CN112070822A - Synchronization method for equatorial telescope for lunar observation of foundation - Google Patents

Synchronization method for equatorial telescope for lunar observation of foundation Download PDF

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CN112070822A
CN112070822A CN202010878140.4A CN202010878140A CN112070822A CN 112070822 A CN112070822 A CN 112070822A CN 202010878140 A CN202010878140 A CN 202010878140A CN 112070822 A CN112070822 A CN 112070822A
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moon
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lunar
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CN112070822B (en
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王一豪
王爽
武俊强
李娟�
刘欢
冯向朋
胡炳樑
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XiAn Institute of Optics and Precision Mechanics of CAS
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Abstract

The invention relates to an equatorial telescope synchronization method, in order to solve the technical problems that the manpower consumption is large and the precision error is large in the traditional astronomical observation field that the equatorial telescope synchronization correction adopts a manual observation and adjustment method, the invention provides a synchronization method of a geostationary moon observation equatorial telescope, a star finder is adopted to identify the lunar centroid through an image processing mode, the equatorial telescope can be synchronized without strictly aligning the optical axes of a slit-type spectrometer and the star finder, the minimum circumcircle algorithm adopted for identifying the lunar centroid is not influenced by the lunar phase, the lunar centroid can be accurately identified without judging the lunar phase; the equatorial telescope is synchronized through the lunar centroid position, extra star map data are not needed, and the synchronization method is accurate and simple.

Description

Synchronization method for equatorial telescope for lunar observation of foundation
Technical Field
The invention relates to an equatorial telescope synchronization method, in particular to a synchronization method for a foundation-to-moon observation equatorial telescope.
Background
The moon is used as a highly stable radiation source, ground-based moon observation is carried out, a full-moon phase period moon radiation model is established, and the method has important significance for on-orbit moon calibration. As shown in fig. 1, the ground-based moon observation system comprises a slit-type spectrometer 01, a large-field finder 02, an equatorial telescope 03, an industrial personal computer 04 and other main devices, wherein the equatorial telescope 03 serves as a turntable, the slit-type spectrometer 01 is mounted on the equatorial telescope 03, the finder 02 is fixed on the slit-type spectrometer 01, the finder 02 and the slit-type spectrometer 01 synchronously move under the driving of the equatorial telescope 03, the slit-type spectrometer 01 is used for collecting lunar spectrum data, the finder 02 is used for lunar positioning and lunar image data collection, the equatorial telescope 03 serves as a turntable for stably tracking a moon, and the industrial personal computer 04 is mainly used for analyzing and processing data.
The conventional monthly observation task requires that lunar data are collected for N times at equal time intervals. Before data is collected each time, the spectrometer 01 carried by the equatorial telescope 03 is controlled to point to the moon according to the lunar right ascension and declination coordinates at the current moment, wherein the lunar right ascension and declination coordinates are calculated by a lunar formula according to the current observation place and observation time. Since the slit spectrometer 01 has a small field of view, it is required that the lunar pointing accuracy is high, otherwise, complete lunar spectral data cannot be acquired. However, since the mechanical rotation of the equatorial telescope 03 has accumulated errors and the lunar right ascension and declination coordinates of the moon at the current time calculated by the lunar equation have errors, even if the equatorial telescope 03 is aligned to the moon in the initial state, the pointing direction of the equatorial telescope 03 is deviated after several lunar data acquisitions at time intervals, so that the slit-type spectrometer 01 cannot acquire complete lunar spectral data.
The traditional solution is to observe the moon for a period of time, manually observe whether the moon spectral data is complete, when the moon is found to deviate from the view field of the slit-type spectrometer 01, suspend the observation task, manually control the slit-type spectrometer 01 carried by the equatorial telescope 03 to point to the center of the moon again, then synchronize the internal coordinate system of the equatorial telescope 03, and achieve the purpose of calibrating the equatorial telescope 03. The traditional manual method consumes manpower, automatic monthly observation can not be realized all night long, and errors exist in the precision of the method for manually controlling the equatorial telescope 03.
