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- W1657321649 abstract "Close to the surface of the sun, the corona (the sun's outer atmosphere) suddenly attains temperatures above 1,000,000 Kelvin (K), much hotter than the 6000K of the photosphere below. In the recent history of solar physics, no single problem has been as stubborn as that of explaining this coronal heating. The corona supplies the energy and momentum that sustains the solar wind; understanding the interdependence between the solar magnetic field and the solar wind patterns may help resolve the puzzle of the coronal heating (1). A flotilla of space solar observatories (including the Yohkoh, SOHO, and TRACE satellites), together with in situ solar-wind measurements from the Ulysses, WIND, ACE, and SOHO satellites, now give us an opportunity to understand these processes. The new TRACE observations reported by Nakariakov et al. on page 862 of this issue (2) illustrate the uses of these new data." @default.
- W1657321649 created "2016-06-24" @default.
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- W1657321649 date "1999-08-06" @default.
- W1657321649 modified "2023-10-16" @default.
- W1657321649 title "SOLAR PHYSICS:How the Sun's Corona Gets Hot" @default.
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- W1657321649 doi "https://doi.org/10.1126/science.285.5429.849" @default.
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