Physics 681: Solar Physics and Instrumentation – Lecture 25 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research.

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Physics 681: Solar Physics and Instrumentation – Lecture 25 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research

December 6, 2005Center for Solar-Terrestrial Research The Corona  Coronal temperature is much higher (> 10 6 K) than the temperature of the photosphere  Electron temperature T e ≠ ion temperature T ion  Energy has to be pumped from low to high temperatures  F (Fraunhofer) corona (2–3 solar radii, weakly polarized, scattered photospheric light, zodiacal light)  K (german: Kontinuum) corona (Thomson scattering by free electrons, highly polarized, strong dependence on the position angle, drops steeply with distance from the Sun)  The shape of the corona is closely related to the Sun’s (magnetic) activity cycle  Minimum corona: polar plumes, lines of force resemble a bar magnet  Maximum corona: spherically symmetric, more structured  Condensations, enhancements, helmets, and streamers

December 6, 2005Center for Solar-Terrestrial Research  Emission lines (exceed continuum brightness by a factor of 100)  Forbidden transitions (e.g., Fe X (637 nm) and Fe XIV (530 nm), “coronium”, ΔL = ±1)  Large ionization potential of emission lines  high temperatures, non-LTE, Saha equation does not describe ionization equilibrium  statistical equilibrium (electron collisions, radiative recombination, and dielectronic recombination)  The UV/EUV is dominated by emission lines (e.g., N VII, O VIII, Fe XVIII to Fe XXIII (during flares))  Plasma loops with a width of about 10 6 m  The (isothermal) loops are not in hydrostatic equilibrium  X-ray corona appears bright and highly structure in front of the cool, dark photosphere  Coronal holes

December 6, 2005Center for Solar-Terrestrial Research Maximum and Minimum Corona

December 6, 2005Center for Solar-Terrestrial Research Solar Cycle

December 6, 2005Center for Solar-Terrestrial Research

December 6, 2005Center for Solar-Terrestrial Research

December 6, 2005Center for Solar-Terrestrial Research Solar Wind  Ion tails of comets (small angle <5° between solar radius vector)  Radiation pressure only accounts for dust tail  High-speed (supersonic), continuous, variable flow of ionized matter  Electrons, protons, and α-particles  High-speed streams (about 700 km/s) originate at locations of “open” field lines (coronal holes)  27-day rotation modulation  Transition region outflows with up to 20 km/s in the chromospheric network of coronal holes  Ulysses out-of-ecliptic measurements of the solar wind latitude dependence  First Ionization Potential (FIP) Effect: Elements with a FIP lower than 10 eV are enriched  Ambipolar diffusion (ions and neutral particles are subject to different diffusion velocities and different drift velocities in the magnetic field)

December 6, 2005Center for Solar-Terrestrial Research Comet Hale-Bopp

December 6, 2005Center for Solar-Terrestrial Research

December 6, 2005Center for Solar-Terrestrial Research

December 6, 2005Center for Solar-Terrestrial Research

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