3145 Topics in Theoretical Physics - radiation processes - Dr J Hatchell. Multiwavelength Milky Way
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1 Multiwavelength Milky Way
2 PHY3145 Topics in Theoretical Physics Astrophysical Radiation Processes Dr. J. Hatchell, Physics 406,
3 Textbooks Main texts Rybicki & Lightman Radiative Processes in Astrophysics (Wiley-Interscience) unsurpassed introduction to basics, rigorous analysis, in places going further than Longair. CGS units. UL RYB Longair High Energy Astrophysics, Vols. I and II (Cambridge University Press) covers high energy processes only, chatty style. SI units. UL LON Supporting texts Griffiths, Introduction to Electrodynamics (Prentice Hall) - basic introduction to relativistic electrodynamics - UL 537 GRI Feynman, Leighton, Sands Lectures on Physics, vol. II (Addison-Wesley) - imaginative introduction to relativistic motion of charged particles - UL 530 FEY/ X Spitzer Physical processes in the Interstellar Medium (Wiley Classics) - oldfashioned but a classic. Physics library. CGS units.
4 Radiation Processes Summary Bremsstrahlung: radiation from unbound charges accelerated by Coulomb interactions Gyrotron/Cyclotron/Synchrotron: radiation from charges accelerated in a magnetic field. Gyrotron: non-relativistic Cyclotron: mildly relativistic Synchrotron: fully relativistic Thomson/Compton/Inverse Compton: scattering of radiation from charges Thomson: classical scattering, non-relativistic, low-energy photons Compton: high-energy photon scattering with wavelength shift due to loss of momentum Inverse Compton: photons gain energy due to upscattering from hot electrons
5 Radio galaxies Quasars Radio jet from galaxy Red: VLA 20cm White: HST optical Quasar radio spectra Image: Keel, Ledlow & Owen (2006 AJ ) / STSci, NRAO/AUI/NSF, NASA; Spectra: Scheuer & Williams 1968 ARAA
6 Course objectives Explain the mechanisms behind important astrophysical radiation processes: Bremsstrahlung Gyrotron/cyclotron/synchrotron Thomson scattering/compton scattering/inverse Compton Relate emission and absorption through the equation of radiative transfer (Sect. 1) Calculate the power emitted by accelerated charges in a range of situations (Sect. 2) Show how relativistic velocities affect the radiation seen by an observer (Sect. 3 & 4) Understand how your toolkit of basic physics can be applied in steps to tackle complex, research-level problems (Sect. 5). If an equation is in a coloured box, you should be able to reproduce it in the exam!
7 Course structure 1. Radiation basics. Radiative transfer. 2. Accelerated charges produce radiation. Larmor formula. Acceleration in electric and magnetic fields non-relativistic bremsstrahlung and gyrotron radiation. 3. Relativistic modifications I. Doppler shift and photon momentum. Thomson, Compton and inverse Compton scattering. 4. Relativisitic modifications II. Emission and arrival times. Superluminal motion and relativistic beaming. Gyrotron, cyclotron and synchrotron beaming. Acceleration in particle rest frame. 5. Bremsstrahlung and synchrotron spectra.
8 1. Radiation basics a) Measures of radiation b) Equation of radiative transfer Example: thermal dust emission c) Kirchoff s law for thermal emission Example: Einstein coefficients
9 Measures of radiation Luminosity L W Total power emitted in all directions Intensity I W m -2 sterad -1 I ν W m -2 Hz -1 sterad -1 Power per unit area in a particular direction per unit frequency (specific intensity) Flux F W m -2 F ν W m -2 Hz -1 Power per unit area per unit frequency (specific flux) For a source emitting isotropically
10 Emission and absorption coefficients Absorption coefficient α ν m -1 Hz -1 Emission coefficient j ν W m -3 Hz -1 sterad -1
11 Measures of radiation Quantity Symbol Unit Energy W J Power or Luminosity Power per unit solid angle W sterad -1 Intensity or surface brightness Specific intensity eg. black-body intensity Flux P L W I W m -2 sterad -1 I ν B ν W m -2 Hz -1 sterad -1 F or S F ν W m -2 W m -2 Hz -1 Emission coefficient j ν W m -3 Hz -1 sterad -1 Absorption coefficient α ν m -1 Hz -1
12 Radiative transfer Macroscopic description of the interaction of radiation with matter. Specific intensity Emission coefficient j ν Absorption coefficient α ν 1 st order differential equation. Multiply by and integrate. SEE LECTURES FOR DERIVATION
13 Radiative transfer continued Optical depth Limiting cases: Optically thick Optically thin Equation of radiative transfer source function
14 Kirchoff s law for thermal emission For thermal radiation from an emitter in equilibrium at temperature T Kirchoff s law relates emissivity j ν and absorption coeff. α ν via Planck black-body function: where is the Planck function So for a thermal emitter the equation of radiative transfer becomes
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