud radius, 1/3 3 MC RC = ( ) 4πρ0 We can find the critical mass for collapse:

5 k T 3/2 3 1/2 MC > MJ ~ ( ) ( ) G µ mH 4 πρ0 If the cloud’s mass is greater than MJ it will collapse. Similarly, we can define a critical radius, RJ, such that if a cloud is larger than that radius it will collapse:

15 k T 1/2 RC > RJ ~ ( ) 4 π G µ mH ρ0

and note that these are of course for ideal conditions. Rotation, B, etc. count. Mass Estimators: The simplest case = zero energy bound orbit. Test particle in orbit, mass m, velocity v, radius R, around a body of mass M E = K + U = 1/2 mv2 - GmM/R = 0 1/2 mv2 = GmM/R M = 1/2 v2 R /G This formula gets modified for other orbits (i.e. not zero energy) e.g. for circular orbits 2K + U = 0 so M = v2 R /G What about complex systems of particles? The Virial Theorem

Consider a moment of inertia for a system of N particles and its derivatives:

N I = ½ Σ m r . r (moment of inertia) i=1 i i i . . . I = dI/dt = Σ mi ri ri ...... 2 2 . . I = d I/dt = Σ mi (ri ri + ri ri ) Assume that the N particles have mi and ri and are self gravitating --- their mass forms the overall potential. We ..can use the equation of motion to elimiate ri : .. Gmimj miri = −Σ 3 ( ri - rj ) j = i |ri –rj| and note that . . . Σ miri ri = 2T (twice the Kinetic Energy) Then we can write (after substitution) .. Gm m i j . I – 2T = − Σ Σ 3 ri (ri – rj) i j=i |ri - rj| Gmi mj . reversing = − Σ Σ 3 rj (rj – ri) labels j i=j |rj - ri| Gmi mj . = − ½ Σ Σ 3 (ri - rj) (ri – rj) adding i j=i |ri - rj|

Gmi mj = − ½ Σ Σ = U the potential energy |ri - rj| .. I = 2T + U If we have a relaxed (or statistically steady) system which is.. not changing shape or size, d2I/dt2 = I = 0 2T + U = 0; U = -2T; E = T+U = ½ U conversely, for a slowly changing or periodic system 2 + = 0 Virial Equilibrium Virial Mass Estimator We use the Virial Theorem to estimate masses of astrophysical systems (e.g. Zwicky and Smith and the discovery of Dark Matter) Go back to: N N 2 1 Σ mi = ΣΣ Gmimj < > i=1 i=1 j denotes the time average, and we have N point masses of mass mi, position ri and velocity vi Assume the system is spherical. The observables are (1) the l.o.s. time average velocity: 2 2 < v R,i> Ω = 1/3 vi

projected radial v averaged over solid angle i.e. we only see the radial component of motion &

vi ~ √3 vr Ditto for position, we see projected radii R, R = θ d , d = distance, θ = angular separation So taking the average projection,

1 1 1 = < >Ω |r – r | < sin θ >Ω |Ri – Rj| i j ij and π ∫ dθ 1 ∫ (sinθ)-1dΩ 0 = = 0 = π/2 < sin θij >Ω dΩ ∫ π sinθ dθ

Remember we only see 2 of the 3 dimensions with R Thus after taking into account all the projection effects, and if we assume masses are the same

so that Msys = Σ mi = N mi we have 2 3π Σ vi M = N VT 2G Σ (1/R ) iVelocity dispersion -1 [ Σ (1/Rij)] = Harmonic Radius i

In the 1980’s, the search for a stable mass estimator led Bahcall & Tremaine and eventually Heisler, Bahcall & Tremaine to posit a new estimator with the form

~ [dispersion x size ] Derived PM Mass estimator checked against simulations: f M = p Σ v 2 R where P GN i i,c

