Large-aperture high-precision Cassegrain refraction and reflection type day lug astronomical telescope

Abstract

The invention relates to the technical field of telescopes, and discloses a large-aperture high-precision Cassegrain refraction and reflection type day er astronomical telescope which comprises a front-end ERF filter, a self optical assembly, a built-in magnifying lens, an interferometer etalon and a tail-end cut-off filter, the front-end ERF filter is installed on the left side of the front-end ERF filter, and the tail-end cut-off filter is installed on the right side of the front-end ERF filter. The built-in magnifying lens is arranged on the right side of the self optical assembly, the interferometer etalon is arranged on the right side of the built-in magnifying lens, and the tail end cut-off filter is arranged on the right side of the interferometer etalon; through the cooperation of the above structures, the transmittance and cut-off depth of the filter can be optimized, so that the telescope system can better adapt to different observation requirements and conditions, the observation accuracy and precision are improved, and the observation safety and the equipment stability are ensured.

Description

Technical Field

[0001] The present invention belongs to the technical field of telescopes, and specifically relates to a large-aperture, high-precision Cassegrain catadioptric solar prominence telescope. Background Art

[0002] Currently, all solar prominence telescopes on the market are refracting telescopes. Due to the characteristics of refracting telescopes themselves, the aperture is limited. Moreover, for large-aperture refracting telescope interferometer etalons, they need to be made very large, resulting in high costs. And for long-focal-length lens barrels, they are very long, with large volumes and are not convenient to carry. Some traditional telescope filters often have relatively wide bandwidths and cannot accurately filter the light in the H-α band, resulting in unclear details of the solar chromosphere and prominences observed. The filtering accuracy may not reach the high precision required for observing the solar chromosphere and prominences, affecting the observation effect. The filter is not precise enough to effectively cope with the influence of temperature changes on the imaging stability, affecting the observation effect, and it is difficult to adapt to different observation requirements and conditions, with poor observation accuracy, precision, and safety.

[0003] Therefore, we propose a large-aperture, high-precision Cassegrain catadioptric solar prominence telescope. Summary of the Invention

[0004] The purpose of the present invention is to provide a large-aperture, high-precision Cassegrain catadioptric solar prominence telescope in order to better adapt to different observation requirements and conditions, improve the accuracy and precision of observations, ensure the safety of observations and the stability of the equipment.

[0005] The technical solution adopted by the present invention is as follows: A large-aperture, high-precision Cassegrain catadioptric solar prominence telescope, including a front-end ERF filter, its own optical components, an internal barlow lens, an interferometer etalon, and a terminal cut-off filter. The front-end ERF filter is installed on the left side of the front-end ERF filter, the internal barlow lens is arranged on the right side of the own optical components, the interferometer etalon is arranged on the right side of the internal barlow lens, and the terminal cut-off filter is arranged on the right side of the interferometer etalon.

[0006] In a preferred embodiment of the invention, the front-end ERF filter has an H-α narrow-band filter with a bandwidth of about 100 nm.

[0007] In a preferred embodiment of the invention, the own optical components include a primary mirror, a secondary mirror, a corrector lens, and an eyepiece.

[0008] In a preferred embodiment of the invention, the interferometer etalon has two extremely precise parallel flat glass plates.

[0009] In a preferred embodiment of the invention, the parallel flat glass plates are ground to a flatness level better than 1 / 100 wavelength RMS.

[0010] In a preferred embodiment of the invention, the end cut-off filter is composed of an induced filter and a cut-off filter.

[0011] In a preferred embodiment of the invention, the bandwidth of the induced filter is 6 nm, and the bandwidth of the cut-off filter is 0.6 nm.

[0012] In a preferred embodiment of the invention, the built-in teleconverter extends the focal ratio of the telescope to F / 30.

[0013] In summary, due to the adoption of the above technical solutions, the beneficial effects of the present invention are as follows: 1. In the present invention, the unnecessary band light is filtered by the front-end ERF filter, reducing heat accumulation, thereby protecting the interferometer etalon from damage and ensuring the stability and durability of the telescope system; in the extremely narrow-band observation in the range of 0.1 - 0.01 nm, the front-end ERF filter can ensure extremely high transmittance within the window wavelength range, enabling only the light of the target wavelength to pass through smoothly, while the stray light is effectively suppressed, which helps to improve the accuracy and precision of the observation, making the observed celestial phenomena such as prominences clearer and more detailed, and enabling the observer to obtain high-quality images and data; the design of the front-end ERF filter not only considers the need for light reduction, but also runs through the goal of suppressing stray light energy. This comprehensive design makes the film system design of the coronagraph system more complex and delicate, but at the same time improves the overall performance of the system; by optimizing the transmittance and cut-off depth of the filter, the telescope system can better adapt to different observation requirements and conditions.

[0014] 2. In the present invention, by controlling the refractive index and spacing of the medium between the two glass reflecting surfaces through the interferometer etalon, the continuous light can be "comb-filtered", and a spiky transmission spectrum can be output. The high-precision flatness and parallelism can ensure the stability and consistency of the filtering performance, and can significantly improve the interference effect and enhance the filtering performance.

