Results 151 to 160 of about 682 (184)

Chromosphere, Corona, and Solar Wind

1989
In the preceding chapters we have learned about convection and rotation, the main causes of solar magnetism. And we have learned about this magnetism itself. We shall now recognize that the Sun¯s magnetic field is the main source of almost all structure and variability which we find in the outermost layers: the chromosphere, the corona, and the solar ...
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4.1.1.4 Solar photosphere and chromosphere

2009
Traditionally, the atmosphere of the Sun has been divided into four layers, starting with the photosphere at the bottom, followed by the chromosphere, the transition region, and the corona as the outermost region. The photosphere is a layer of only a few hundred kilometers thickness in which the temperature drops outwards from around 6000 K at the ...
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Rotation of the solar chromosphere

1978
No abstract ...
Antonucci E., Azzarelli L., Casalini P., Cerri S., Denoth F.   +4 more
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Perovskite solar cells with atomically coherent interlayers on SnO2 electrodes

Nature, 2021
Hanul Min, Do Yoon Lee, Junu Kim
exaly  

Efficient perovskite solar cells via improved carrier management

Nature, 2021
Jason J Yoo, Gabkyung Seo, Matthew R Chua   +2 more
exaly  

Pseudo-halide anion engineering for α-FAPbI3 perovskite solar cells

Nature, 2021
Jaeki Jeong, Jongdeuk Seo, Haizhou Lu
exaly  

The solar chromosphere

1987
R. W. Noyes, E. H. Avrett
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High-Efficiency Perovskite Solar Cells

Chemical Reviews, 2020
Jin Young Kim, Jin-Wook Lee, Hyun Suk Jung   +2 more
exaly  

The Solar Chromosphere

Physics Today, 1974
R. J. Bray, R. E. Loughhead, Robert D. Chapman   +2 more
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Physics of the solar chromosphere

Planetary and Space Science, 1961
Richard N. Thomas, R. Grant Athay, F. R. Scott   +2 more
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