Disclosure of Invention
The invention provides a synchronization method for a foundation-to-moon observation equatorial telescope, which aims to solve the technical problems of high labor consumption and high precision error of a manual observation and adjustment method for synchronization correction of the equatorial telescope in the field of traditional astronomical observation.
In order to achieve the purpose, the invention provides the following technical scheme:
a synchronization method for a foundation-to-moon observation equatorial telescope is characterized by comprising the following steps:
s1, adjusting the right ascension coordinate and the declination coordinate of the equatorial telescope to enable the slit type spectrometer to be aligned with the moon;
s2, obtaining the coordinates (cx) of the moon centroid image in the finder mirror at the moment by adopting a threshold segmentation method and a minimum circumcircle algorithm0,cy0) Setting the coordinate as the moon reference coordinate of the finder mirror;
s3, adjusting the right ascension coordinates of the equatorial telescope to enable the moon image to move from the upper edge to the lower edge of the finder, obtaining the moon centroid image coordinates and right ascension coordinates corresponding to the moon positioned at the upper edge of the finder, and the moon centroid image coordinates and right ascension coordinates corresponding to the moon positioned at the lower edge of the finder, and calculating to obtain the relation coefficient pra of the moon moving from the upper edge to the lower edge of the finder, the moon centroid image coordinate change value and the right ascension coordinate change value;
s4, adjusting the declination coordinate of the equatorial telescope to enable the moon image to move from the left edge to the right edge of the finder mirror, obtaining the moon centroid image coordinate and the declination coordinate corresponding to the moon located at the left edge of the finder mirror, and the moon centroid image coordinate and the declination coordinate corresponding to the moon located at the right edge of the finder mirror, and calculating the relation coefficient pdec of the moon moving from the left edge to the right edge of the finder mirror, and the moon centroid image coordinate change value and the declination coordinate change value;
s5, during observation, calculating the right ascension coordinates and declination coordinates of the current moon according to a moon position formula, adjusting an equatorial telescope to enable the equatorial telescope to point to the moon, and obtaining the coordinates (cx, cy) of the spherical center image of the current moon by adopting a threshold segmentation method and a minimum circumcircle algorithm;
s6, calculating the center coordinates (cx, cy) of the current moon to the moon reference coordinates (cx)0,cy0) The offset of (2);
s7, correcting the right ascension coordinate orientation of the equatorial telescope according to the relation coefficient pra between the coordinate change value of the lunar centroid image and the change value of the right ascension coordinate and the longitudinal offset in the offsets obtained in the step S6;
correcting the declination coordinate orientation of the equatorial telescope according to the lunar centroid image coordinate change value and declination coordinate change value relation coefficient pdec and the transverse offset in the offset obtained in the step S6;
obtaining the coordinates (cx ', cy') of the moon centroid image at the moment;
s8, the moon image offset a at this time is obtained by:
Figure BDA0002653264320000021
judging whether the a is within a preset threshold value, if so, taking the right ascension coordinates and the declination coordinates of the equatorial telescope at the moment as the lunar actual coordinates, and synchronizing the internal coordinate system of the equatorial telescope; otherwise, the current moon centroid image coordinates (cx ', cy') are taken as the current moon centroid coordinates (cx, cy) in step S6, and steps S6-S8 are repeatedly performed until a is within the preset threshold.
Further, in step S2 and step S5, the threshold value is divided into 10% of the maximum gray-level value in the threshold value division method; the minimum circumcircle algorithm adopts a four-point iteration method.
