Surya Namaskar
om Hram mitraya namah
A sweeping prominence, a huge cloud of relatively cool dense plasma is seen suspended in the Sun's hot, thin corona. At times, promineces can erupt, escaping the Sun's atmosphere. Emission in this spectral line shows the upper chromosphere at a temperature of about 60,000 degrees K (over 100,000 degrees F). Every feature in the image traces magnetic field structure. The hottest areas appear almost white, while the darker red areas indicate cooler temperatures. (Courtesy of SOHO/EIT consortium)
om Hrim ravaye namah
This TRACE 171Е-wavelength image from November 11, 2006 shows a sizeable active region at the east limb of the Sun (rotated clockwise 90 degrees so north is to the right) just as it rotates onto Earth-facing hemisphere. Notice the low-lying dark structures of filaments at the leading edge of the region, some "levitating" dark material on the right-hand side of the region, and the small ephemeral region towards the lower right. (NASA/TRACE)
om Hrum suryaya namah
Detailed closeup of magnetic structures on the Sun's surface, seen in the H-alpha wavelength on August 22, 2003. (Swedish 1-m Solar Telescope (SST) operated by the Royal Swedish Academy of Sciences, Oddbjorn Engvold, Jun Elin Wiik, Luc Rouppe van der Voort)
om Hraim bhanave namah
Hinode (formerly known as Solar-B) successfully captured a massive solar flare on 13 December 2006. It was one of the largest flares occurring in that period of solar activity minimum. (JAXA/NASA/PPARC)
om hraum khagaya namah
The Sun, observed on May 22, 2008. With the Sun persisting in a near-minimal state of activity, only a few small regions of some activity are seen on the disk. The cell-like appearance is formed by the multitude of small clusters of magnetic flux that are collected in the downflow regions of the supergranular network of convective motions. (NASA/TRACE)
om Hrah pusne namah
Image of an active solar region taken on July 24, 2002 near the eastern limb of the Sun. The image highlights the three-dimensional nature of the photosphere when seen at these large angles. The structures in the dark sunspots in the upper central area of the image show distinct elevation above the dark "floor" of the sunspot. The height of the structures has been estimated by Dr. Bruce Lites of the High Altitude Observatory to be between 200 and 450 km. The smallest resolvable features in the image are about 70 km in size. There are also numerous bright "faculae" visible on the edges of granules that face towards the observer. (Prof. Goran Scharmer/Dr. Mats G. Lцfdahl/Institute for Solar Physics of the Royal Swedish Academy of Sciences)
om Hram hiranyagarbhaya namah
A sweeping prominence, a huge cloud of relatively cool dense plasma is seen suspended in the Sun's hot, thin corona. At times, promineces can erupt, escaping the Sun's atmosphere. Emission in this spectral line shows the upper chromosphere at a temperature of about 60,000 degrees K (over 100,000 degrees F). Every feature in the image traces magnetic field structure. The hottest areas appear almost white, while the darker red areas indicate cooler temperatures. (Courtesy of SOHO/EIT consortium)
om Hrim maricaye namah
TRACE 171Е image of an erupting solar filament above Active Region 9077 on July 19, 2000. Filaments are concentrated bundles of magnetic field filled with relatively cool gas, suspended in the solar corona. When they become unstable, they can erupt, triggering coronal mass ejections and solar flares. The dark material here is relatively cool, while the bright material is hotter than a million degrees. As this hot material cools, it condenses and drains down the lines of magnetic field in the corona much like beads moving along a wire, a process some scientists refer to as "coronal rain." (Caption courtesy Dan Seaton, Photo courtesy Dick Shine, NASA/TRACE)
om Hrum adityaya namah
A view of an irregular-shaped sunspot and granules on the Sun's surface, seen on August 22, 2003. (Swedish 1-m Solar Telescope (SST) operated by the Royal Swedish Academy of Sciences, Oddbjorn Engvold, Jun Elin Wiik, Luc Rouppe van der Voort, Oslo)
om Hraim savitre namah
The image shows the corona for a moderately active Sun, with some (red) hot active regions in both hemispheres, surrounded by the (blue/green) cooler plasma of the quiet-Sun corona. Notice also the north polar-crown filament, the trans-equatorial loops, and the coronal hole in the south-east (lower-right) corner of the image and the smaller one over the north pole. This image shows the solar corona in a false-color, 3-layer composite: the blue, green, and red channels show the 171Е, 195Е, and 284Е wavelengths, respectively (most sensitive to emission from 1, 1.5, and 2 million degree gases). (TRACE Project, Stanford-Lockheed Institute for Space Research, NASA)
om Hraum arkaya namah
This LASCO C2 image, taken 8 January 2002, shows a widely spreading coronal mass ejection (CME) as it blasts more than a billion tons of matter out into space at millions of kilometers per hour. The C2 image was turned 90 degrees so that the blast seems to be pointing down. An EIT 304 Angstrom image from a different day was enlarged and superimposed on the C2 image so that it filled the occulting disk for effect (Courtesy of SOHO/LASCO consortium)
om Hrah bhaskaraya namah
A transit of the Moon across the face of the Sun on February 25, 2007 - but not seen from Earth. This sight was visible only from the STEREO-B spacecraft in its orbit about the sun, trailing behind the Earth. NASA's STEREO mission consists of two spacecraft launched in October, 2006 to study solar storms. STEREO-B is currently about 1 million miles from the Earth, 4.4 times farther away from the Moon than we are on Earth. As the result, the Moon appears 4.4 times smaller than what we are used to. (NASA/STEREO)
Фотографии взяты оттуда:
http://www.boston.com/bigpicture/2008/10/the_sun.html
