Presentation on theme: "Bremsstrahlung 1.Review – accelerated rad. 2.Principles of brems. 3.Refer to Rybicki & Lightman Chapter 5 for discussion of thermal brems. Professor George."— Presentation transcript:
Bremsstrahlung 1.Review – accelerated rad. 2.Principles of brems. 3.Refer to Rybicki & Lightman Chapter 5 for discussion of thermal brems. Professor George F. Smoot Extreme Universe Lab, SINP Moscow State University
BREMSSTRAHLUNG RADIATION Bemsstrahlung is a German word directly describing the process: "Strahlung" means "radiation", and "Bremse" means "brake. An incoming free electron can get close to the nucleus of an atom (or other charged particle), the strong electric field of the nucleus will attract the electron, thus changing direction and speed of the electron – accelerating it. An energetic electron loses energy by emitting an X-ray photon and less energetic will emit lower energy photons. The energy of these photons will depend on the degree of interaction between nucleus and electron, i.e. the passing distance as well as the initial energy of the electron. Several subsequent interactions between one and the same electron and different nuclei are possible. X-rays originating from this process are called bremsstrahlung. Lower energy photons from this process are often called free-free emission. Free-free because the electron is free before and free after. Compare to bound-bound and free-bound interactions
Short Review of Radiation from an Accelerated Charge – e.g. brems A charged particle accelerating in a vacuum radiates power, as described by the Larmor formula and its relativistic generalizations. Although the term "bremsstrahlung" is usually reserved for charged particles accelerating in matter, not vacuum, the formulas are similar.
Review continued: Angular Distribution where n is a unit vector pointing from the particle towards the observer, and d is a infinitesimal bit of solid angle. In the case where velocity is parallel to acceleration (for example, linear motion), this simplifies to
Quantum Process Where Z is atomic number An analysis of the doubly differential cross section above shows that electrons whose kinetic energy is larger than the rest energy (511 keV) emit photons in forward direction while electrons with a small energy emit photons isotropically.
For a short constant acceleration Spectrum produced in the Bremsstrahlung process. The spectrum is flat up to a cutoff frequency wc ut, and falls off exponentially at higher frequencies.
X-ray tube In an X-ray tube, electrons are accelerated in a vacuum by an electric field and shot into a piece of metal called the "target". X-rays are emitted as the electrons slow down (decelerate) in the metal. The output spectrum consists of a continuous spectrum of X-rays, with additional sharp peaks at certain energies (see graph on right). The continuous spectrum is due to bremsstrahlung, while the sharp peaks are characteristic X-rays associated with the atoms in the target. For this reason, bremsstrahlung in this context is also called continuous X-rays. pm is picometers
Simple Bremsstrahlung Formula for free-free radiation Makes it easy to estimate the bremsstrahlung produced radiation field for a reasonable temperature plasma. For much hotter plasma one must take the gaunt factor in to more careful account. For reasonable temperature there is log rise
Bremsstrahlung Probability of bremsstrahlung production per atom is proportional to the square of Z of the absorber Energy emission via bremsstrahlung varies inversely with the square of the mass of the incident particle –Protons and alpha particles produce less than one-millionth the amount of bremsstrahlung radiation as electrons of the same energy
Bremsstrahlung Ratio of electron energy loss by bremsstrahlung production to that lost by excitation and ionization = EZ/820 –E = kinetic energy of incident electron in MeV –Z = atomic number of the absorber Bremsstrahlung x-ray production accounts for ~1% of energy loss when 100 keV electrons collide with a tungsten (Z = 74) target in an x-ray tube
Thermal Bremsstrahlung The emission of a single electron, with impact parameter b and velocity v. We would now like to generalize the results to a population of electrons with a certain velocity and density distribution. An astrophysically useful case is for a population with a uniform temperature T. The total emission by all particles in this population is called thermal bremsstrahlung. Consider an cloud of ionised gas with a characteristic temperature T. The velocity distribution of the particles in this cloud is given by the Maxwell distribution. In cgs units the power emitted per cubic cm is Here, g B is the frequency averaged gaunt factor for the thermal distribution of velocities, and is of order unity.
Thermal Bremsstrahlung Power Spectrum The bremsstrahlung power spectrum rapidly decreases for large photon energy, and is also suppressed near the Electron plasma frequency p. This plot is for the quantum case.
