CN111562022B - Solar self-adaptive optical system for correcting strong turbulence - Google Patents
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Abstract
The invention discloses a solar self-adaptive optical system for correcting strong turbulence, which comprises a tilting mirror, a deformable mirror, a fine tracking wavefront sensor, a relevant shack-Hartmann wavefront sensor and a wavefront controller. The method aims at the requirements of high-resolution imaging observation on the sun under the condition of partial strong turbulence, starts from the detection wavelength, the correction order and the self structure of the adaptive optical system, improves the correction capability of the adaptive optical system under the condition of extreme turbulence intensity, and meets the application requirements of urban science popularization and the like. In the aspect of detection, the influence of strong turbulence is reduced by using long-wave detection; in terms of system parameters, the space-time characteristics of the correction object are analyzed, and a detection and correction unit is added to be matched with the turbulence intensity. On the aspects of control algorithm and correction order, on the basis of improving the closed-loop correction stability of the system by adopting mode method control, a method of high-order detection and low-order correction is carried out based on the analysis of correction precision requirements, and the stable closed-loop work of the system is further ensured.
Description
Technical Field
The invention relates to a solar self-adaptive optical system, belongs to the technical field of self-adaptive optics, and particularly relates to a solar self-adaptive optical system for strong turbulence correction, which is used for detecting and correcting optical wavefront distortion caused by extreme turbulence intensity (atmospheric coherence length is 3-5 cm) in the sun observation process.
Background
The self-adaptive optical system performs real-time compensation and correction on wavefront distortion caused by atmospheric turbulence to enable the large-caliber telescope to obtain ideal imaging capacity, and is a necessary device of the current large-caliber astronomical telescope. In the field of solar observation, although the aperture of a solar telescope is small, turbulence is stronger and more variable than night observation due to the influence of solar radiation on the earth in the daytime, so that a self-adaptive optical system is also needed to recover the high-resolution imaging capability of a large-aperture telescope.
As is well known, for a solar adaptive optics system, since the structural features of the solar atmosphere itself are required to be used as a beacon for wavefront extraction, in order to ensure a certain detection accuracy, in general, the design and operation of the solar adaptive optics system have a lower limit of atmospheric conditions, that is, an atmospheric turbulence is required to be not less than 8cm (Thomas r. rimmel and joint Marino, solar adaptive optics, Living rev. solar physics, 8,2, 2011). Although some systems improve a control algorithm and the like, the lower limit of the turbulence condition of the system operation can be properly reduced, the traditional solar adaptive optical system cannot work under the extreme turbulence condition.
Although some sites observed by the sun have better average seeing, the atmospheric seeing intensity is variable, and sometimes very poor instantaneous atmospheric seeing occurs; furthermore, as the range of human activities increases, the atmospheric conditions at the sites of early astronomical observations are increasingly affected. Even if a traditional solar adaptive optical system is equipped under the condition of partial atmospheric turbulence, high-resolution observation of the sun cannot be carried out. On the other hand, with the vigorous popularization of science popularization work in countries in recent years, science popularization observation puts forward new requirements on the traditional adaptive optical technology; due to the special popular science for the public, an area with good atmospheric conditions cannot be selected as a station site in a remote area, and due to the influence of human activities near cities, solar telescopes are exposed to extreme turbulent conditions. For the above application requirements, how to ensure that the solar adaptive optics system can stably work under extreme turbulent flow conditions is a new challenge facing adaptive optics technology.
Disclosure of Invention
The technical problem to be solved by the invention is as follows: the method aims at the requirements of high-resolution imaging observation on the sun under the condition of partial strong turbulence, starts from the detection wavelength, the correction order and the self structure of the adaptive optical system, improves the correction capability of the adaptive optical system under the condition of extreme turbulence intensity, and meets the application requirements of urban science popularization and the like. In the aspect of wave-front detection, the influence of strong turbulence is reduced by using long-wave detection; in the aspect of system parameters, the space-time characteristics of a correction object are analyzed, and a detection and correction unit is added to be matched with the turbulence intensity; on the aspects of control algorithm and correction order, on the basis of improving the closed-loop correction stability of the system by adopting mode method control, a method of high-order detection and low-order correction is carried out based on the analysis of correction precision requirements, and the stable closed-loop work of the system is further ensured.
