Presentation on theme: "Physics of the Atmosphere 2 Radiation and Energy Balance Lecture, Summer Term 2015 Ulrich Foelsche Institute of Physics, Institute for Geophysics, Astrophysics,"— Presentation transcript:
Physics of the Atmosphere 2 Radiation and Energy Balance Lecture, Summer Term 2015 Ulrich Foelsche Institute of Physics, Institute for Geophysics, Astrophysics, and Meteorology (IGAM) University of Graz und Wegener Center for Climate and Global Change firstname.lastname@example.org http://www.uni-graz.at/~foelsche/
Textbooks Atmo II 01 C. Donald Ahrens, Meteorology Today: An Introduction to Weather, Climate, and the Environment, Brooks/Cole, 9. Ed., ISBN: 0495555746 (also paperback) UB-Semesterhandapparat, IGAM-Library K.N. Liou, (Ed.), An Introduction to Atmospheric Radiation, Academic Press, 2nd Ed., ISBN: 978-0-12-451451-5, 2002 (partial) Murry L. Salby, Physics of the Atmosphere and Climate, Cambridge Univ. Press, 2nd Ed., ISBN: 978-0-521-76718-7, 2012 (partial)
Lehrbücher Helmut Kraus, Die Atmosphäre der Erde - Eine Einführung in die Meteorologie, Springer, Berlin, 3. Auflage, ISBN: 978-3-540-20656-9 (auch paperback) UB-Semesterhandapparat, IGAM-Bibliothek Gösta H. Liljequist & Konrad Cehak, Allgemeine Meteorologie, Springer, Berlin, 3. Auflage ISBN: 3540415653 (nützliches deutsch-englisches Register) UB-Semesterhandapparat, IGAM-Bibliothek Ludwig Bergmann & Clemens Schaefer, Lehrbuch der Experimentalphysik, Band 7, Erde und Planeten, (Kapitel 3 – Meteorologie, Kapitel 4 – Klimatologie), de Gruyter, Berlin, ISBN: 978-3-11-016837-2 UB-Semesterhandapparat, IGAM-Bibliothek Atmo II 02
Exams Atmo II 03 No, it will be the other way round – you will be forced to answer questions – in my office & IGAM Exam dates and registration via UNIGRAZonline: online.uni-graz.at Picture credit: Gary Larson
Different Aspects of Atmospheric Radiation Atmo II 04 UF
(1) Electromagnetic Waves NASA Physics of the Atmosphere II Atmo II 05
The Electromagnetic Field Basic Properties of the Electromagnetic Field Within the framework of classical electrodynamic theory, it is represented by the vector fields: Electric field E [V/m] Magnetic field B [Vs/m 2 ] = [T] (Tesla) Atmo II 06 To describe the effect of the field on material objects, it is necessary to introduce a second set of vectors: the Electric current density j [A/m 2 ] Electric displacement fieldD [As/m 2 ] Magnetizing field H [A/m] The space and time derivatives of the vectors field are related by Maxwell's equations – we will focus on the differential form.
The Electromagnetic Field The electric field E and the electric displacement field D are related by where ε 0 is the electric constant 8.854 187 817 · 10 -12 AsV -1 m -1 (exact) [NIST Reference: http://physics.nist.gov/cuu/Constants/index.html], and P is the electric polarization – the mean electric dipole moment per volume. Atmo II 07 The magnetic field B and the magnetizing field H are related by where µ 0 is the magnetic constant 4π·10 -7 VsA -1 m -1 (exact), and M is the magnetic polarization – the mean magnetic dipole moment per volume.
Maxwell's Equations in Matter The First Maxwell Equation, also known as Gauss’s Law: relates the divergence of the displacement field to the (scalar) free charge density: Positive electric charges are sources of the displacement field (negative electric charges are sinks). Closed field lines can be caused by induction. Atmo II 08 The Second Maxwell Equation or Gauss’s Law for Magnetism: states that there are no magnetic charges (magnetic monopoles). The magnetic field has no sources or sinks – its field lines can only form closed loops.
Maxwell's Equations in Matter The Third Maxwell Equation, or Faraday’s Law of Induction: describes how a time-varying magnetic field causes an electric field (induction). Atmo II 09 The Fourth Maxwell Equation: shows that magnetic (magnetizing) fields can be caused by electric currents (Ampère’s Law), but also by changing electric (displacement) fields (Maxwell’s Correction – which is very important, since it “allows” for electromagnetic waves – also in vacuum).