Further, in step S3, the calculating step obtains that the moon moves from the upper edge to the lower edge of the finder mirror, and the relationship coefficient pra between the coordinate change value of the moon centroid image and the coordinate change value of the right ascension specifically is:
let the moon centroid image coordinate corresponding to the moon located at the upper edge of the finder as Centery1The coordinate of the right ascension is ra1(ii) a The corresponding moon centroid image coordinate is Center when the moon is positioned at the lower edge of the findery2The coordinate of the right ascension is ra2；
Calculating a relation coefficient pra of the coordinate change value of the lunar spherical center image and the coordinate change value of the right ascension according to the following formula:
Figure BDA0002653264320000031
further, in step S4, the calculating result shows that the moon moves from the left edge to the right edge of the finder mirror, and the relationship coefficient pdec between the coordinate variation of the moon centroid image and the variation of the declination coordinate is specifically:
let the moon centroid image coordinate corresponding to the moon located at the left edge of the finder be the Centerx1Declination coordinate is dec1(ii) a The corresponding moon centroid image coordinate is Center when the moon is positioned at the right edge of the star finderx2Declination coordinate is dec2；
Calculating a relation coefficient pdec between the coordinate change value of the moon spherical center image and the coordinate change value of declination according to the following formula:
Figure BDA0002653264320000032
further, step S7 is specifically:
let d be the longitude deviation of the current moon center coordinate from the reference moon coordinate of the finder moon obtained in step S6yCalculating the right ascension coordinate ra of the equatorial telescope needing to be corrected by the following formulay：
ray＝pra*dy；
The latitude deviation of the current moon center coordinate obtained in step S6 from the moon reference coordinate of the finder mirror is set asdxCalculating to obtain the declination coordinate dec of the equatorial instrument needing to be corrected by the following formulax：
decx＝pdec*dx。
Furthermore, synchronous motors are installed on the red warp shaft and the red weft shaft of the equatorial telescope.
Compared with the prior art, the invention has the beneficial effects that:
1. according to the equatorial telescope synchronization method for the ground-based moon observation, the lunar centroid is identified by the star finder in an image processing mode, the equatorial telescope can be synchronized without strictly aligning the slit type spectrometer with the star finder optical axis, and the lunar centroid can be accurately identified by the minimum circumcircle algorithm adopted for identifying the lunar centroid without being influenced by the lunar phase and judging the lunar phase; the equatorial telescope is synchronized through the lunar centroid position, extra star map data are not needed, and the synchronization method is accurate and simple.
2. The moon centroid recognition method adopts a four-point iteration minimum circumcircle algorithm, can more accurately confirm the moon shape, and further accurately recognize the moon centroid.
3. According to the invention, by respectively establishing the relationship between the lunar centroid and the right ascension coordinate and the relationship between the lunar centroid and the right ascension coordinate when the moon goes from the upper edge to the lower edge and from the left edge to the right edge of the finder, the right ascension coordinate and the right ascension coordinate in the internal coordinate system of the equatorial telescope are corrected during observation until the deviation meets the preset requirement, so that accurate observation can be met.
Drawings
FIG. 1 is a schematic structural diagram of a ground-based moon observation system in the background art
In FIG. 1, 01-slit spectrometer, 02-finder mirror, 03-equatorial, 04-industrial control computer.
FIG. 2 is a schematic flow chart of an embodiment of the method for synchronizing the equatorial telescope for ground-based lunar observation according to the present invention;
FIG. 3 is a spectral image of a slit spectrometer aligned to the moon according to an embodiment of the present invention;
FIG. 4 is a moon centroid image of a finder mirror according to an embodiment of the present invention;
FIG. 5 is a schematic diagram of a moon image moving from the upper edge to the lower edge of a finder mirror in an embodiment of the present invention;
FIG. 6 is a schematic diagram of a moon image moving from the left edge to the right edge of a finder mirror according to an embodiment of the present invention;
FIG. 7 is a diagram illustrating a moon image in the star finder calculated by a moon position formula during formal observation according to an embodiment of the present invention.
Detailed Description
The technical solution of the present invention will be clearly and completely described below with reference to the embodiments of the present invention and the accompanying drawings, and it is obvious that the described embodiments do not limit the present invention.