[0015] 3. In the present invention, the filter of the end cut-off filter has a bandwidth of 0.6 nm, which can accurately match a single spike in the light after the comb-filtering of the etalon. Through its high-precision filtering characteristics, it can effectively screen out the specific wavelength light required for observation, improving the accuracy and precision of the observation; moreover, this filter has the characteristic of high cut-off depth, which can deeply cut off harmful infrared and ultraviolet rays, effectively blocking the entry of these rays, ensuring the safety of the observation and the stability of the equipment. BRIEF DESCRIPTION OF THE DRAWINGS

[0016] Figure 1 is a schematic structural diagram of the present invention; Figure 2 is the first optical quality parameter diagram of the present invention; Figure 3 It is the second optical quality parameter diagram of the present invention; Figure 4 It is the third optical quality parameter diagram of the present invention.

[0017] Explanation of reference numerals: 1 - front-end ERF filter; 2 - its own optical component; 3 - built-in teleconverter; 4 - interferometer etalon; 5 - end cut-off filter. Detailed implementation manners

[0018] To make the objectives, technical solutions and advantages of the embodiments of the present invention clearer, the technical solutions in the embodiments of the present invention will be clearly and completely described below in conjunction with the embodiments of the present invention. Obviously, the described embodiments are part of the embodiments of the present invention, rather than all of the embodiments. All other embodiments obtained by those of ordinary skill in the art based on the embodiments of the present invention without making creative efforts shall fall within the protection scope of the present invention.

[0019] Below will be combined with Figures 1 - 4 A detailed description will be given of the large-aperture high-precision Cassegrain catadioptric solar prominence telescope according to the embodiments of the present invention. Embodiment

[0020] Refer to Figures 1 - 4, a large-aperture, high-precision Cassegrain catadioptric solar prominence telescope, which includes a front-end ERF filter 1, its own optical components 2, a built-in Barlow lens 3, an interferometer etalon 4, and a terminal cut-off filter 5. The front-end ERF filter 1 is installed on the left side of the front-end ERF filter 1. The built-in Barlow lens 3 is arranged on the right side of its own optical components 2. The interferometer etalon 4 is arranged on the right side of the built-in Barlow lens 3. The built-in Barlow lens 3 extends the focal ratio of the telescope to F / 30. The terminal cut-off filter 5 is arranged on the right side of the interferometer etalon 4. Its own optical components 2 include a primary mirror, a secondary mirror, a corrector lens, and an eyepiece. The front-end ERF filter 1 has an H-α narrowband filter with a bandwidth of about 100 nm. Specifically, a large-aperture solar prominence mirror is combined with a front-end ERF filter 1 to prevent excessive heat after light concentration from damaging the interferometer etalon 4 and ensure the stability and durability of the telescope system. Because in the extremely narrowband observation in the order of 0.1 - 0.01 nm, even for a bright target like the sun, too low transmittance will result in dim imaging, poor visual effect, and low signal-to-noise ratio in photography. However, in the extremely narrowband observation in the order of 0.1 - 0.01 nm, the front-end ERF filter 1 can ensure extremely high transmittance within the window wavelength range, allowing only the light of the target wavelength to pass through smoothly while effectively suppressing stray light, which helps improve the accuracy and precision of observation, making celestial phenomena such as solar prominences observed more clearly and meticulously, enabling the observer to obtain high-quality images and data. The design of the front-end ERF filter 1 not only considers the need for light reduction but also aims at suppressing the energy of stray light. This comprehensive design makes the thin film design of the solar prominence mirror system more complex and delicate, but at the same time improves the overall performance of the system. By optimizing the transmittance and cut-off depth of the filter, the telescope system can better adapt to different observation requirements and conditions.

[0021] Refer to Figures 1 - 4 , the interferometer etalon 4 has two extremely high-precision parallel flat glasses, and the parallel flat glasses are ground to a flatness level better than 1 / 100 wavelength RMS. Specifically, by controlling the refractive index and spacing of the medium between the two glass reflecting surfaces through the interferometer etalon 4, continuous light can be "comb-filtered" to output a spike-shaped transmission spectrum. The high-precision flatness and parallelism can ensure the stability and consistency of the filtering performance, and can significantly improve the interference effect and enhance the filtering performance.

[0022] Refer to Figures 1 - 4, the end cut-off filter 5 is composed of an induced filter and a cut-off filter. The bandwidth of the induced filter is 6 nm, and the bandwidth of the cut-off filter is 0.6 nm. Specifically, the filter of the end cut-off filter 5 has a bandwidth of 0.6 nm, which can accurately match a single peak in the light after the etalon comb filtering. Through its high-precision filtering characteristics, it can effectively screen out the specific wavelength light required for observation, improving the accuracy and precision of observation. Moreover, this filter has the characteristic of high cut-off depth, which can deeply cut off harmful infrared and ultraviolet rays, effectively blocking the entry of these rays, ensuring the safety of observation and the stability of the equipment.