Bethe-Heitler Eqn An analysis of the doubly differential cross section above shows that electrons whose kinetic energy is larger than the rest energy (511 keV) emit photons I n forward direction while electrons with a small energy emit photons isotropically.
So what sort of temperatures and energies are involved in high energy thermal radiation? First let’s review a few equations related to electromagnetic radiation. To calculate the thermal source temperature we use Wien’s law: x10 6 nm K max T = The photon energy and momentum are related to frequency via: E = h and Momentum = h / c where h is Planck ’ s constant Recall that wavelength and frequency are related via: c = where c is the speed of light Click hereClick here to be reminded about the physical constants and units used. This means that when a photon loses energy and momentum, its frequency decreases. Thermal Issues
Gamma radiation is generally defined by photons with 1.24 MeV and T >10 8 K. Such high energy photons are created in nuclear reactions and other very high energy processes. X-rays are those photons in within the wavelength range nm < < 10 nm, with 124 eV < E < 1.24 MeV and 10 6 K < T < 10 8 K. These high energy photons are created, for example, in supernovae remnants and the solar corona, as well as in the hot gas between galaxy clusters. Armed with these equations, we can now see what thermal temperatures and energies are involved in high energy radiation: Gamma & X-rays Ranges
Types of Thermal Radiation You are familiar with atomic excitation and de-excitation as a means of producing photons. Thermal atomic excitation is generally via collisions, which excite atoms, and as they de-excite, they emit photons. The hotter the medium, the higher the kinetic energy of the impacts, and the higher the resulting photon energy. photon
H+H+ e-e- If a negative electron approaches a positive ion, they will be attracted to each other and the strong electric force will alter the trajectory of the electron (i.e. accelerating it), which leads to electromagnetic radiation being emitted: This type of emission form is called free-free emission, or thermal bremsstrahlung - which is German for “braking radiation”. As well as atomic excitation, another thermal process is bremsstrahlung radiation, which occurs when free electrons interact with ions in, for example, the hot atmospheres of stars. Thermal Bremsstrahlung
The frequency range of the radiation depends on how much the electron’s trajectory is bent by the interaction with the positive ion. This depends on several things, including the relative velocities of the two bodies, which in turn depends on the temperature of the gas, which is why free-free emission is a thermal process. An example of high energy thermal bremsstrahlung is the X-ray emission from giant elliptical galaxies and hot intercluster gas. X-ray image of hot intercluster gas in Hydra A Energy of Thermal Bremsstrahlung
Bremsstrahlung Radiation Movie of the bremsstrahlung process
BREMSSTRAHLUNG ON HEAVY NUCLEUS Movie of bremsstrahulung on a heavy nucleus with bound electrons. This is more relevant to detectors and man-generated x-rays than astro
DIFFERENT DEGREES OF DECCELERATION X-RAYS HEAT
BREMS RADIATION IS: POLYENERGETIC ! 90% OF X-RAYS ARE PRODUCED THROUGH BREMS INTERACTIONS WHEN KVP APPLIED
BREMS EMISSION- CONTINUOUS
The high energy electron can also cause an electron close to the nucleus in a metal atom to be knocked out from its place. This vacancy is filled by an electron further out from the nucleus. The well defined difference in binding energy, characteristic of the material, is emitted as a monoenergetic photon. When detected this X-ray photon gives rise to a characteristic X-ray line in the energy spectrum. Characteristic X-rays
Characteristic Radiation KE OF PROJECTILE ELECTRON > BINDING ENERGYORBITAL ELECTRON
TUNGSTEN-74 K-70 KEV L-12 KEV M-2.8 KEV BINDING ENERGIES OF DIFFERENT SHELL ELECTRONS
CHARACTERISTIC X-RAYS L K = 58 keV MK 70-3 = 67 keV M L 12-3 = 9 keV
Bremsstrahlung “Free-free Emission” “Braking” Radiation Radiation due to acceleration of charged particle by the Coulomb field of another charge. Relevant for (i) Collisions between unlike particles: changing dipole emission e-e-, p-p interactions have no net dipole moment (ii) e- - ions dominate: acc(e-) > acc(ions) because m(e-) << m(ions) recall P~m -2 ion-ion brems is negligible Bremsstrahlung
Method of Attack: (1) emission from single e- pick rest frame of ion calculate dipole radiation correct for quantum effects (Gaunt factor) (2) Emission from collection of e- thermal bremsstrahlung or non-thermal bremsstrahlung (3) Relativistic bremsstrahlung (Virtual Quanta)
A qualitative picture
Emission from Single-Speed Electrons v e- R Ze ion b Electron moves past ion, assumed to be stationary. b= “impact parameter” - Suppose the deviation of the e- path is negligible small-angle scattering The dipole moment is a function of time during the encounter. - Recall that for dipole radiation whereis the Fourier Transform of
After some straight-forward algebra, (R&L pp. 156 – 157), one can derive in terms of impact parameter, b.