Therefore, the invention provides a synchronization method of a foundation moon observation equatorial telescope, which automatically synchronizes an equatorial telescope coordinate system before each moon data acquisition by means of a large-view-field finder, ensures the pointing accuracy of a spectrometer to the moon, and meets the requirement of foundation moon automatic observation. The method mainly comprises the steps of moon real-time image position identification, moon image position and alignment position offset calculation, lunar pointing correction in the right ascension direction, lunar pointing correction in the declination direction, and finally, synchronizing an equatorial telescope according to current lunar coordinates. The automatic synchronization method of the equatorial telescope for the moon observation of the foundation is realized, the accurate positioning and long-term stable tracking of the equatorial telescope for the moon are ensured, and the guarantee is provided for the automatic collection of the moon observation data.
As shown in fig. 2, the method specifically includes the following steps:
(1) before formal observation, initialization operation is performed, and the right ascension coordinate and the declination coordinate of the equatorial telescope are adjusted to enable the slit spectrometer to be aligned with the moon, for example, fig. 3 shows a spectrum image in the slit spectrometer, and at the moment, the spectrum image is located in the center and the width reaches the maximum.
(2) Obtaining the moon centroid image coordinates (cx) of the finder mirror at the moment shown in figure 4 by adopting a threshold segmentation method and a minimum circumcircle algorithm0,cy0) Setting the coordinate as a reference coordinate of the moon of the finder;
(3) as shown in fig. 5, the right ascension coordinates of the equatorial telescope are manually adjusted, so that the moon image moves from the upper edge to the lower edge of the finder, the moon centroid image coordinates and the right ascension coordinates corresponding to the moon located at the upper edge of the finder are obtained, and the moon centroid image coordinates and the right ascension coordinates corresponding to the moon located at the lower edge of the finder are obtained, and the relationship coefficient pra of the moon coordinate change value and the right ascension coordinate change value when the moon moves from the upper edge to the lower edge of the finder is obtained through calculation;
specifically, the method comprises the following steps: let the moon centroid image coordinate corresponding to the moon located at the upper edge of the finder as Centery1The coordinate of the right ascension is ra1(ii) a The corresponding moon centroid image coordinate is Center when the moon is positioned at the lower edge of the findery2The coordinate of the right ascension is ra2；
Calculating a relation coefficient pra of the coordinate change value of the lunar spherical center image and the coordinate change value of the right ascension according to the following formula:
Figure BDA0002653264320000051
(4) as shown in fig. 6, the declination coordinate of the equatorial telescope is manually adjusted, so that the moon image moves from the left edge to the right edge of the finder, the moon centroid image coordinate and the declination coordinate corresponding to the moon positioned at the left edge of the finder and the moon centroid image coordinate and the declination coordinate corresponding to the moon positioned at the right edge of the finder are obtained, and the relation coefficient pdec of the moon moving from the left edge to the right edge of the finder, the moon centroid image coordinate change value and the declination coordinate change value is calculated;
specifically, the method comprises the following steps: let the moon centroid image coordinate corresponding to the moon located at the left edge of the finder be the Centerx1Declination coordinate is dec1(ii) a The corresponding moon centroid image coordinate is Center when the moon is positioned at the right edge of the star finderx2Declination coordinate is dec2；
Calculating a relation coefficient pdec between the coordinate change value of the moon spherical center image and the coordinate change value of declination according to the following formula:
Figure BDA0002653264320000061
the initialization is completed.
