In the center of the line, we obtain the image of the upper layer of hydrogen, characterized by brilliant areas and dark filaments. Granulation and solar vortices are much less visible in this case. Even the small sunspots seem erased.

At the sun limb, prominences are quite visible but the narrow band-width can limit their visibility if they have fast radial motions (important spectral shift). It is with this wavelength that we can better observe the solar flares.

We also can, by masking the solar disc, highlight prominences and obtain an image looking like what a small coronagraph (prominence attachment) would give.

• Ionised calcium K line (393.37nm)

This line is really very wide and complex, showing a profile in absorption and in emission. It results from various levels of the chromosphère. The emissive part of this line reflects the temperature of the matter and creates brilliant regions, called "plages" or faculae , which we notice particularly around sunspots. We also observe spotless faculae, which can be the place of appearing of new spots, or mark the place of disappeared spots. Other brilliant points mark the outlines of the cells of the supergranulation and form the chromospheric network. The line H (396.85nm), also induced by ionized calcium, gives the same images as her twin sister K.

As for the line of hydrogen, the deviation from the axis gives the image of the low layer (500km), close to the photosphere, with quite visible spots and faculae areas which appear clearly. We speak here about the component K1 of the K line.

Near the core of the line (0,02 nm), the chromospheric network appears clearly and facula areas brilliant (own emission) with regard to the rest of the very dark disc. It is the component known as K2.

The core of the line (component K3) is characterized by a strong absorption revealing dark filaments and, as in the case of the H alpha line, prominences in emission at the sun limb. In fact, the images obtained with a band-width of 0,05 nm can not give a pure image K3. We rather speak in this case about images K2,3. There is a less good visibility of filaments and prominences.

• Hydrogen Hb, Hg and Hd lines (resp. 486.13, 434.05 et 410.18nm )

Images obtained in these three lines also show filaments and prominences but with a lower contrast. They also reveal broad dark areas around the active areas and a dark chromospheric network. The contrast of the details decreases much with H-delta because the width of the line is rather narrow.

• Helium "D3" line (587.56nm)

This spectral line is at the origin of the discovery of the element Helium the name of which is diverted from Helios. It is easily visible in emission in the prominences, appears on the disc only in particular conditions. One can locate it in aborption in the dense filaments and in the "plages". It can also appear in emission in the flares when the temperature borders 20000 K and if the density is sufficient.

• IRT, ionized calcium infra-red triplet (854nm)

The CCD sensor allows generally to investigate the spectrum a little farther in the red or the purple than allows human eye. There are in the infrared 3 lines of absorption induced by ionized calcium. Here, a comparison between the purple and infrared lines shows that the same chromosphériques structures are visible with a similar aspect.

• Images with other spectral lines

Some attempts were tempted with other lines (iron 404,6 nm, magnesium 518,4 nm) which, although intense, are however too much fine for the band-width of this spectroheliograph. Images are close to what we can observe in white light, with a clear reinforcement of facula areas. The image opposite is taken with a line of iron (404,6 nm)