Ri,c = Projected distance from the center vi = l.o.s. difference from the center fp = Projection factor which depends on (includes) orbital eccentricities The projection factor depends fairly strongly on the average eccentricities of the orbits of the objects (galaxies, stars, clusters) in the system: fp = 64/π for primarily Radial Orbits = 32/π for primarily Isotropic Orbits = 16/π for primarily Circular Orbits (Heisler, Bahcall & Tremaine 1985) Richstone and Tremaine plotted the effect of eccentricity vs radius on the velocity dispersion profile: Expected projected l.o.s. sigmas

Richstone & Tremaine Applications: Coma Cluster (PS2) M31 Globular Cluster System 11 σ ~ 155 km/s MPM = 3.1+/−0.5 x 10 MSun Virgo Cluster (core only!) 14 σ ~ 620 km/s MVT = 7.9 x 10 MSun 14 MPM = 8.9 x 10 MSun Etc.

M31 G1 = Mayall II M31 Globular Clusters (Perrett et al.)

The Structure of Elliptical Galaxies Main questions 1. Why do elliptical galaxies have the shapes they do? 2. What is the connection between light & mass & kinematics? = How do stars move in galaxies? Basic physical description: star piles. For each star we have (r, θ, ϕ) or (x,y,z) and (dx/dt, dy/dt, dz/dt) = (vx,vy,vz) the six dimensional kinematical phase space Generally treat this problem as the motion of stars (test particles) in smooth gravitational potentials For the system as a whole, we have the density, ρ(x,y,z) or ρ(r,θ,ϕ) The Mass M = ∫ ρ dV ρ(x’) The Gravitational Φ(x) = -G ∫ d3x’ |x’-x| Potential Force on unit mass at x F(x) = - ∇Φ(x) plus Energy Conservation Angular Momentum Conservation Mass Conservation (orthogonally) Plus Poisson’s Equation: ∇2Φ = 4 πGρ (divergence of the gradient) Gauss’s Theorem 4 π G ∫ ρ dV = ∫ ∇Φ d2S enclose mass surface integral For spherical systems we also have Newton’s theorems: 1. A body inside a spherical shell sees no net force 2. A body outside a closed spherical shell sees a force = all the mass at a point in the center. The potential Φ = -GM/r The circular speed is then G M(r) v 2 = r dΦ/dr = c r and the escape velocity from such a potential is ve = √ 2 | Φ(r) | ~ √ 2 vc For homogeneous spheres with ρ = const r ≤ rs = 0 r > rs 4πGρ v = 1/2 r c ( 3 ) We can also ask what is the “dynamical time” of such a system ≡ the Free Fall Time from the surface to the center. Consider the equation of motion 2 d r = - G M ( r ) = - 4 π G ρ r dt2 r2 3

Which is a harmonic oscillator with frequency 2π/T where T is the orbital peiod of a mass on a 1/2 circular orbit T = 2πr/vc = (3π/Gρ) Thus the free fall time is ¼ of the period 3π ½ td = ( 1 6 G ρ ) The problem for most astrophysical systems reduces to describing the mass density distribution which defines the potential. E.g. for a Hubble Law, if M/L is constant 2 -2 2 I(r) = I0/(a + r) = I0a /(1 + r/a)

2 -3/2 2 -3/2 so ρ(r) ∝ [(1 + r/a) ] ∝ ρ0 [(1 + r/a) ] A distributions like this is called a Plummer model --- density roughly constant near the center and falling to zero at large radii For this model Φ = - GM √r2 + a2 By definition, there are many other possible spherical potentials, one that is nicely integrable is the isochrone potential - GM Φ(r) = b + √b2 +r2 Today there are a variety of “two power” density distributions in use

ρ0 ρ(r) = (r/a)α (1 – r/a)β-α

With β = 4 these are called Dehnen models β = 4, α = 1 is the Hernquist model β = 4, α = 2 is the Jaffe model β = 3, α = 1 is the NFW model Circular velocities versus radius

Mod Hubble law Dehnen like laws Theory’s End

There is a theory which states that if ever anyone discovers exactly what the Universe is for and why it is here, it will instantly disappear and be replaced by something even more bizzare and inexplicable. There is another theory which states that this has already happened. Douglas Adams