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  2. Stellar corona - Wikipedia

    en.wikipedia.org/wiki/Stellar_corona

    The Sun's corona is much hotter (by a factor from 150 to 450) than the visible surface of the Sun: the corona's temperature is 1 to 3 million kelvin compared to the photosphere's average temperature – around 5 800 kelvin. The corona is far less dense than the photosphere, and produces about one-millionth as much visible light.

  3. Corona (optical phenomenon) - Wikipedia

    en.wikipedia.org/wiki/Corona_(optical_phenomenon)

    Lunar corona A solar corona up Beinn Mhòr (South Uist). In meteorology, a corona (plural coronae) is an optical phenomenon produced by the diffraction of sunlight or moonlight (or, occasionally, bright starlight or planetlight) [1] by individual small water droplets and sometimes tiny ice crystals of a cloud or on a foggy glass surface.

  4. Stellar atmosphere - Wikipedia

    en.wikipedia.org/wiki/Stellar_atmosphere

    During a total solar eclipse, the photosphere of the Sun is obscured, revealing its atmosphere's other layers. [1] Observed during eclipse, the Sun's chromosphere appears (briefly) as a thin pinkish arc, [11] and its corona is seen as a tufted halo. The same phenomenon in eclipsing binaries can make the chromosphere of giant stars visible. [12]

  5. Photosphere - Wikipedia

    en.wikipedia.org/wiki/Photosphere

    The Sun is composed primarily of the chemical elements hydrogen and helium; they account for 74.9% and 23.8%, respectively, of the mass of the Sun in the photosphere.All heavier elements, colloquially called metals in stellar astronomy, account for less than 2% of the mass, with oxygen (roughly 1% of the Sun's mass), carbon (0.3%), neon (0.2%), and iron (0.2%) being the most abundant.

  6. Helmet streamer - Wikipedia

    en.wikipedia.org/wiki/Helmet_streamer

    The white-light emissions of helmet streamers is due to the high electron density of the confined plasma relative to the surrounding corona. Light from the photosphere is Thomson scattered off of these electrons with the intensity of scattered light depending on the number of electrons along the observer's line of sight. [5]

  7. Coronal loop - Wikipedia

    en.wikipedia.org/wiki/Coronal_loop

    Coronal loops begin and end at two footpoints on the photosphere and project into the transition region and lower corona. They typically form and dissipate over periods of seconds to days [ 1 ] and may span anywhere from 1 to 1,000 megametres (621 to 621,000 mi) in length.

  8. Radiative zone - Wikipedia

    en.wikipedia.org/wiki/Radiative_zone

    A radiative zone is a layer of a star's interior where energy is primarily transported toward the exterior by means of radiative diffusion and thermal conduction, rather than by convection. [1]

  9. Solar phenomena - Wikipedia

    en.wikipedia.org/wiki/Solar_phenomena

    The slow solar wind has a velocity of about 400 kilometres per second (250 mi/s), a temperature of 2 × 10 5 K and a composition that is a close match to the corona. The fast solar wind has a typical velocity of 750 km/s, a temperature of 8 × 10 5 K and nearly matches the photosphere's.