Quiet 3D Sun

Quiet 3D Sun The Sun continues to dwell in its own quiet zone as its level of activity has recently shown almost no signs of rising. But we can still have some fun with it. By combining two images taken 12 hours apart by STEREO (Ahead) on August 7, 2009, we can create a nicely rounded Sun (visible with 3D anaglyph glasses). In those 12 hours, the Sun has rotated around enough to create a sufficiently separated perspective to create 3D. The Sun in extreme UV light shows us a dark coronal hole near the central line from which fast solar wind is streaming. We can also see loops of magnetic field lines arcing out and above a small active region to the lower right.

You can create your own 3D images of the Sun or just about anything else with a digital camera, some software or an online resource, and 3D glasses. Go here to find out how: http://stereo.gsfc.nasa.gov/classroom/3d.shtml

]]> /gallery/item.shtml /img/3dimages/3D195_20090807_thumb.jpg /img/3dimages/preview/3D195_20090807.jpg /img/3dimages/preview/195_20090807.jpg /img/3dimages/print/3D195_20090807.tif 3D Sun Sequence of STEREO images from February 24, 2007 taken by the EUVI telescope in the 195 angstroms wavelength, showing a close up of an active region eruption at the limb.

]]> /gallery/item.shtml /img/3dimages/195_Left_Limb_Ana_thumb.jpg /img/3dimages/preview/195_Left_Limb_Ana.jpg 3D Sun 3D HD resolution animation showing 1)Results from a three dimensional computation of the magnetic field structure of an active region extrapolating the fields from measurements of the magnetic field on the surface of the Sun. This model assumes there are no electrical currents in the corona, leading to a very simple magnetic configuration. From Tahar Amari, Centre de Physique Theorique, Ecole Polytechnique, Paris. 2)Results from a three dimensional computation of the magnetic field structure of an active region extrapolating the fields from measurements of the magnetic field on the surface of the Sun. This model allows currents to flow and assumes force balance, leading to a more complex magnetic configuration for the same surface magnetic fields. From Tahar Amari. 3)Results from a three dimensional computation of the magnetic field structure of the corona extrapolating the fields from measurements of the magnetic field on the surface of the Sun. This models the corona for February 2007. Model from Pete Riley, SAIC, San Diego.

]]> /gallery/item.shtml /img/3dimages/Solar_Model_Ana_thumb.jpg /img/3dimages/preview/Solar_Model_Ana.jpg 3D Sun - May 1, 2007 A solar active region is featured by combining images from the Ahead and Behind spacecraft taken at the same time on May 1, 2007 in the 171 Angstrom wavelength of extreme UV light.

]]> /gallery/item.shtml /img/3dimages/3D_050107sun_thumb.jpg /img/3dimages/preview/3D_050107sun.jpg /img/3dimages/print/3D_050107sun.tif End of 2008 3D Here we offer a 3D sun image from STEREO (Ahead) as a kind of farewell to a very inactive solar year for 2008. The use of 3D is appropriate since STEREO is the first 3D solar mission ever. The north and south polar coronal holes, which appear much darker than the rest of the image, are the most noticeable features of a quiet sun with no active regions at the moment. This image (Dec. 19, 2008) was generated by digitally combining two extreme UV images taken 12 hours apart by the same spacecraft, which were then processed to create the depth and roundedness of 3D. (This is not true 3D - that could only be produced when the two spacecraft were much closer together than they are now.)

]]> /gallery/item.shtml /img/3dimages/3D_20081219_thumb.jpg /img/3dimages/preview/3D_20081219.jpg /img/3dimages/print/3D_20081219.tif Following a 3-D Active Region In true 3-D we follow an active region as it rotates with the Sun for an entire week (April 29 - May 5, 2007). The Sun is being observed in the 195 wavelength of extreme ultraviolet light. Active regions are the sources of most solar storms. This region appears to show two explosions over this time period.