The technical scheme adopted by the invention for solving the technical problems is as follows: a solar self-adaptive optical system for correcting strong turbulence comprises a collimating lens 1, an inclined wavefront corrector 2, a high-order wavefront corrector 3, a first spectroscope 4, a fine tracking wavefront sensor 5, a fine tracking wavefront correction controller 6, a second spectroscope 7, an imaging subsystem 8, a relevant shack-Hartmann wavefront sensor 9 and a high-order wavefront correction controller 10. The tilt wavefront corrector 2, the fine tracking wavefront sensor 5 and the fine tracking wavefront correction controller 6 form a closed-loop subsystem for performing tilt correction on the atmospheric turbulence. The higher-order wavefront corrector 3, the associated shack-hartmann wavefront sensor 9 and the higher-order wavefront correction controller 10 constitute a closed-loop subsystem for performing higher-order aberration correction on atmospheric turbulence. Light passing through the primary focus of the telescope is first collimated by a collimator lens 1 and then enters a tilted wavefront corrector 2 and a higher order wavefront corrector 3, where the higher order wavefront corrector 3 is located at a conjugate position of the telescope's entrance pupil. The first beam splitter 4 divides the light into two beams, and one beam is used for detecting low-order oblique aberration by the fine tracking wavefront sensor 5; the other beam enters an imaging subsystem 8 and a related shack-Hartmann wavefront sensor 9 through a second beam splitter 7 respectively.
In order to improve the accuracy of high-order wavefront detection under an extreme turbulence condition (the atmospheric coherence length is 3-5 cm), the system abandons the traditional classical detection waveband (500-550 nm), and adopts a TiO waveband (central wavelength 705.7nm) with longer wavelength to perform wavefront detection. The detection wavelength and the turbulence intensity have the following relationship:
wherein λ is 0 And λ d Respectively, the measuring wavelength of the turbulence intensity and the detection wavelength, r, of the adaptive optics 0 And
respectively, the atmospheric coherence length corresponding to the turbulence measurement and adaptive optics detection wavelengths. Known length ofWave detection can increase the atmospheric turbulence coherence length and improve the wave front detection precision. In addition, the opacity of the TiO wave band is very sensitive to temperature, the line depth of TiO is obviously increased in the penumbra of black particles, particularly in the area with low temperature such as the penumbra, and the wave band is adopted for wavefront detection, so that higher image contrast is obtained when the solar active region is observed, and the extraction of the wavefront aberration of the system is facilitated.
In order to improve the correction capability of the system, according to the design principle that the space scale of the wavefront detection and correction of the system is equivalent to the coherence length of the atmospheric turbulence, the influence of the sampling error of the wavefront sensor of the system and the fitting error of the wavefront corrector on the correction effect is reduced, and the system is ensured to have enough detection and correction capability on the strong turbulence.
On the basis of the mode closed-loop correction, when the front N-term Zernike mode of the distorted wavefront is completely corrected, the residual high-order wavefront distortion RMS value sigma is φ ＝0.14λ I When the imaging resolution can reach twice the optical diffraction limit resolution of the telescope, the system is considered to meet the requirement of self-adaptive optical wavefront correction, wherein lambda is I Representing the center wavelength of the imaging band. According to the theory of the turbulent aberration decomposition by Zernike based on Robert j.noll (Robert j.noll, Zernike polymoials and tomo scientific interference.j.opt.soc.am., 3,66,1976), the residual high-order wavefront aberration after the current N-term modal aberration is corrected can be expressed as:
wherein D and
the aperture of the imaging solar telescope and the atmospheric coherence length corresponding to the imaging wave band are respectively, and N is the number of terms of a corrected Zernike mode. According to the aperture of the telescope, the imaging wavelength and the corresponding turbulence intensity, the order of the wavefront aberration to be corrected can be calculated. It can be found that for small-caliber solar telescopes, the requirements can be met only by correcting very limited orders.
The relevant shack-Hartmann wavefront sensor adopts a TiO (central wavelength 705.6nm) waveband as a detection wavelength. The TiO wave band is more sensitive to temperature and is suitable for observing the solar active black particles in a low-temperature area, and in addition, compared with the traditional detection wavelength of about 500nm, the long-wave detection further reduces the influence of strong turbulence, so that the detection precision is improved.
The first spectroscope 4 and the second spectroscope 7 are both dichroic spectroscopes. Wherein, the first spectroscope 4 transmits the wave-front detector needed wavelength and reflects other wavelengths; the second beam splitter 7 reflects the wavelength required by the detection of the high-order wavefront aberration and transmits the rest wavelengths for high-resolution imaging. The transmission and reflection wavelengths of the first beam splitter 4 and the second beam splitter 7 can be interchanged according to the arrangement positions of the components of the system.
