SOLAR ULTRAVIOLET MEASUREMENTS OF EMITTED RADIATION

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Spectral Atlas

Flare Lines

Figures

• Figure 1. (740 KB GIF)
  The north-east quadrant of the Sun in the light of the C III (977 Å) resonance line on 28-30 Jan 1996. The line is formed at a temperature of 70 000 K and is representative for the lower transition region. It is one of the brightest lines in the SUMER wavelength range providing high-contrast images of the chromospheric network structure (Space Sci. Rev. 93, 411, 2000), the EUV spicules (A&A 360, 351, 2000) and prominences (ASP Conf. Ser. 118, 259, 1997).
• Figure 2. (818 KB GIF)
  The north-east quadrant of the Sun in the light of thr Ne VIII (770 Å) resonance line on 02 Feb 1996. The line is formed at a temperature of 630 000 K and is representative for the lower corona. The quiet-Sun chromospheric network structure is still visible, but the network disappears in the polar coronal hole (A&A 334, 685, 1998). A prominence in absorption by the H I Lyman continuum is an interesting feature in this image (ASP Conf. Ser. 118, 259, 1997).
• Figure 3. (737 KB GIF)
  The south-east quadrant of the Sun in the light of the He I (584 Å) resonance line on 02-04 Mar 1996. The line is formed at a temperature of 30 000 K and is representative for the upper chromosphere. The chromospheric network, effects of the polar coronal hole and spicules can be seen in this image. A prominence, which is optically thick in this line, extends to a height of 70 000 km (Sol. Phys. 170, 75, 1997).
• Figure 4. (1000 KB GIF)
  The east limb of the Sun in the light of the S VI (944 Å) resonance line, which is blended with Si VIII, on 08 May 1996. The lines are formed at temperatures of 200 000 K and 850 000 K, respectively. The image is thus representative for the upper transition region and lower corona. A small active region is visible near the east limb.
• Figure 5. (256 KB GIF)
  The solar disk center (270" x 300") in the light of the O VI (1031 Å) resonance line on 30 Jan 1996. The line is formed at a temperature of 300 000 K. The image shows that the transition region consists of loop-like structures that straddle the network boundaries (Adv. Space Res. 25, 1723, 2000).

Movies

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MPEG movies are viewed best as a loop with 0.5 to 1.0 s per frame.

• Movie 1. (431 KB anim.GIF) (68 KB MPEG)
  Up and down in the northern polar coronal hole of the Sun on 27 Jan 1996. The sequence shows C I (1253 Å), the red wing of H I Ly a (1218 Å), S II (1253 Å), N V (1242 Å), and Mg X (609 Å), representing the lower, middle and upper chromosphere, the transition region, and the corona. All lines are observed simultaneously during a single raster scan. The chromospheric network and the sharp solar limb can be seen in the cool lines (C I, H I and Si II), spicules are prominent in N V, and plumes with inter-plume lanes are delineated by Mg X.
• Movie 2. (2767 KB anim.GIF) (396 KB MPEG)
  Up and down in the south-east polar coronal hole boundary of the Sun on 11 Aug 1996. The sequence shows C I (1249 Å), Si II (1250 Å), S II (1250 Å), N V (1238 Å), O V (629 Å), Mg X (624 Å), and Fe XII (1242 Å). The chromospheric network seen in the cooler lines of this sequence (C I, Si II, N V, and O V) is very similar inside and outside of the coronal hole on the solar disk (Astrophys. Space Sci. 264, 43, 1999). However, the limb features (spicules etc.) are increasing with higher formation temperatures. Mg X depicts plumes and inter-plume lanes above the coronal hole, whereas this region is void of emission in Fe XII, demonstrating that the electron temperature above the hole is lower than in the quiet-Sun region towards the north.
• Movie 3. (5381 KB anim.GIF) (758 KB MPEG)
  Up and down in an equatorial coronal hole of the Sun on 30 Aug 1996. The sequence shows the same lines as in Movie 2. The coronal hole can be identified in Mg X and Fe XII in the western portion of the image. The feature east of it is a filament channel.
• Movie 4. (2084 KB anim.GIF) (287 KB MPEG)
  Up and down in the north-west polar coronal hole boundary of the Sun on 21 Sep 1996. The sequence shows continuum (1543 Å), Si II (1533 Å), C IV (1548 Å), and Ne VIII (770 Å). The polar coronal hole is clearly outlined by the Ne VIII line (Science 283, 810, 1999).
• Movie 5. (859 KB anim.GIF) (406 KB MPEG)
  Full disk of the Sun on 04-05 Feb 1996, alternating in continuum (1549 Å) and C IV (1548 Å). Note the similarities of the network between the images and the differences as far as the prominences and the spicules are concerned.
• Movie 6. (797 KB anim.GIF) (356 KB MPEG)
  Full disk of the Sun on 02-04 Mar 1996, alternating in continuum (1169 Å) and He I (584 Å).
• Movie 7. (1125 KB anim.GIF) (344 KB MPEG)
  Full disk of the Sun on 12 May 1996, alternating in H I Ly e (937 Å), S VI (933 Å), and S VI (944 Å) blended with Si VIII. An isolated active region can be seen near the center of the disk. Note the changing length of the plasma structures with the formation temperature of the emission lines and the absence of any significant limb brightening of the H I line, which is emitted from optically thick plasmas.
• Movie 8. (1161 KB anim.GIF) (681 KB MPEG)
  Full disk of the Sun on 07 Jun 1996, alternating in C IV (1548 Å), O IV (787 Å), and Ne VIII (Å). Note the changing structure of the chromospheric network inside and outside of the polar coronal holes.