The previous formulations are known as Maxwell’s Macroscopic Equations or Maxwell’s Equations in Matter. Under specific conditions the relations on slide 07 can be simplified. The Earth's atmosphere is a linear medium – the induced polarization P is a linear function of the imposed electric field E. The Earth’s atmosphere is also an isotropic medium – P is parallel to E: Atmo II 10 Maxwell's Equations in Gas The electric susceptibility χ e degenerates to a simple scalar (in general it would be a tensor of second rank) and we get: where ε is the permittivity (or dielectric constant in a homogenous medium) and ε r = 1 + χ e is the dimensionless relative permittivity, which depends on the material and is unity for vacuum.
Similar considerations for M and H yield: Atmo II 11 Maxwell's Equations in Gas where χ m is the (scalar) magnetic susceptibility (in general it would be again a tensor of second rank), µ is the permeability and µ r = 1 + χ m is the dimensionless relative permeability (which is also unity in vacuum). The electric current density j is related to the electric field E via the electric conductivity σ [Ω -1 m- 1 ] (a scalar for isotropic media, but in general again a tensor) through the differential form of Ohm’s Law:
The lower atmosphere (troposphere and stratosphere, at least up to ~ 50 km) is a neutral (ρ free = 0), and isotropic medium, and has a negligible electric conductivity (σ = 0) yielding j = 0. Maxwell’s equations can therefore be written as: Atmo II 12 Maxwell's Equations in Neutral Gas
Maxwell's equations relate the vector fields by means of simultaneous differential equations. On elimination we can obtain differential equations, which each of the vectors must separately satisfy. Applying the curl operator on Faraday’s law, interchanging the order of differentiation with respect to space and time (which can be done for a slowly varying medium like the atmosphere is one at frequencies of practical interest) and inserting the fourth Maxwell equation yields: Atmo II 13 Electromagnetic Waves with we get
These partial differential equations are standard wave equations. Considering plane waves, the solutions have the form: Atmo II 14 Electromagnetic Waves and where ν is the frequency (Hz) and λ is the wavelength [m]. Inserting the above solutions into Maxwell’s equations yields: where k is the wave number vector, pointing in the direction of wave propagation. The angular frequency, ω [rad/s] and the angular wave number, k [rad/m], are defined as (with k = |k|):
Atmo II 15 Electromagnetic Waves which shows that the field vectors E and B are perpendicular to each other and that both are perpendicular to k. Electromagnetic waves are thus transverse waves. micro.magnet.fsu.edu wikimedia
Atmo II 16 Electromagnetic Waves Inserting the first equation of slide 14 in to the wave equation using the vector identity: and the orthogonality yields With the definition of the phase velocity: we see that monochromatic electromagnetic waves propagate in a medium with the phase velocity:
Atmo II 17 Electromagnetic Waves And in vacuum we get: C 0 = 299 792 458 m s -1 which is nothing else than the speed of light in vacuum In geometric optics the refractive index of a medium (n) is defined as the ratio of the speed of light in vacuum (c 0 ) to that in the medium (c): which is known as the Maxwell Relation. In the Earth’s atmosphere the relative permeability is almost exactly = 1, thus we get (in a general, frequency-dependent form):
Atmo II 18 Electromagnetic Waves James N. Imamura, Univ. Oregon
Gamma Rays NASA/DOE/Swift Atmo II 20 A gamma-ray blast 12.8 billion light years away, Supernova Cassiopeia A, Cygnus region.
X Rays JAXA/NASA/POLAR Atmo II 21 The Sun and the Earth’s northern Aurora-Oval in X-Rays.
Ultraviolet NASA/SDO Atmo II 22 The Sun in UV and the “Ozone Hole” above Antarctica.
Visible The visible part of the solar spectrum – including Fraunhofer lines (US) National Optical Astronomy Observatory Atmo II 23
Visible Jenny Mottar SOHO/Jeannie Allen Atmo II 24 Color temperatures of stars and spectral signatures on Earth.
Near–Infrared Jeff Carns/NASA Atmo II 25 Vegetation and different Soil types from reflected near–infrared.
Infrared NASA/Jeff Schmaltz MODIS Atmo II 26 Saturn’s strange aurora and forest fires in California.
Microwaves NASA Atmo II 27 Hurricane Katrina. Corresponding Wavelengths: 1m to 1 mm
Radio Waves Michael L. Kaiser, Ian Sutton, Farhad Yusef-Zedeh NASA Atmo II 28
Radio Waves Atmo II 29 In German: LW – Langwelle MW – Mittelwelle KW – Kurzwelle UKW – Ultrakurzwelle Microwaves – 1m to 1 mm Military Radar Nomenclature: L (1 – 2 GHz), S, C, X (8 – 12 GHz), Ku, K (18 – 27 GHz) and Ka bands Physics Hypertextbook
Solar EM Waves Atmo II 30 For processes in the lower atmosphere wavelengths from 0.2 to 100 µm are most important Wiki