The fine tracking wavefront sensor 5 is composed of a relay optical element 11, an aperture diaphragm 12, an imaging objective lens 13 and an imaging camera 14. Under the condition of strong turbulence, an aperture diaphragm can be used for reducing an imaging aperture, the influence of the turbulence on image quality is reduced, and the extraction of low-order oblique aberration by the fine tracking wavefront sensor is facilitated.
The imaging subsystem 9 may include one or more imaging channels as required.
Compared with the prior art, the invention has the advantages that:
(1) the invention abandons the classical wave-front detection wave band (500 nm-550 nm) of the traditional solar adaptive optics and adopts a TiO wave band (central wavelength 705.7nm) with longer wavelength to carry out wave-front detection. The TiO wave band is more sensitive to temperature and is suitable for observing solar active black seeds in a low-temperature area; in addition, compared with the traditional detection wavelength of about 500nm, the long-wave detection further reduces the influence of strong turbulence, thereby improving the detection precision.
(2) The invention is used as a self-adaptive optical system specially aiming at the closed-loop correction of the solar active area, and breaks through the limitation that the space scale of the traditional solar self-adaptive optical system is not less than 8cm in wave-front detection and correction. According to the design principle that the space scale of the system wave-front detection and correction is equivalent to the coherence length of the atmospheric turbulence, the space sampling rate far higher than that of a conventional solar self-adaptive optical system is adopted, the influence of the sampling error of a system wave-front sensor and the fitting error of a wave-front corrector on the correction effect is reduced, and the system is ensured to have enough detection and correction capability on the strong turbulence.
(3) On the basis of mode-method closed-loop correction, the invention breaks through the convention that wavefront detection is matched with wavefront correction, carries out the control method of high-order detection and low-order correction, and further improves the correction effectiveness on the basis of ensuring the stable closed-loop work of the system.
Drawings
FIG. 1 is a schematic block diagram of the optical path of a solar adaptive optics system for high turbulence correction according to the present invention;
FIG. 2 is a schematic diagram of a fine tracking wavefront sensor according to the present invention;
fig. 3 is an example of the arrangement of the corresponding detection and correction units of the shack-hartmann wavefront sensor and the wavefront corrector of the sun adaptive optics system for strong turbulence correction designed on the basis of a 600 mm-caliber solar telescope.
In the figure, 1 is a collimating lens, 2 is an inclined wavefront corrector, 3 is a high-order wavefront corrector, 4 is a first beam splitter, 5 is a fine tracking wavefront sensor, 6 is a fine tracking wavefront correction controller, 7 is a second beam splitter, 8 is a second beam splitter, 9 is a correlated shack-hartmann wavefront sensor, 10 is a high-order wavefront correction controller, 11 is a collimating relay optical element, 12 is an aperture diaphragm, 13 is an imaging objective lens, and 14 is an imaging camera.
Detailed Description
The present invention will be further explained below by taking the design of the adaptive optics system of a 600mm aperture solar telescope as an example, with reference to the accompanying drawings.
As shown in fig. 1, the system is composed of a collimating mirror 1, an inclined wavefront corrector 2, a higher-order wavefront corrector 3, a first beam splitter 4, a fine tracking wavefront sensor 5, a fine tracking wavefront correction controller 6, a second beam splitter 7, a second beam splitter 8, a relevant shack-hartmann wavefront sensor 9 and a higher-order wavefront correction controller 10. The tilt wavefront corrector 2, the fine tracking wavefront sensor 5 and the fine tracking wavefront correction controller 6 form a closed-loop subsystem for performing tilt correction on the atmospheric turbulence. The higher-order wavefront corrector 3, the associated shack-hartmann wavefront sensor 9 and the higher-order wavefront correction controller 10 constitute a closed-loop subsystem for performing higher-order aberration correction on atmospheric turbulence.
Light passing through the primary focus of the telescope is first collimated by a collimator lens 1 and then enters a tilted wavefront corrector 2 and a higher order wavefront corrector 3, where the higher order wavefront corrector 3 is located at a conjugate position of the telescope's entrance pupil. The first beam splitter 4 divides the light into two beams, and one beam is used for detecting low-order oblique aberration by the fine tracking wavefront sensor 5; the other beam enters an imaging subsystem 8 and a related shack-Hartmann wavefront sensor 9 through a second beam splitter 7 respectively.
