The Domeless Solar Telescope (DST)
The Sun is the only star for which we can observe fine details on
its surface and investigate the associated activity. Once the underlying
physics has been established, it can be applied to the understanding
of other activities in the Universe.
The Domeless Solar Telescope
(DST) was designed to acquire solar surface images at the highest
spatial resolution. Since its establishment in
1979, the DST has contributed to the great scientific progress in recent years in the
understanding of the mechanisms which cause solar explosive events, and other phenomena in
space plasma physics.
The DST Lyot filter has a very narrow passband of 0.25
angstroms, and provides arbitrary wavelength tuning. With
this filter, we can see the three-dimensional velocity structure of
the solar atomosphere.
|Operating the DST
The file sizes are somewhat large, so it may take some time to download them.
- Automatic guide to make the telescope point toward
the Sun. [QuickTime (4.5MB)], [GIF animation (4.9MB)]
- To open the entrance lid and let in the Sun's light. [QuickTime (7.2 MB)], [GIF animation (7.4MB)]
- At the start of daily operations, the observer searches
for an object suitable for the scientific purpose of his research, such as a prominence, some emerging flux, spots, etc.
When the object comes
into the field of view, the observer can look at its 3D structure by changing
the observed wavelength.
[QuickTime(14 MB)], [GIF Animation(32 MB)]
|Type||Domeless Tower Vacuum Telescope|
|Type||Gregorian type reflector telescope|
|Effective apature||600 mm|
|Focal length of objective mirror||3,150mm|
|Total focal length||32.19m|
|Total F ratio||F/53.7|
|The diameter of the solar image||299.95 mm = 1922 arcsec|
(1arcsec = 0.1561 mm)
|Tracking system||Photoelectric sensor|
|Pressure inside the vacuum chamber||2 - 5 mmHg|
|Total weight||21 ton||
|Dispersion||0.33 A/mm (2nd order)||0.14 A/mm (5th order)|
|Effective wavelength range||3600 - 11000 A||3600 - 11000 A|
|Total weight||3 ton||10 ton|
|Note||Simultaneous observation of all the visible spectrum||High dispersion|