(5) During formal observation, the current lunar right ascension coordinates and declination coordinates are calculated according to a lunar position formula each time, an equatorial telescope is adjusted to point to the moon, a lunar image in the finder is shown in figure 7, and a threshold segmentation method and a minimum circumcircle algorithm are adopted to obtain coordinates (cx, cy) of a current lunar center image; in the most preferable scheme, in the step (2) and the step (5), the division threshold in the threshold division method is 10% of the maximum gray value, the minimum circumscribed circle algorithm adopts a four-point iteration method, namely, the upper, lower, left and right boundary points are initially assumed to form a minimum circle, the iteration considers the conditions that other points are inside and outside the minimum circle to update four points, and finally, when all the points are in the minimum circle formed by the four points, the circle is the minimum circumscribed circle.
(6) Calculating the coordinate (cx, cy) of the center of the current moon relative to the reference coordinate (cx) of the moon of the finder0,cy0) The offset of (2);
(7) setting the longitude deviation of the current moon center coordinate obtained in the step (6) relative to the reference moon coordinate of the finder star as dyI.e. the longitudinal offset, the right ascension coordinate ra of the equatorial instrument to be corrected is calculated by the following formulay：
ray＝pra*dy；
Setting the latitude deviation of the current moon center coordinate obtained in the step (6) relative to the moon reference coordinate of the finder as dxI.e. the lateral offset, the declination coordinate dec of the equatorial telescope to be corrected is calculated by the following formulax：
decx＝pdec*dx。
Correcting the lunar orientation according to the equatorial coordinate orientation and the equatorial declination coordinate orientation to obtain a lunar centroid image coordinate (cx ', cy');
(8) the moon image shift a at this time is obtained by:
Figure BDA0002653264320000071
judging whether the a is within a preset threshold value, if so, considering that the lunar centroid is at the reference position, taking the right ascension coordinate and the declination coordinate of the equatorial telescope at the moment as the lunar actual coordinate, and synchronizing the internal coordinate system of the equatorial telescope; otherwise, the current moon centroid image coordinates (cx ', cy') are taken as the current moon centroid coordinates (cx, cy) in step S6, and steps S6-S8 are repeatedly performed until a is within the preset threshold.
Wherein, the equatorial telescope can adopt the equatorial telescope of 50kg of maximum load, and synchronous machine is all installed to polar axis and declination axle, can realize biax automatic control. The equatorial instrument can be controlled to be synchronous and directional by inputting absolute coordinates of right ascension and declination by adopting an ascom standard astronomy interface.
The inventive equatorial telescope synchronization method for ground-based moon observation can be used for carrying out moon observation at a certain night to realize automatic moon observation all the night.
And performing initialization operation before observation, and controlling a slit type spectrometer carried by an equatorial instrument to be aligned with the moon, wherein the alignment is already indicated when a spectrum image of the moon is positioned in the middle and has the maximum width. The moon image in the large view field star finder at the moment is subjected to a threshold segmentation method and a minimum circumcircle algorithm to obtain the moon centroid image coordinates (cx) in the star finder at the moment0,cy0)＝(450，213)。
Manually adjusting the right ascension coordinates of the equatorial telescope to enable the moon image in the star finder to move from the upper edge to the lower edge of the star finder to obtain the corresponding moon centroid image coordinate Center when the moon is positioned at the upper edge of the star findery130 in the right ascension coordinate ra14.1859, and a moon centroid image coordinate Center corresponding to the moon located at the lower edge of the finder mirrory2526, right ascension coordinate ra21.3527, by:
Figure BDA0002653264320000072
calculating to obtain a relation coefficient pra of the coordinate change value of the lunar centroid image and the coordinate change value of the right ascension between the lunar moving from the upper edge to the lower edge of the finder mirror to be-5.7121 e-3。
Then manually adjusting the declination coordinate of the equatorial telescope to enable the moon image to be from the left side of the finderThe edge is moved to the right edge to obtain the corresponding moon centroid image coordinate Center when the moon is positioned at the left edge of the star finderx145, corresponding to declination coordinate dec126.5873, and the corresponding moon centroid image coordinate Center when the moon is at the right edge of the finder mirrorx2739, the corresponding declination coordinate dec2-4.2146, prepared by:
Figure BDA0002653264320000073
calculating the relation coefficient pdec between the coordinate variation value of the moon centroid image and the variation value of declination coordinate as-4.4383 e when the moon moves from the left edge to the right edge of the finder mirror-2At this point, preparation before observation is completed.