In order to improve the accuracy of high-order wavefront detection under an extreme turbulence condition (the atmospheric coherence length is 3-5 cm), the system abandons the traditional classical detection waveband (500-550 nm), and adopts a TiO waveband (central wavelength 705.7nm) with longer wavelength to perform wavefront detection. The detection wavelength and the turbulence intensity have the following relationship:
wherein λ is 0 And λ d Respectively, the measuring wavelength of the turbulence intensity and the detection wavelength, r, of the adaptive optics 0 And
respectively, the atmospheric coherence length corresponding to the turbulence measurement and adaptive optics detection wavelengths. It can be known that the wavelength λ 0 4cm atmospheric coherence length, measured 500nm, 6.05cm in the TiO band. In addition, the opacity of the TiO wave band is very sensitive to temperature, the line depth of TiO is obviously increased in the penumbra of black particles, particularly in the area with low temperature such as the penumbra, and the wave band is adopted for wavefront detection, so that higher image contrast is obtained when the solar active region is observed, and the extraction of the wavefront aberration of the system is facilitated.
As shown in fig. 2, the fine tracking wavefront sensor includes a collimating relay optical element 11, an aperture stop 12, an imaging objective lens 13, and an imaging camera 14. Under the condition of strong turbulence, an aperture diaphragm can be used for reducing an imaging aperture, the influence of the turbulence on image quality is reduced, and the extraction of low-order oblique aberration by the fine tracking wavefront sensor is facilitated.
Fig. 3 shows the arrangement of the detection and correction units corresponding to the shack-hartmann wavefront sensor and the wavefront corrector of the solar adaptive optical system for strong turbulence correction designed on a 600 mm-caliber solar telescope. In order to improve the correction capability of the system, according to the design principle that the space scale of the wavefront detection and correction of the system is equivalent to the coherence length of the atmospheric turbulence, the influence of the sampling error of the wavefront sensor of the system and the fitting error of the wavefront corrector on the correction effect is reduced, and the system is ensured to have enough detection and correction capability on the strong turbulence. For a 600mm aperture solar telescope, in order to correct strong turbulence with an atmospheric turbulence coherence length of 4cm, 15 wavefront detection and correction units are required in the radial direction and are arranged in a square, and 177 units are required in the whole system, which is much higher than that of the traditional solar adaptive optics system.
On the basis of mode closed-loop correction, when the front N-term Zernike mode of the distorted wavefront is completely corrected, the residual high-order wavefront distortion RMS value sigma φ ＝0.14λ I When the imaging resolution can reach twice the optical diffraction limit resolution of the telescope, the system is considered to meet the requirement of self-adaptive optical wavefront correction, wherein lambda is I Representing the center wavelength of the imaging band. Noll, based on the theory of Zernike decomposition of turbulent aberrations, the residual higher order wavefront aberration after the current N-mode aberration is corrected can be expressed as:
wherein D and
the aperture of the imaging solar telescope and the atmospheric coherence length corresponding to the imaging wave band are respectively, and N is the number of terms of a corrected Zernike mode. According to the aperture of the telescope, the imaging wavelength and the corresponding turbulence intensity, the instrument can be usedThe order of the wavefront aberration that needs to be corrected is calculated. It can be found that for small-caliber solar telescopes, the requirements can be met only by correcting very limited orders. A600 mm-aperture solar telescope and an imaging wavelength are considered, a TiO waveband is selected, the requirement can be met only by correcting the front 27 Zernike wave front aberrations under the condition that the corresponding turbulence intensity is 4cm, and for a 177-unit system, the system stability is greatly improved through low-order partial correction.
Portions of the invention not described in detail are within the skill of the art.
