CN202885806U - Multifunctional astronomical theodolite - Google Patents

Abstract

The utility model provides a multifunctional astronomical theodolite, belongs to the technical field of an astrometric instrument and solves the problems of an axis collimation system in a low-latitude meridian circle that the structure is complicated and a data processing period is long. The multifunctional astronomical theodolite comprises a longitude and latitude base and a reflection telescope; a left horizontal axis and a right horizontal axis are respectively mounted on a left fork arm and a right fork arm; an upper disc is sleeved on an azimuth axis of a middle disc; an axis end of the azimuth axis is provided with an azimuth coded disc; the back end of the reflection telescope is provided with a micrometer dial with a CCD (Charge Coupled Device) camera; the left horizontal axis is provided with a coded disc No.1 and the right horizontal axis is provided with a coded disc No.2; the coded discs No.1and the No.2 are annular grating angle encoders; and the outer sides of the coded discs No.1 and the No.2 are respectively provided with two pairs of reading heads which are in diameter orthogonal distribution. According to the multifunctional astronomical theodolite disclosed by the utility model, a jerk value of each axis end can be solved by eccentric errors of each coded disc, the measurement efficiency of oscillating quantity of a height axis is improved and the detection structure is simple.

Description

Multifunctional astronomical theodolite

Technical Field

The utility model belongs to the technical field of celestial body measuring instrument, in particular to a theodolite for celestial body is measured.

Background

In optical celestial measuring instruments, a meridian ring is used to determine the coordinates of the stars and a reference system is established on the celestial sphere. The celestial globe, the prism contour gauge, the photoelectric contour gauge, the photographing zenith cylinder, the zenith gauge and the like are used for measuring world time or polar motion and provide earth rotation parameters for scientific research and national defense construction. They all obtain desired measurement results by measuring the position of the celestial body with reference to a plumb line or a mercury surface.

The foreign meridian ring is an astronomical instrument special for measuring the position of a star and establishing an celestial sphere reference system, which is invented by Denmark astronomical Rome in 1689, and then is assisted by German astronomical Meier to perfect the precision of theoretically measuring the position of the star to 2 arc seconds. In 1839, the russian astronomy stebruvit establishes the principle of absolute determination of celestial body position in the newly-built platform, and after gradually raising strict requirements for instrument manufacturing and gradually introducing auxiliary equipment and technology, the measurement accuracy is gradually improved to 0.4 arc second in the middle of the 20 th century.

The original meridian ring is a refraction telescope with the caliber of 15-20 cm and the focal length of 2.0-2.5 m, and is supported in V-shaped grooves on two side foundation piers through pivots at the ends of left and right horizontal shafts at the middle section of the lens barrel, and a vertical dial is arranged on the horizontal shaft close to the lens barrel. The instrument has a large volume, uses an optical dial as an angle measuring reference, has very high processing precision requirement, and can be observed visually. And the original observation method can only be used for observation in high-latitude areas. At the end of the 20 th century, a low latitude meridian ring was successfully developed by the Yunnan astronomical stage, and the absolute determination of the celestial body position in low latitude areas was realized by adopting an original observation principle and method. The low latitude meridian ring adopts a reflection telescope, an optical dial is used as a main reference for angle measurement, a linear array CCD is used as a photoelectric measuring element, a pivot is still used, and a gear transmission mechanism is adopted.

Because the low latitude meridian ring uses the optical scale to measure the angle, the swing of its horizontal axis line has adopted the axis collimation system to measure, the axis collimation system structure is complicated, the data processing cycle is long.

Disclosure of Invention

For solving the problem that the axle alignment system structure that is used for measuring the swing of high axle axis is complicated, data processing cycle length in current low latitude meridian ring, the utility model provides a multi-functional astronomical theodolite, its technical scheme as follows:

the multifunctional astronomical theodolite comprises a theodolite base and a reflecting telescope arranged on the theodolite base;

the reflecting telescope is arranged on a middle block between a left horizontal shaft and a right horizontal shaft of the longitude and latitude seat, shaft heads of the left horizontal shaft and the right horizontal shaft are respectively arranged on a left fork arm and a right fork arm on the upper disc, the upper disc is sleeved on an azimuth shaft on the middle disc, an azimuth coded disc is arranged on the shaft end of the azimuth shaft, a plane bearing is arranged between the upper disc and the middle disc, the middle disc is arranged on a supporting seat on the bottom disc, and the bottom disc is arranged on a foundation pier;

a vertical worm wheel is arranged on the left horizontal shaft or the right horizontal shaft close to the middle block, the vertical worm wheel is meshed with a worm, and the worm is connected with a servo motor through a transmission system;

