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Bilder zu 'Prominenze' gefunden, 50

SOLAR PROMINENCES
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Solar prominences
Solar prominences.
Solar prominences
Solar prominences in 1871 and 1872
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Solar prominences, Plate 10, 1872
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Solar prominences, Plate 9, 1872
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Sunspots and prominences in 1973. Image from Skylab's solar telescope. NASA photograph.
Solar prominences, Plate 8, 1872
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Solar Spectrum and Spectrum of the Prominences, during a total Eclipse
Solar corona and prominences
The inner corona of the sun and pink prominences during a total solar eclipse, 1 August 2008 (photo)
Astronomy, solar protuberances, prominences and flares, observed in Palermo, Sicily,  in 1871-1872. 1877 (engraving)
Le Soleil vu by STEREO on 16/08/2008 - Solar activity seen by STEREO spacecraft on august 16 2008 - Protuberances observed by one of the STEREO satellites on 16 August 2008. A STEREO spacecraft observed several solar prominences rise and gyrate above the Sun over a two - day period (Aug. 15 - 16, 2008), with the largest one arcing a distance at least equal to 30 Earth diameters. They are spread out with one in each quadrant. Magnetic forces control solar prominences that rise above the Sun's surface. The prominences were seen in the 304 Angstroms wavelength of ultraviolet light. The material observed is actually ionized Helium at about 60,000 degrees. Prominences are relatively cool clouds of gas suspended above the Sun and controlled by magnetic forces. They can last from hours to months, but most usually remain for just a few days
Total Eclipse of Sun in Zambia. 21/06/2001 - Total Solar Eclipse of 2001 june 21 - Solar protuberances observed during the total eclipse of Sun of 21 June 2001. Solar prominences seen during the totality
Le Soleil vu by STEREO 29/09/2008 - Solar activity seen by STEREO spacecraft on september 29 2008 - Protuberances observed by one of the STEREO satellites on September 29, 2008. The STEREO spacecraft observed this visually stunning prominence eruption on Sept. 29, 2008, in the 304 angstrom wavelength of extreme UV light. Prominences are relatively cool clouds of gas suspended above the sun and controlled by magnetic forces. The prominence rose and cascaded to the right over several hours, appearing something like a flag unfurling, as it broke apart and headed into space. The prominence is composed of ionized Helium that is about 60,000 degrees Kelvin
Total solar eclipse - Turkey 29 March 2006 - Total solar eclipse - Turkey - March 29, 2006 - Total solar eclipse seen on 29 - 03 - 2006 in Turkey. This montage presents the different phases surrounding the third contact: - the top of the protuberances appear - then the chromosphere (in red) in whole - finally the photosphere (in dazzling white) appears in favour of the depressions of the limbe - then the phenomene amplifies before a real solar crescent reappears. This composite shows the different phases surrounding the third contact: - the prominences summit appear - then the chromosphere (in red) - finally the photosphere (the white part of the Sun) appear through the limb's depression - and then the phenomenon increases before the reappearance of a Sun crescent
Total eclipse of the Sun, Turkey, 29 March 2006
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Sir Norman Lockyer, English astronomer, c 1910
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Angelo Secchi, Italian astronomer, c 1860s
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Totally eclipsed sun, early morning 24 October 1995
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The Sun with handle-shaped prominence, 14 September 1999
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Kew photoheliograph, 1857
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Spectroscope with seven prism train, 1868
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Kew photoheliograph, 1857
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Kew photoheliograph, 1857
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Kew photoheliograph, 1857
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Equatorial telescope, Palermo, Sicily, Italy, 1865
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Drawings of solar prominence on the Sun, Rome, Italy, 1869
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Photograph of the Sun, Richmond, London, 8 December 1861
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Kew photoheliograph, 1857
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Spectroscope with seven prism train, 1868
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X-ray picture of the sun, taken from Skylab, 1973
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The Sun, photographed at X-ray wavelengths by Skylab, 1973
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