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Energy, Radio, and Eclipse: Brushing up on that Astrophysics to prep for this Solar Eclipse. #IllhaveaCoronaWithLimePlease #ScienceJokes FIGURE 11.17 Sps in the chomphee of the Sun in addtion, small s the upper left gaudrant of the inuge, and brighter arcias knowa as plage regions are aso vi otsen stions were made asing the Her enssion ine Features as small as 130km are 62Slie 4x I0 K Figure !I19 shows images of the Sun at various wa RE 1I1.18 Logarithmie plots of the temperature structure (solid line) and mass de line) of the upper atmosphere of the Sun. The altitudes observed at various wa icted. Figure adapted from Avrett. in Encyclopedia of Astronomy and Astrop Murdin (ed.), Institute of Physics Publishing. Bristol, 2001 page 2480.J e without a well dehined outer boundary and has an energy output that is nearly lo* times less intense than that of the photosphere. The number density of urticles at the base of the corona is typicaly Ios partieles mwhereas in the vicinity of by the high thermal velocities of the electrons . The Fcorona (for Fr evel in Earth's atmosphere) Because the densizy of the corena is so low, it is essen- nsparent to most electromagnetic radiation (except long radio wavelengths) and cal thermodynamic equilibrium (LTE). For gases that are not in LTE, a unique is not stricty definable (see Section 92). However, the temperatures obtained thermal motions, ionization levels, and radio emissions do give reasonably s For instance, the presence of Fe XIV lines indicates temperatures in K. as do line widths produced by thermal Doppler broadening ionized atoms located throughout the corona; the E corona overlaps the coronas. Since the temperatures are extremely high in the corona, the in the Saha equation encourages ionization because thermal e to ionization potentials. The very low number densi since the chance of recombination is greatly red. light emission that results from photospheric radiation scattered Science jokes
Energy, Radio, and Eclipse: Brushing up on that Astrophysics to prep for
 this Solar Eclipse.
 #IllhaveaCoronaWithLimePlease
 #ScienceJokes
 FIGURE 11.17 Sps in the chomphee of the Sun in addtion, small s
 the upper left gaudrant of the inuge, and brighter arcias knowa as plage regions are aso vi
 otsen stions were made asing the Her enssion ine Features as small as 130km are
 62Slie 4x I0 K Figure !I19 shows images of the Sun at various wa
 RE 1I1.18 Logarithmie plots of the temperature structure (solid line) and mass de
 line) of the upper atmosphere of the Sun. The altitudes observed at various wa
 icted. Figure adapted from Avrett. in Encyclopedia of Astronomy and Astrop
 Murdin (ed.), Institute of Physics Publishing. Bristol, 2001 page 2480.J
 e without a well dehined outer boundary and has an energy output
 that is nearly lo* times less intense than that of the photosphere. The number density of
 urticles at the base of the corona is typicaly Ios partieles mwhereas in the vicinity of
 by the high thermal velocities of the electrons
 . The Fcorona (for Fr
 evel in Earth's atmosphere) Because the densizy of the corena is so low, it is essen-
 nsparent to most electromagnetic radiation (except long radio wavelengths) and
 cal thermodynamic equilibrium (LTE). For gases that are not in LTE, a unique
 is not stricty definable (see Section 92). However, the temperatures obtained
 thermal motions, ionization levels, and radio emissions do give reasonably
 s For instance, the presence of Fe XIV lines indicates temperatures in
 K. as do line widths produced by thermal Doppler broadening
 ionized atoms located throughout the corona; the E corona overlaps the
 coronas. Since the temperatures are extremely high in the corona, the
 in the Saha equation encourages ionization because thermal e
 to ionization potentials. The very low number densi
 since the chance of recombination is greatly red.
 light emission that results from photospheric radiation scattered
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