a micrometer with a CCD camera is arranged at the rear end of the reflecting telescope;

the shaft heads of the left horizontal shaft and the right horizontal shaft are cylindrical and are respectively arranged on deep groove ball bearings arranged on the left fork arm and the right fork arm;

a first code disc is arranged on the left horizontal shaft, a second code disc is arranged on the right horizontal shaft, and the first code disc and the second code disc are both annular grating angle encoders;

two pairs of reading heads which are distributed in a diameter-matching orthogonal mode are arranged on a left fork arm positioned on the outer side of a dial, and the reading heads A are respectively arranged clockwise₁、B₁、C₁、D₁Wherein the reading head A₁Is positioned at the top in the vertical direction, the included angle between two adjacent reading heads is 90 degrees, and the reading head A₁、C₁Is arranged in a diameter-matching way and a reading head B₁、D₁Is arranged in a diameter-matching way and is provided with a reading head A₁、C₁The connecting line and the reading head B₁、D₁The connecting lines of (A) are orthogonal;

two pairs of reading heads which are distributed in a diameter-matching orthogonal mode are arranged on a right fork arm positioned on the outer side of a second code disc and are respectively a reading head A in a clockwise arrangement mode₂、B₂、C₂、D₂Wherein the reading head A₂Is positioned at the top in the vertical direction, the included angle between two adjacent reading heads is 90 degrees, and the reading head A₂、C₂Is arranged in a diameter-matching way and a reading head B₂、D₂Is arranged in a diameter-matching way and is provided with a reading head A₂、C₂The connecting line and the reading head B₂、D₂The connecting lines of (a) are orthogonal.

The method for detecting the shaft end deflection of the height shaft by using the multifunctional astronomical theodolite comprises the following sequential steps:

step 1, installing a detection device:

installing a first dial, a second dial and corresponding reading heads;

step 2, collecting the difference of the readings of each pair of diameter reading heads when the telescope points at each preset zenith distance i, and establishing a regression model of the difference of the readings of each preset zenith distance i and each pair of diameter reading heads, wherein the regression model comprises the following steps:

step 2.1: rotating an azimuth code wheel of the theodolite to 0 degree, arranging a height shaft along the east-west direction, and enabling a first code wheel to be located at the west end of the height shaft and a second code wheel to be located at the east end of the height shaft;

step 2.2: rotating the height axis along the meridian direction by the same rotation angle step pitch to make the telescope point at a plurality of preset zenith distances with the same interval, and collecting the reading head A when the telescope points at each preset zenith distance i₁、C₁Difference between readings (A)₁-C₁)_iReading head B₁、D₁Difference between readings (B)₁-D₁)_iReading head A₂、C₂Difference between readings (A)₂-C₂)_iReading head B₂、D₂Difference between readings (B)₂-D₂)_i；

Step 2.3: all preset zenith distances i and (A)₁-C₁)_iSubstituted into the following equation 1:

equation 1: (A)₁-C₁)_i＝ΔA₀₁+2r_C11sin(a_C11+i)+v_i；

V in the above formula_iIs a random error, and the parameter Delta A is calculated from the above formula by the least square method₀₁、r_C11And a_C11Wherein, Δ A₀₁Representative diameter reading head A₁、C₁Zero-offset of the difference between readings of (a);

step 2.4: all preset zenith distances i and (B)₁-D₁)_iSubstituted into the following equation 2:

equation 2: (B)₁-D₁)_i＝ΔB₀₁+2r_C12sin(a_C12+i+90°)+v_i；

V in the above formula_iIs a random error, and the parameter Delta B is calculated from the above formula by the least square method₀₁、r_C12And a_C12Wherein, Δ B₀₁Representative diameter reading head B₁、D₁Zero-offset of the difference between readings of (a);

get r_C1＝(r_C11+r_C12) [ 2 ] r in the formula_C1Representing the amplitude of a periodic eccentricity error sinusoid of a dial;

get a_C1＝(a_C11+a_C12) /2, a in the formula_C1Representing the initial phase of a periodic eccentric error sine curve of a code disc;

step 2.5: all preset zenith distances i and (A)₂-C₂)_iSubstituted into the following equation 3:

equation 3: (A)₂-C₂)_i＝ΔA₀₂+2r_C21sin(a_C21+i)+v_i；

V in the above formula_iIs a random error, and the parameter Delta A is calculated from the above formula by the least square method₀₂、r_C21And a_C21Wherein, Δ A₀₂Representative diameter reading head A₂、C₂Zero-offset of the difference between readings of (a);