]]> /gallery/item.shtml /img/3dimages/3D_EUVI195_0507_thumb.jpg /img/3dimages/preview/3D_EUVI195_0507.jpg /img/3dimages/print/3D_EUVI195_0507.tif Smaller active regions in 3D This 3D image shows one distinct and a few smaller active regions that appear brighter in the 195 Angstroms wavelength of extreme UV light. It was made by combining two EUVI 195 images from the Ahead STEREO spacecraft about 11 hours apart on April 27, 2008. (Note, it is not true 3D which would need to be taken from two perspectives at the same time. Since the Sun's rotation moves the features and these features do not change that quickly, this 3D effect can be achieved.) The arcing lines extending above the largest active region show the flow of particles along powerful magnetic field lines that rise above the Sun's surface. Active regions, which are seen as sunspots in visible light, are areas of intense magnetic activity that can last days or even months. The darker areas are small coronal holes.

Right and Left Images

]]> /gallery/item.shtml /img/3dimages/3d20080427_thumb.jpg /img/3dimages/preview/3d20080427.jpg /img/3dimages/print/3d20080427.tif 3D Series of Active Regions - June 9, 2007 This is a 3D image showing a row of several active regions that appear brighter in the 195 Angstroms wavelength of extreme UV light. It was made by combining two EUVI 195 images from the Ahead STEREO spacecraft about 12 hours apart on June 9, 2007. (Thus, it is not true 3D where it would be taken from two perspectives at the same time. Since the Sun's rotation moves the features and these features do not change that quickly, this effect can often be achieved.) The arcing lines extending above the largest active region show the flow of particles along powerful magnetic field lines that rise above the Sun's surface. Active regions, which look like sunspots in visible light, are areas of intense magnetic activity that can last days or even months

Right and Left Images

]]> /gallery/item.shtml /img/3dimages/3DAR060907_195_thumb.jpg /img/3dimages/preview/3DAR060907_195.jpg /img/3dimages/print/3DAR060907_195.tif Hot Gas in 3D Above the Sun With the Sun observed at about 2.2 million degrees K in extreme UV light (at 284 Angstroms), one can see concentrations of hot gases as a fuzzy, lighter cloud that extends out in the corona above an active region. This image was created by combining two images from STEREO B (Feb. 24, 2008) taken about 12 hours apart, during which the Sun's rotation provides sufficient perspective to create a nice 3D effect. The material above the active region is changing slowly enough that it is possible to use this technique.

Right and Left Images

]]> /gallery/item.shtml /img/3dimages/3Dgas_thumb.jpg /img/3dimages/preview/3Dgas.jpg /img/3dimages/print/3Dgas.tif May 1, 2007 Full disk view of an eruptive prominence in the EUVI 304 A waveband, May 1, 2007.

Credit: NRL, NASA

]]> /gallery/item.shtml /img/3dimages/304May01_thumb.jpg /img/3dimages/preview/304May01.jpg Eruptive Prominence - May 19, 2007 Close-up view over a one day period of an eruptive prominence (near disk center) in the 304 A waveband (May 19, 2007).

Credit: NRL, NASA

]]> /gallery/item.shtml /img/3dimages/304_May19_thumb.jpg /img/3dimages/preview/304_May19.jpg CME - May 19, 2007 A coronal mass ejection is observed in this close-up of six hours in the 171 A waveband (May 19, 2007).

Credit: NRL, NASA

]]> /gallery/item.shtml /img/3dimages/171May19_thumb.jpg /img/3dimages/preview/171May19.jpg CME - May 16, 2007 A coronal mass ejection erupts from an active region in the 171 A waveband over six hours (May 16, 2007)

Credit: NRL, NASA

]]> /gallery/item.shtml /img/3dimages/171_May16_thumb.jpg /img/3dimages/preview/171_May16.jpg 3D Coronal Hole - October 21, 2007 A 3D coronal hole seen just to the right of the Sun's center in extreme UV light from the STEREO's Behind spacecraft in the 195 Angstrom wavelength. Coronal holes, which appear darker when observed in UV light) are magnetically open areas from which the high-speed solar wind streams into space. This is not a true 3D image (taken from two perspectives at the same time). This image was created by combining two images taken 12 hours apart during which the Sun's rotation provides sufficient perspective to create a nice 3D effect. The coronal hole is changing slowly enough that it is possible to use this technique.

Right and Left Images

]]> /gallery/item.shtml /img/3dimages/102107coronalhole_thumb.jpg /img/3dimages/preview/3D_102107_195.jpg /img/3dimages/print/3D_102107_195.tif May 12-17, 2007 Half disk observation of an active region crossing the Sun using EUVI 195 A data (May 12-17, 2007)