Claims (5)
1. A solar adaptive optics system for high turbulence correction, characterized by: the high-order wavefront correction system comprises a collimating mirror (1), an inclined wavefront corrector (2), a high-order wavefront corrector (3), a first spectroscope (4), a fine tracking wavefront sensor (5), a fine tracking wavefront correction controller (6), a second spectroscope (7), an imaging subsystem (8), a related shack-Hartmann wavefront sensor (9) and a high-order wavefront correction controller (10), wherein the inclined wavefront corrector (2), the fine tracking wavefront sensor (5) and the fine tracking wavefront correction controller (6) form a closed-loop subsystem for performing inclined correction on atmospheric turbulence, the high-order wavefront corrector (3), the related shack-Hartmann wavefront sensor (9) and the high-order wavefront correction controller (10) form a closed-loop subsystem for performing high-order aberration correction on the atmospheric turbulence, and light passing through a main focus of a telescope is firstly collimated by the collimating mirror (1), then the light enters a tilted wavefront corrector (2) and a high-order wavefront corrector (3), wherein the high-order wavefront corrector (3) is positioned at the conjugate position of the entrance pupil of the telescope, the first beam splitter (4) divides the light into two beams, and one beam is used for a fine tracking wavefront sensor (5) to detect low-order tilted aberration; the other beam enters an imaging subsystem (8) and a related shack-Hartmann wavefront sensor (9) through a second beam splitter (7) respectively;
In order to improve the accuracy of high-order wavefront detection under an extreme turbulence condition, namely, the atmospheric coherence length is 3-5 cm, the system abandons the traditional classical detection waveband of 500-550 nm, adopts a TiO waveband with longer wavelength and central wavelength of 705.7nm to perform wavefront detection, and the detection wavelength and the turbulence intensity have the following relationship:
wherein λ is 0 And λ d The measuring wavelength of the turbulence intensity and the detection wavelength, r, of the adaptive optics system, respectively 0 And
the atmospheric coherence length corresponding to the detection wavelength of the turbulence measurement and the adaptive optical system respectively can be known, the atmospheric turbulence coherence length can be increased by long-wave detection, the wave-front detection precision is improved, the opacity of a TiO wave band is very sensitive to the temperature, the line depth of TiO is obviously increased in the area with low temperature such as a shadow and the like in the penumbra of a black son, the wave-front detection is carried out by adopting the wave band, higher image contrast is obtained when the sun active region is observed, and the extraction of the system wave-front aberration is facilitated;
in order to improve the correction capability of the system, according to the design principle that the space scale of the system wavefront detection and correction is equivalent to the coherence length of the atmospheric turbulence, the influence of the sampling error of a system wavefront sensor and the fitting error of a wavefront corrector on the correction effect is reduced, the system is ensured to have enough detection and correction capability to the strong turbulence, and on the basis of the mode method closed-loop correction, when the front N-term Zernike mode of the distorted wavefront is completely corrected, the residual high-order wavefront distortion RMS value sigma (RMS) is completely corrected φ ≤0.14λ I When the imaging resolution can reach twice the optical diffraction limit resolution of the telescope, the system is considered to meet the requirement of self-adaptive optical wavefront correction, wherein lambda is I Representing the center wavelength of the imaging band, according to the theory of Robert J.Noll based on Zernike decomposition of turbulent aberrations, the variance of the residual higher-order wavefront aberrations after the current N-term mode aberrations are corrected can be expressed as:
wherein D and
the order of wavefront aberration to be corrected can be calculated according to the aperture of the telescope, the imaging wavelength and the corresponding turbulence intensity, and for the small-aperture solar telescope, the requirement can be met only by correcting very limited order.
2. The solar adaptive optics system for high turbulence correction according to claim 1, wherein: the relevant shack-Hartmann wavefront sensor adopts a TiO wave band with the central wavelength of 705.6nm as a detection wavelength, the TiO wave band is more sensitive to temperature and is suitable for observing solar activity blackcurrants in a low-temperature area, and compared with the traditional detection wavelength of about 500nm, the long-wave detection further reduces the influence of strong turbulence, thereby improving the detection precision.
3. The solar adaptive optics system for high turbulence correction as recited in claim 1, wherein: the first spectroscope (4) and the second spectroscope (7) are dichroic spectroscopes, wherein the first spectroscope (4) transmits the wavelength required by the fine tracking wavefront detector and reflects the rest of wavelengths; the second spectroscope (7) reflects the wavelength required by the detection of the high-order wavefront aberration, transmits the rest wavelengths for high-resolution imaging, and the transmission and reflection wavelengths of the first spectroscope (4) and the second spectroscope (7) can be interchanged according to the arrangement positions of all components of the system.
4. The solar adaptive optics system for high turbulence correction as recited in claim 1, wherein: the precise tracking wavefront sensor (5) is composed of a relay optical element (11), an aperture diaphragm (12), an imaging objective lens (13) and an imaging camera (14), and the aperture diaphragm is used for reducing the imaging aperture under the condition of strong turbulence, so that the influence of the turbulence on image quality is reduced, and the precise tracking wavefront sensor can conveniently extract low-order oblique aberration.
5. The solar adaptive optics system for high turbulence correction as recited in claim 1, wherein: the imaging subsystem comprises one or more imaging channels according to the requirement.
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