step 2.6: all preset zenith distances i and (B)₂-D₂)_iSubstituted into the following equation 4:

equation 4: (B)₂-D₂)_i＝ΔB₀₂+2r_C22sin(a_C22+i+90°)+v_i；

V in the above formula_iIs a random error, and the parameter Delta B is calculated from the above formula by the least square method₀₂、r_C22And a_C22Wherein, Δ B₀₂Representative diameter reading head B₂、C₂Zero-offset of the difference between readings ofA difference;

get r_C2＝(r_C21+r_C22) [ 2 ] r in the formula_C2Representing the amplitude of a periodic eccentric error sine curve of a second code disc;

get a_C2＝(a_C21+a_C22) /2, a in the formula_C2Representing the initial phase of the periodic eccentric error sine curve of the second code disc;

step 3, measuring and calculating the deflection of the shaft end of the height shaft in real time when observing the star to be measured:

step 3.1: rotating an azimuth code wheel of the theodolite to 0 degree, arranging a height shaft along the east-west direction, and enabling a first code wheel to be located at the west end of the height shaft and a second code wheel to be located at the east end of the height shaft;

step 3.2: rotating the height axis along the meridian direction to make the telescope point to the star to be measured with zenith distance z, and collecting the reading head A₁、C₁Difference between readings (A)₁-C₁)_zReading head B₁、D₁Difference between readings (B)₁-D₁)_zReading head A₂、C₂Difference between readings (A)₂-C₂)_iReading head B₂、D₂Difference between readings (B)₂-D₂)_iRespectively substituted into the following equations 5 to 8, and Δ a obtained by the solution in step 2 is calculated₀₁、ΔB₀₁、r_C1And a_C1And Δ A₀₂、ΔB₀₂、r_C2And a_C2Substituted into the following equations 5-8:

equation 5:

equation 6:

equation 7:

equation 8:

respectively solved by the above formulaAnd

wherein,

and

respectively the north and upward offset of the west end of the height axis when observing the star body to be measured,

andrespectively the south-facing offset and the upward offset of the east end of the height axis when observing the star to be detected;

get

The deflection of the east end of the height axis relative to the west end in the north-south direction when the star to be measured is observed;

get

The upward deflection of the east end of the height axis relative to the west end of the height axis is observed when the star body to be measured is observed.

In the above method, the preset zenith distance i in step 2 may be an integer value angle with a step distance between-75 ° and 75 ° being 1 °.

In the above method, the upward offset refers to an offset in a direction opposite to the gravity direction, such as:

for observing the upward offset of the west end of the height axis when the star to be measured is measured, the meaning is

The offset of the west end of the height axis in the direction opposite to the gravity direction when observing the star body to be measured.

The utility model discloses an at the both ends of high axle, respectively set up a high steel band code wheel, digit angle encoder promptly, and the reading head that two pairs of quadrature diameter distributions, by the change of each code wheel eccentric error, the change of the difference between the two reading head readings of diameter promptly, solve out the direction and the quantity value of beating that each axle head arouses by the shafting error respectively, and then solve out the direction and the quantity value of the real-time beat of high axle in the observation process, thereby substitute an axle collimator, because the measuring result of grating code wheel is the digital quantity, consequently, high axis oscillating quantity measuring efficiency has been improved greatly, and it is simpler to detect the structure. Originally, a shaft alignment system is adopted to measure the shaft line swing to obtain an analog image, and then digital processing is carried out to obtain a digital signal. The resulting images were observed every night, which took 4 hours to process. After the double-code disc is adopted for detection, the swing parameters can be obtained in real time, and even real-time measurement is realized.

There is the ruling error in the position code wheel of solving current astronomical theodolite, influences the problem of observing the precision, the utility model provides a device is corrected in multi-functional astronomical theodolite position code wheel ruling, its technical scheme as follows:

two pairs of reading heads which are distributed in a diameter-matching orthogonal mode are mounted on the upper disc along the periphery of the azimuth code disc, and the included angle between every two adjacent reading heads is 90 degrees.