And during the N-th observation, calculating the right ascension coordinate and the declination coordinate of the current moon according to a moon position formula, adjusting the equatorial telescope to enable the equatorial telescope to point to the moon to obtain a moon image in the large-field finder at the moment, and obtaining the coordinates (cx, cy) of the moon centroid image at the moment by adopting a threshold segmentation method and a minimum circumcircle algorithm (296,218). Then, the moon centroid coordinate (cx, cy) at the moment is calculated relative to the moon reference coordinate (cx)0,cy0) Offset amount of (2):
dx＝cx-cx0＝-154；dy＝cy-cy0＝5；
the equatorial ascension coordinates are corrected by:
ray＝pra*dy
obtaining the right ascension coordinate ra of the equatorial telescope needing to be correctedy＝-2.8561e-2；
Correcting the declination coordinate of the equatorial telescope by:
ray＝pra*dy
obtaining the declination coordinate dec of the equatorial telescope needing to be correctedx＝6.8350；
Correcting the directions of the right ascension coordinates and the declination coordinates of the equatorial telescope, pointing again, then adopting a threshold segmentation method and a minimum circumcircle algorithm again to obtain the coordinates (cx ', cy') (451,212) of the lunar centroid image in the finder mirror at the moment,
by:
Figure BDA0002653264320000081
the obtained moon image offset a at this time is 1.414, and the preset threshold is 3, wherein the setting of the preset threshold can be adjusted and determined according to the actual observation precision requirement. In the embodiment, the situation that the moon in the finder is located at the reference position and meets the precision requirement is explained, the right ascension coordinate and the declination coordinate of the equatorial telescope at the moment are taken as the actual coordinates of the moon, the internal coordinate system of the automatic synchronous equatorial telescope is adjusted, and the purpose of automatically synchronizing the equatorial telescope before data collection of the moon is achieved.
The above description is only an embodiment of the present invention, and is not intended to limit the scope of the present invention, and all equivalent structural changes made by using the contents of the present specification and the drawings, or applied directly or indirectly to other related technical fields, are included in the scope of the present invention.

Claims (6)

1. A synchronization method for a foundation-to-moon observation equatorial telescope is characterized by comprising the following steps:
s1, adjusting the right ascension coordinate and the declination coordinate of the equatorial telescope to enable the slit type spectrometer to be aligned with the moon;
s2, obtaining the coordinates (cx) of the moon centroid image in the finder mirror at the moment by adopting a threshold segmentation method and a minimum circumcircle algorithm0,cy0) Setting the coordinate as the moon reference coordinate of the finder mirror;
s3, adjusting the right ascension coordinates of the equatorial telescope to enable the moon image to move from the upper edge to the lower edge of the finder, obtaining the moon centroid image coordinates and right ascension coordinates corresponding to the moon positioned at the upper edge of the finder, and the moon centroid image coordinates and right ascension coordinates corresponding to the moon positioned at the lower edge of the finder, and calculating to obtain the relation coefficient pra of the moon moving from the upper edge to the lower edge of the finder, the moon centroid image coordinate change value and the right ascension coordinate change value;
s4, adjusting the declination coordinate of the equatorial telescope to enable the moon image to move from the left edge to the right edge of the finder mirror, obtaining the moon centroid image coordinate and the declination coordinate corresponding to the moon located at the left edge of the finder mirror, and the moon centroid image coordinate and the declination coordinate corresponding to the moon located at the right edge of the finder mirror, and calculating the relation coefficient pdec of the moon moving from the left edge to the right edge of the finder mirror, and the moon centroid image coordinate change value and the declination coordinate change value;
s5, during observation, calculating the right ascension coordinates and declination coordinates of the current moon according to a moon position formula, adjusting an equatorial telescope to enable the equatorial telescope to point to the moon, and obtaining the coordinates (cx, cy) of the spherical center image of the current moon by adopting a threshold segmentation method and a minimum circumcircle algorithm;