[0023] The implementation principle of the large-aperture high-precision Cassegrain catadioptric solar prominence telescope of this application is as follows: By filtering out unnecessary band light through the front-end ERF filter 1, heat accumulation is reduced, thereby protecting the etalon 4 of the interferometer from damage and ensuring the stability and durability of the telescope system. In the extremely narrow-band observation in the order of 0.1 - 0.01 nm, the front-end ERF filter 1 can ensure extremely high transmittance within the window wavelength range, enabling only the light of the target wavelength to pass through smoothly, while stray light is effectively suppressed, which helps to improve the accuracy and precision of observation, making celestial phenomena such as solar prominences observed clearer and more detailed, enabling observers to obtain high-quality images and data. The design of the front-end ERF filter 1 not only considers the need for light reduction but also runs through the goal of suppressing stray light energy. This comprehensive design makes the film system design of the solar prominence mirror system more complex and delicate, but at the same time improves the overall performance of the system. By optimizing the transmittance and cut-off depth of the filter, the telescope system can better adapt to different observation requirements and conditions.

[0024] On the other hand, by controlling the refractive index and spacing of the medium between the two glass reflecting surfaces through the etalon 4 of the interferometer, continuous light can be "comb-filtered" to output a spike-shaped transmission spectrum. The high-precision flatness and parallelism can ensure the stability and consistency of the filtering performance, significantly improving the interference effect and enhancing the filtering performance. The filter of the end cut-off filter 5 has a bandwidth of 0.6 nm, which can accurately match a single peak in the light after the etalon comb filtering. Through its high-precision filtering characteristics, it can effectively screen out the specific wavelength light required for observation, improving the accuracy and precision of observation. Moreover, this filter has the characteristic of high cut-off depth, which can deeply cut off harmful infrared and ultraviolet rays, effectively blocking the entry of these rays, ensuring the safety of observation and the stability of the equipment.

[0025] It should be noted that, in this document, relational terms such as first and second are only used to distinguish one entity or operation from another entity or operation, and do not necessarily require or imply any actual relationship or order between these entities or operations. Moreover, the term "comprising", "including" or any other variant thereof is intended to cover non-exclusive inclusion, so that a process, method, article or device comprising a series of elements not only includes those elements, but also includes other elements not expressly listed, or also includes elements inherent to such process, method, article or device. Without further limitation, an element defined by the statement "comprising an..." does not exclude the existence of additional identical elements in the process, method, article or device comprising the element.

[0026] The above embodiments are only used to illustrate the technical solutions of the present invention, rather than to limit it; although the present invention has been described in detail with reference to the foregoing embodiments, those of ordinary skill in the art should understand that they can still modify the technical solutions recorded in the foregoing embodiments, or perform equivalent replacements for some of the technical features; and these modifications or replacements do not cause the essence of the corresponding technical solutions to deviate from the spirit and scope of the technical solutions of the embodiments of the present invention.

Claims

1. A large-aperture, high-precision Cassegrain catadioptric prominence astronomical telescope, comprising a front-end ERF filter (1), an optical component (2), a built-in multiplier (3), an interferometer etalon (4) and a terminal cutoff filter (5), characterized in that: The front-end ERF filter (1) is installed on the left side of the front-end ERF filter (1), the built-in magnifier (3) is arranged on the right side of the optical component (2), the interferometer etalon (4) is arranged on the right side of the built-in magnifier (3), and the end cut-off filter (5) is arranged on the right side of the interferometer etalon (4).

2. The large-aperture, high-precision Cassegrain catadioptric prominence astronomical telescope according to claim 1, characterized in that: The front-end ERF filter (1) is an H-alpha narrowband filter with a bandwidth of about 100 nm.

3. The large-aperture, high-precision Cassegrain catadioptric prominence telescope according to claim 1, characterized in that: The optical component (2) comprises a primary mirror, a secondary mirror, a corrective mirror and an eyepiece.

4. The large-aperture, high-precision Cassegrain catadioptric prominence astronomical telescope according to claim 1, characterized in that: The interferometer etalon (4) has two pieces of extremely high-precision parallel flat glass.

5. The large-aperture, high-precision Cassegrain catadioptric prominence astronomical telescope according to claim 4, characterized in that: The parallel plate glass is ground to a flatness level better than 1 / 100 wavelength RMS.

6. The large-aperture, high-precision Cassegrain catadioptric prominence astronomical telescope according to claim 1, characterized in that: The terminal cut-off filter (5) is composed of an induction filter and a cut-off filter.

7. The large-aperture, high-precision Cassegrain catadioptric prominence astronomical telescope according to claim 6, characterized in that: The bandwidth of the induction filter is 6 nm, and the bandwidth of the cutoff filter is 0.6 nm.

8. The large-aperture, high-precision Cassegrain catadioptric prominence astronomical telescope according to claim 1, characterized in that: The built-in magnifier (3) extends the focal ratio of the telescope to F / 30.

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