SU761974A1 - Twin-channel telescopic instrument - Google Patents

Description

The invention relates to astronomical instruments, namely, devices used to study the effect of optical instability of the atmosphere on the image quality of celestial objects.

Known periscopic system [1] ⁵

and a hyposcope [2], where two sighting tubes (channels) rotate relative to each other, which leads to a change in the distance between the inlets of the tubes (base of the instrument). This "property" ^{10 is} used in these devices only to determine the distance to objects and their stereoscopic viewing due to the cover. In this case, _constructed) $ nye the focus of the two channels of ground (surface) of the objects observed images are always separated from each other at a distance and are considered only one _{of 20} visually temporarily two eyes, which creates a stereoscopic effect.

Thus, in devices not about

combining two images,

2

created by sighting tubes, which does not allow to study the image quality of celestial objects, formed by telescopes with different diameters of lenses.

Also known is a double-beam astroclimate instrument containing two sighting tubes with lenses, mirrors, an optical mapping unit of two channels and a photodetector. In a two-beam instrument, the light from a celestial body, for example, from a star, enters the two inlets of two telescopes. These two inlets. Are separated from each other at some distance, called the base of the two-beam device. Then the light is collected in the focal plane of each of the two lenses with which the receiver is connected. Superimposed images of a star characterize atmospheric interference, which is studied only on a constant base, i.e., for the edge rays of that astronomical telescope,

761974

the size of the inlet of which is equal to the base of the two-beam device [3 ^.

To study the quality of star images. for smaller or larger telescopes

lens diameters than the base of the two-beam device, is no longer possible. ^five

The aim of the invention is to change the base of observation.

This goal is achieved by the fact that both target tubes are installed with ₁₀ possibility of rotation relative to each other around an axis coinciding with the geometric axis of symmetry of the optical alignment unit.

On fig. Figure 1 shows a general view of a two-variable telescope with a variable base; in fig. 2 and 3 - telescope longitudinal and transverse sections.

A two-channel variable-buff telescope consists of a left 1 n right 2 channel (sighting tube), a bracket 3, a platform (element) of a light receiver located in the focus of channels 4 and a flange 5.

The channels are mounted mirrors 6 and 7 in the frames 8 and 9, lenses 10 and 11, ₂₅

plane-parallel glass plates 12 and 13 fixed in cardan hangers, a reflective surface prism 14 (in the left) and a beam-splitting cube 15 (in the right) channels. _thirty

Sighting tubes 1 and 2 cylindrical guides - pins (not marked in the drawing) are installed in holes of bracket 3 fixed to flange 5. Flange 5 is made in the form of an angle 16 with a hole 17 for fastening a two-channel telescope to the mount's axis. ).

Channels 1 and 2 are fixed to flange _{40 by} racks 18 and 19. Racks 18 and 19 are able to move along the cylindrical surface of flange 5, rotating relative to the axis O - O, defined by the holes in the bracket 3 ₄₅

and non-cylindrical trunnions of the sighting tubes, thereby simulating the operation of telescopes with different diameters of the inlets.

FIG. 1 and 2 show the position ₅ θ of the sighting tubes 1 and 2, corresponding to the largest base between the inlets of the channels, for example, indicated by B ^,

In this position, light, for example, from a star, having entered channel 1 after reflection at an angle of 90 ° from mirror 6 and passing through the lens 10, plate 12, is reflected by a prism 14 at an angle of 90 ° and, passing the beam-splitting cube 15,

enters the light receiver 4, where the image of the star is formed. At the same time, channel 2, in the same way as channel 1, forms an image of a star on the same focal plane, combined with the image formed by channel [1}.

To combine with each other two. images of the star, given by individual channels of the device, and simultaneously with the axis O-O, the plane-parallel plates 12 and 13 should be installed perpendicular to the optical axes of the corresponding sighting tubes.

The image of the star thus obtained is equivalent to the quality of the image formed by the edge beams of that astronomical telescope, the size of the entrance aperture of which is equal to the maximum base of the two-channel telescope B ^.

By rotating the left channel in the directions of the arrow E and the right channel in the direction of the arrow F, the base between the inlets of the channels can be reduced, for example ^ to the size В ^.

In this position, in the focus of the two-channel telescope, a different quality of image of the star is obtained, equivalent to that which forms the telescope with lens diameter B ^, etc. Thus, the installation of possible bases of the proposed device forms a number of image qualities of the same object under study.

Their study allows you to choose the optimal size of the lens of the telescope installed in the area.

Claims (1)

Claim A two-channel telescopic device containing two target tubes with lenses, mirrors, an optical combination unit of two channels and a photo receiver, characterized in that, in order to change the observation base, the sight tubes are installed with the possibility of rotating relative each other around an axis coinciding with the geometric axis of symmetry optical alignment unit.