s6, calculating the center coordinates (cx, cy) of the current moon to the moon reference coordinates (cx)0,cy0) The offset of (2);
s7, correcting the right ascension coordinate orientation of the equatorial telescope according to the relation coefficient pra between the coordinate change value of the lunar centroid image and the change value of the right ascension coordinate and the longitudinal offset in the offsets obtained in the step S6;
correcting the declination coordinate orientation of the equatorial telescope according to the lunar centroid image coordinate change value and declination coordinate change value relation coefficient pdec and the transverse offset in the offset obtained in the step S6;
obtaining the coordinates (cx ', cy') of the moon centroid image at the moment;
s8, the moon image offset a at this time is obtained by:
Figure FDA0002653264310000011
judging whether the a is within a preset threshold value, if so, taking the right ascension coordinates and the declination coordinates of the equatorial telescope at the moment as the lunar actual coordinates, and synchronizing the internal coordinate system of the equatorial telescope; otherwise, the current moon centroid image coordinates (cx ', cy') are taken as the current moon centroid coordinates (cx, cy) in step S6, and steps S6-S8 are repeatedly performed until a is within the preset threshold.
2. The method for synchronizing the geosynchronous lunar observers according to claim 1, wherein: in step S2 and step S5, the threshold value is 10% of the maximum gray-level value in the threshold value division method; the minimum circumcircle algorithm adopts a four-point iteration method.
3. The method for synchronizing the geosynchronous lunar observers according to claim 1, wherein: in step S3, the calculation result shows that the moon moves from the upper edge to the lower edge of the finder mirror, and the relationship coefficient pra between the coordinate change value of the lunar centroid image and the coordinate change value of the right ascension specifically is:
let the moon centroid image coordinate corresponding to the moon located at the upper edge of the finder as Centery1The coordinate of the right ascension is ra1(ii) a The corresponding moon centroid image coordinate is Center when the moon is positioned at the lower edge of the findery2The coordinate of the right ascension is ra2；
Calculating a relation coefficient pra of the coordinate change value of the lunar spherical center image and the coordinate change value of the right ascension according to the following formula:
Figure FDA0002653264310000021
4. the method for synchronizing the geosynchronous lunar observers according to claim 1, wherein: in step S4, the calculation result shows that the moon moves from the left edge to the right edge of the finder mirror, and the relationship coefficient pdec between the coordinate change value of the lunar centroid image and the change value of the declination coordinate specifically includes:
let the moon centroid image coordinate corresponding to the moon located at the left edge of the finder be the Centerx1Declination coordinate is dec1(ii) a The corresponding moon centroid image coordinate is Center when the moon is positioned at the right edge of the star finderx2Declination coordinate is dec2；
Calculating a relation coefficient pdec between the coordinate change value of the moon spherical center image and the coordinate change value of declination according to the following formula:
Figure FDA0002653264310000022
5. the method for synchronizing the geosynchronous lunar observers according to claim 1, wherein: step S7 specifically includes:
let d be the longitude deviation of the current moon center coordinate from the reference moon coordinate of the finder moon obtained in step S6yCalculating the right ascension coordinate ra of the equatorial telescope needing to be corrected by the following formulay：
ray＝pra*dy；
Let d be the latitude deviation of the current moon center coordinate from the reference moon coordinate of the finder moon obtained in step S6xCalculating to obtain the declination coordinate dec of the equatorial instrument needing to be corrected by the following formulax：
decx＝pdec*dx。
6. The method for synchronizing the geosynchronous lunar observers according to claim 1, wherein: synchronous motors are arranged on the red warp shaft and the red weft shaft of the equatorial telescope.
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