Now, suppose you have a bunch of electrons, all with the same speed, v, which interact with a bunch of ions.
Let n i = ion density (# ions/vol.) n e = electron density (# electrons / vol) The # of electrons incident on one ion is # e-s /Vol d/t around one ion, in terms of b
So total emission/time/Vol/freq is Again, evaluating the integral is discussed in detail in R&L p We quote the result
Energy per volume per frequency per time due to bremsstrahlung for electrons, all with same velocity v. Gaunt factors are quantum mechanical corrections function of e- energy, frequency Gaunt factors are tabulated (more later)
Naturally, in most situations, you never have electrons with just one velocity v. Maxwell-Boltzmann Distribution Thermal Bremsstrahlung Average the single speed expression for dW/dwdtdV over the Maxwell-Boltzmann distribution with temperature T: The result, with
where In cgs units, we can write the emission coefficient Free-free emission coefficient ergs /s /cm 3 /Hz
Integrate over frequency: where In cgs: Ergs sec -1 cm -3
The Gaunt factors - Analytical approximations exist to evaluate them - Tables exist you can look up - For most situations, so just take
Numerical Values of gaunt factor
Handy table, from Tucker: Radiation Processes in Astrophysics
Important Characteristics of Thermal Bremsstrahlung Emissivity (1) Usually optically thin. Then (2) is ~ constant with hν at low frequencies (3) falls of exponentially at
VLA (radio region) ``image'' of Perseus A, overlayed on the X-ray image from the Chandra telescope. The central source is clearly seen, as well as radio lobes which loosely coincide with the two circum-nuclear ``bubbles'' in the X-ray image.
Examples : Important in hot plasmas where the gas is mostly ionized, so that bound-free emission can be neglected. Solar flare10 7 (~ 1keV)radio flat X-ray exponential H II region10 5 radio flat Orion10 4 radio-flat Sco X optical-flat X-ray flat/exp. Coma Cluster ICM10 8 X-ray flat/exp. T ( o K)Obs. of
Bremsstrahlung (free-free) absorption Recall the emission coefficient, jν, is related to the absorption coefficient αν for a thermal gas: is isotropic, soand thus in cgs: Brems emission Inverse Bremss. free-free abs. e- ion e- photon collateral
Important Characteristics of (1)(e.g. X-rays) Because of term, is very small unless n e is very large. in X-rays, thermal bremsstrahlung emission can be treated as optically thin (except in stellar interiors)
(2)e.g. Radio: Rayleigh Jeans holds Absorption can be important, even for low n e in the radio regime.
From Bradt’s book: BB spectrum is optically thick limit of Thermal Bremss.
HII Regions, showing free-free absorption in their radio spectra:
R&L Problem 5.2 Spherical source of X-rays, radius R distance L=10 kpc flux F= erg cm -2 s -1 (a) What is T? Assume optically thin, thermal bremsstrahlung. Turn-over in the spectrum at log hν (keV) ~ 2
(b) Assume the cloud is in hydrostatic equilibrium around a central mass, M. Find M, and the density of the cloud, ρ Vol. 1/r 2 Vol. emission coeff.
- Since T=10 9 K, the gas is completely ionized - Assume it is pure hydrogen, so n i = n e, then ρ=mass density, g/cm3 Z=1 since pure hydrogen (1)
- Hydrostatic equilibrium another constraint upon ρ, R Virial Theorem: For T=10 9 K(2) - Eqn (1) & (2) Substituting L=10 kpc, F=10 -8 erg cm -2 s -1