ROUGH DRAFT authorea.com/7799
Main Data History
Export
Show Index Toggle 0 comments
  •  Quick Edit
  • Phys 131 Study Guide

    Special Relativity

    Lorenz Boosts

    For a boost in the x direction,

    \[\begin{split} t' = \gamma ( t - v x) \\ x' = \gamma (x - vt) \\ y' = y \\ z' = z \\ \end{split}\]

    Fun with 4 Vectors

    \[\begin{split} \mathbf{u} = (\gamma, \gamma v) \\ \mathbf{u} \cdot \mathbf{u} = -1 \\ \mathbf{p_{\gamma}} \cdot \mathbf{p_{\gamma}} = 0 \\ E_{obs} = - p \cdot \mathbf{u} \\ \mathbf{p}^2 = m^2 \\ E^2 = p^2 + m ^2 \\ \end{split}\]

    More special relativity

    \[\begin{split} l' = \frac{l}{\gamma} \\ \Delta x' = \gamma (\Delta x - v \Delta t) \\ \Delta t' = \gamma (\Delta t - x \Delta x) \\ u' = \frac{u - v}{1- uv} \end{split}\]

    where

    \[\gamma = \frac{1}{\sqrt{1-v^2}}\]

    Principle of Equivalence

    elevators in a feely falling elevator on earth experience the same physics as someone who is not in the elevator. From this you can get the bending of light

    weight in elevator \( = m(g+a) \) so if \(a = -g\) then \(w = 0\) so gravity is not a real force and can be seen as a curvature in spacetime

    Spacetime Geometry

    \[\begin{split} ds^2 = g_{\alpha \beta} \frac{d}{d x}^{\alpha} \frac{d}{d x}^{\beta}\\ \end{split}\]

    If the time component is bigger than the space component than its time like. If the space component is bigger than the time than its spacelike. If they’re equal than its null.

    Gravitational Redshift

    In a static universe, t is ignorable so there is a killing vector \(\xi = (1,0,0,0)\). \(\xi \cdot \mathbf{u}\) is conserved along the trajectory of the particle. Therefore,

    \[\begin{split} \frac{E_{\rm{obs}}}{E_e} & = \frac{g_{tt}(e)}{g_{tt}(obs)} \\ \frac{\omega_{\inf}}{\omega_{e}} & = \sqrt{ \left( 1-\frac{2 M}{r_e} \right)} \end{split}\]

    to compare to positions, find the shift with respect to infinity to 1 and then 2 and then take the ratio to find \(\frac{\omega_1}{\omega_2}\):

    \[\frac{\omega_1}{\omega_2} = \sqrt{\frac{1-\frac{2M}{r_2}}{1-\frac{2M}{r_1}}}\]

    Schwarzchild Metric

    \[ds^2 = -(1-\frac{2GM}{r}) dt^2 + (1-\frac{2GM}{r})^{-1}dr^2 + r^2(d\theta^2+\sin^2\theta d \phi^2)\]

    Orbits of a Photon

    From the schwarzchild metric,

    \[\begin{split} e = -\xi \cdot u &= W_{\rm{eff}}(r) \frac{d t}{d \lambda} \\ l = \eta \cdot u &= r^2 \sin^2 \theta \frac{d \phi}{d \lambda} \end{split}\]

    are conserved quantities along the path of the photon.

    setting \(u \cdot u = 0\) since its a light ray with \(\theta = \frac{\pi}{2}\) gives

    \[\begin{split} u \cdot u = g_{\alpha \beta} \frac{d x^\alpha}{d \lambda}\frac{d x^\alpha}{d \lambda} \\ \frac{1}{b^2} = \frac{1}{l^2}\left( \frac{dr}{\lambda}\right)^2 + W_{\rm{eff}}(r) \end{split}\]

    where

    \[\begin{split} b^2 &= \frac{l^2}{e^2} \\ W_{\rm{eff}}(r) &= \frac{1}{r^2}(1-\frac{2M}{r}) \end{split}\]

    Another useful equation:

    \[\delta \phi_{\rm{def}} = \frac{4 G M }{c^2 b}\]

    where b is the impact parameter

    Grav Lenses

    Diagram is in figure \ref{fig:gravlense}.

    \[\theta D_{S} = \beta D_S + \alpha D_{LS}\]

    Because \(b \approx \xi\) and \(\xi \approx \theta D_L\) we can use the small angle approx. Therefore, \(\theta = \beta + \frac{\theta_{E}^2}{\theta}\). Where \(\theta_E\) is the Einstein Angle:

    \[\theta_E = \left[ 2 R_S \frac{D_{LS}}{D_{S}D_{L}} \right] ^\frac{1}{2}\]