Soles de primavera

He aquí tres imágenes tomadas con el Coronado Solarmax de 40mm con filtro Ha, y la Canon T2i, tomas únicas a 400 iso 1/250seg. 
Luego siguen las tomas logradas por el SOHO en tres registros del espectro electromagnético.

SOHO: solar and heliosferic observatory
http://sohowww.estec.esa.nl/home.html

Extremo ultravioleta, imagen del SOHO.
Imágenes de la atmósfera solar a longitudes de onda extremas que muestran el material solar a diversas temperaturas. Esta imagen a 304 Angstrom muestra el material brillante de 60.000 a 80.000º K. 
EIT (Extreme ultraviolet Imaging Telescope) images the solar atmosphere at several wavelengths, and therefore, shows solar material at different temperatures. In the images taken at 304 Angstrom the bright material is at 60,000 to 80,000 degrees Kelvin. In those taken at 171 Angstrom, at 1 million degrees. 195 Angstrom images correspond to about 1.5 million Kelvin, 284 Angstrom to 2 million degrees. The hotter the temperature, the higher you look in the solar atmosphere.

Magnetograma del SOHO
La imagen muestra el campo magnético sobre la fotosfera solar. En negro y blanco los polos opuestos.
The MDI (Michelson Doppler Imager) images shown here are taken in the continuum near the Ni I 6768 Angstrom line. The most prominent features are the sunspots. This is very much how the Sun looks like in the visible range of the spectrum (for example, looking at it using special 'eclipse' glasses: Remember, do not ever look directly at the Sun!). The magnetogram image shows the magnetic field in the solar photosphere, with black and white indicating opposite polarities.

Coronógrafo del SOHO
Imagen de la corona solar, lograda a raíz de bloquear la emisión directa de luz solar mediante un eclipse artificial óptico producido dentro del equipo.
LASCO (Large Angle Spectrometric Coronagraph) is able to take images of the solar corona by blocking the light coming directly from the Sun with an occulter disk, creating an artificial eclipse within the instrument itself. The position of the solar disk is indicated in the images by the white circle. The most prominent feature of the corona are usually the coronal streamers, those nearly radial bands that can be seen both in C2 and C3. Occasionally, a coronal mass ejection can be seen being expelled away from the Sun and crossing the fields of view of both coronagraphs. The shadow crossing from the lower left corner to the center of the image is the support for the occulter disk.

http://sohowww.estec.esa.nl/data/realtime/image-description.html