Matches in DBpedia 2015-10 for { ?s ?p "The chromosphere (literally, "sphere of color") is the second of the three main layers in the Sun's atmosphere and is roughly 2,000 kilometers deep. It sits just above the photosphere and just below the solar transition region.The density of the chromosphere is very low, it being only 10−4 times that of the photosphere, the layer just below it, and 10−8 times that of the atmosphere of Earth. This makes the chromosphere normally invisible and it can be seen only during a total eclipse, where its reddish color is revealed. The color hues are anywhere between pink and red.However, without special equipment, the chromosphere cannot normally be seen due to the overwhelming brightness of the photosphere.The density of the chromosphere decreases with distance from the center of the sun. This decreases logarithmically from 1017 particles per cubic centimeter, or approximately 6996200000000000000♠2×10−4 kg/m3 to under 6989160000000000000♠1.6×10−11 kg/m3 at the outer boundary. The temperature begins to decrease from the inner boundary of about 6,000 K to a minimum of approximately 3,800 K, before increasing to upwards of 35,000 K at the outer boundary with the transition layer of the corona. Figure 1 shows the trends which density and temperature follow through the chromosphere.Chromospheres have been observed also for stars different from the Sun."@en }
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- Chromosphere abstract "The chromosphere (literally, "sphere of color") is the second of the three main layers in the Sun's atmosphere and is roughly 2,000 kilometers deep. It sits just above the photosphere and just below the solar transition region.The density of the chromosphere is very low, it being only 10−4 times that of the photosphere, the layer just below it, and 10−8 times that of the atmosphere of Earth. This makes the chromosphere normally invisible and it can be seen only during a total eclipse, where its reddish color is revealed. The color hues are anywhere between pink and red.However, without special equipment, the chromosphere cannot normally be seen due to the overwhelming brightness of the photosphere.The density of the chromosphere decreases with distance from the center of the sun. This decreases logarithmically from 1017 particles per cubic centimeter, or approximately 6996200000000000000♠2×10−4 kg/m3 to under 6989160000000000000♠1.6×10−11 kg/m3 at the outer boundary. The temperature begins to decrease from the inner boundary of about 6,000 K to a minimum of approximately 3,800 K, before increasing to upwards of 35,000 K at the outer boundary with the transition layer of the corona. Figure 1 shows the trends which density and temperature follow through the chromosphere.Chromospheres have been observed also for stars different from the Sun.".