A sweeping prominence, a huge cloud of relatively cool dense plasma is seen suspended in the Sun's hot, thin corona. At times, promineces can erupt, escaping the Sun's atmosphere. Emission in this spectral line shows the upper chromosphere at a temperature of about 60,000 degrees K (over 100,000 degrees F). Every feature in the image traces magnetic field structure. The hottest areas appear almost white, while the darker red areas indicate cooler temperatures. (Courtesy of SOHO/EIT consortium)
om Hrim ravaye namah
This TRACE 171Е-wavelength image from November 11, 2006 shows a sizeable active region at the east limb of the Sun (rotated clockwise 90 degrees so north is to the right) just as it rotates onto Earth-facing hemisphere. Notice the low-lying dark structures of filaments at the leading edge of the region, some "levitating" dark material on the right-hand side of the region, and the small ephemeral region towards the lower right. (NASA/TRACE)
om Hrum suryaya namah
Detailed closeup of magnetic structures on the Sun's surface, seen in the H-alpha wavelength on August 22, 2003. (Swedish 1-m Solar Telescope (SST) operated by the Royal Swedish Academy of Sciences, Oddbjorn Engvold, Jun Elin Wiik, Luc Rouppe van der Voort)
om Hraim bhanave namah
Hinode (formerly known as Solar-B) successfully captured a massive solar flare on 13 December 2006. It was one of the largest flares occurring in that period of solar activity minimum. (JAXA/NASA/PPARC)
om hraum khagaya namah
The Sun, observed on May 22, 2008. With the Sun persisting in a near-minimal state of activity, only a few small regions of some activity are seen on the disk. The cell-like appearance is formed by the multitude of small clusters of magnetic flux that are collected in the downflow regions of the supergranular network of convective motions. (NASA/TRACE)
om Hrah pusne namah
Image of an active solar region taken on July 24, 2002 near the eastern limb of the Sun. The image highlights the three-dimensional nature of the photosphere when seen at these large angles. The structures in the dark sunspots in the upper central area of the image show distinct elevation above the dark "floor" of the sunspot. The height of the structures has been estimated by Dr. Bruce Lites of the High Altitude Observatory to be between 200 and 450 km. The smallest resolvable features in the image are about 70 km in size. There are also numerous bright "faculae" visible on the edges of granules that face towards the observer. (Prof. Goran Scharmer/Dr. Mats G. Lцfdahl/Institute for Solar Physics of the Royal Swedish Academy of Sciences)
om Hram hiranyagarbhaya namah
A sweeping prominence, a huge cloud of relatively cool dense plasma is seen suspended in the Sun's hot, thin corona. At times, promineces can erupt, escaping the Sun's atmosphere. Emission in this spectral line shows the upper chromosphere at a temperature of about 60,000 degrees K (over 100,000 degrees F). Every feature in the image traces magnetic field structure. The hottest areas appear almost white, while the darker red areas indicate cooler temperatures. (Courtesy of SOHO/EIT consortium)
om Hrim maricaye namah
TRACE 171Е image of an erupting solar filament above Active Region 9077 on July 19, 2000. Filaments are concentrated bundles of magnetic field filled with relatively cool gas, suspended in the solar corona. When they become unstable, they can erupt, triggering coronal mass ejections and solar flares. The dark material here is relatively cool, while the bright material is hotter than a million degrees. As this hot material cools, it condenses and drains down the lines of magnetic field in the corona much like beads moving along a wire, a process some scientists refer to as "coronal rain." (Caption courtesy Dan Seaton, Photo courtesy Dick Shine, NASA/TRACE)
om Hrum adityaya namah
A view of an irregular-shaped sunspot and granules on the Sun's surface, seen on August 22, 2003. (Swedish 1-m Solar Telescope (SST) operated by the Royal Swedish Academy of Sciences, Oddbjorn Engvold, Jun Elin Wiik, Luc Rouppe van der Voort, Oslo)
om Hraim savitre namah
The image shows the corona for a moderately active Sun, with some (red) hot active regions in both hemispheres, surrounded by the (blue/green) cooler plasma of the quiet-Sun corona. Notice also the north polar-crown filament, the trans-equatorial loops, and the coronal hole in the south-east (lower-right) corner of the image and the smaller one over the north pole. This image shows the solar corona in a false-color, 3-layer composite: the blue, green, and red channels show the 171Е, 195Е, and 284Е wavelengths, respectively (most sensitive to emission from 1, 1.5, and 2 million degree gases). (TRACE Project, Stanford-Lockheed Institute for Space Research, NASA)
om Hraum arkaya namah
This LASCO C2 image, taken 8 January 2002, shows a widely spreading coronal mass ejection (CME) as it blasts more than a billion tons of matter out into space at millions of kilometers per hour. The C2 image was turned 90 degrees so that the blast seems to be pointing down. An EIT 304 Angstrom image from a different day was enlarged and superimposed on the C2 image so that it filled the occulting disk for effect (Courtesy of SOHO/LASCO consortium)
om Hrah bhaskaraya namah
A transit of the Moon across the face of the Sun on February 25, 2007 - but not seen from Earth. This sight was visible only from the STEREO-B spacecraft in its orbit about the sun, trailing behind the Earth. NASA's STEREO mission consists of two spacecraft launched in October, 2006 to study solar storms. STEREO-B is currently about 1 million miles from the Earth, 4.4 times farther away from the Moon than we are on Earth. As the result, the Moon appears 4.4 times smaller than what we are used to. (NASA/STEREO)
Фотографии взяты оттуда:
http://www.boston.com/bigpicture/2008/10/the_sun.html