The method for correcting the scribing of the azimuth code wheel by using the multifunctional astronomical theodolite comprises the following steps in sequence:

step 1: installing equipment:

a reading head is arranged on an upper disc at the periphery of the azimuth code disc;

selecting a plurality of fixed stars i to be detected, and observing and calculating each fixed star i to be detected according to the following steps 2 to 6;

step 2: acquiring an initial value t of the star crossing recording moment of the star i to be detected₀：

Selecting one fixed star i to be measured, firstly rotating an azimuth code disc of a theodolite to an azimuth angle A, exposing the star i to be measured for 6 seconds by using a CCD camera at the 12 second moment before the star i to be measured passes through a perpendicular line in a telescope view field of the theodolite, then rotating a theodolite base of the theodolite around an azimuth axis within 12 seconds, rotating the azimuth code disc to the azimuth angle A +180 degrees, rotating a telescope around a horizontal axis, wherein the rotating angle is twice the zenith distance of the fixed star i to be measured, pointing the telescope to the fixed star i to be measured again and exposing light for 6 seconds, and calculating the initial star crossing record value t of the fixed star i to be measured by using the following formula₀：

t₀＝(t^(A)+t^(A+180°))/2+Δx·k/cosδ；

In the above formula, t^(A)Representing the star image exposure time t of the fixed star i to be measured when the azimuth code disc rotates to the azimuth A^{(A，A+180°)}Representing the star image exposure time of the fixed star i to be detected when the azimuth code disc rotates to an azimuth angle A +180 degrees, delta x representing the difference between the star image positions of the fixed star i to be detected on the target surface of the CCD camera when the azimuth code disc rotates to the azimuth angle A and the azimuth angle A +180 degrees respectively, k representing the pixel scale of the CCD camera of the main optical path system, and delta representing the apparent declination of the fixed star i to be detected;

and step 3: calculating the theoretical satellite-passing time t by the following formula₁：

${\mathrm{<figure-callout\; id="1"\; label="t"\; filenames="HDA00002202402600012.png"\; state="\{\{state\}\}">t</figure-callout>}}_1=\mathrm{\&alpha;}\stackrel{\&OverBar;}{+}{\mathrm{<figure-callout\; id="2"\; label="t"\; filenames="HDA00002202402600011.png,HDA00002202402600021.png"\; state="\{\{state\}\}">t</figure-callout>}}_2;$

In the above formula, the first and second carbon atoms are,

in the above formula, the first and second carbon atoms are,

in the above formula, α represents the visual declination of the fixed star i to be measured, t₂Represents an included angle between the right ascension circle and the meridian circle, namely a time angle, q represents an azimuth angle formed between the right ascension circle of the fixed star i to be detected and the horizontal longitude circle of the azimuth angle A,

representing a local latitude adopted value, and delta represents the apparent declination of the fixed star i to be detected;

and 4, step 4: the deviation Δ a of the actual orientation from the nominal orientation at the moment of observation is calculated by the following formula:

ΔA＝-cosδ cosq cscz Δt；

in the formula, δ represents the apparent declination of the fixed star i to be detected, q represents the star position angle formed between the right ascension circle of the fixed star i to be detected and the horizontal ascension circle of the azimuth angle A, and z represents the zenith distance of the fixed star i to be detected;

in the above formula, Δ t is t₀-t₁；

And 5: calculating the average value theta of the orientation code disc reading when the front and the back of the rotating shaft are observed by the following formula:

θ＝(θ^(A)+θ^(A+180°)-180°)/2；

in the above formula, θ^(A)RepresentsWhen the azimuth code disk rotates to the azimuth angle A, the average value theta of the readings of the four reading heads on the periphery of the azimuth code disk^(A+180°)Representing the average value of the readings of four reading heads on the periphery of the azimuth code disc when the azimuth code disc rotates to an azimuth angle A +180 degrees;

step 6: substituting the delta A in the step 4 and the theta in the step 5 into the following formula to calculate the corrected reading A of the azimuth code disc when the azimuth code disc rotates to the azimuth angle A_i：

A_i＝ΔA+θ；

And 7: taking A of all fixed stars i to be measured_iThe arithmetic mean value of the values is the corrected reading A of the azimuth code disc when the azimuth code disc of the theodolite rotates to the azimuth angle A^(A)。

The above-mentioned azimuth angle a may be 45 °, 90 °, or 135 °.

Utilize the utility model discloses correct the device, can detect and correct astronomical theodolite position code wheel ruling error portably, realize the improvement of instrument observation precision, mainly do the correction to the ruling error of code wheel, take Renilshao's annular grating encoder as an example, the ruling precision of the product of its 200mm diameter is about 0.9 ", adopt this method should improve to about 0.1", make the reading of position code wheel more reliable.

As the preferred scheme of the utility model:

the axle body of the left horizontal shaft between the left fork arm and the middle block is in a circular truncated cone shape, and the axle body of the right horizontal shaft between the right fork arm and the middle block is in a circular truncated cone shape. This structure is intended to give it equal stiffness properties, with the aim of using less material to obtain greater stiffness.

As the preferred scheme of the utility model:

the reflection telescope is a Cassegrain telescope and comprises a main mirror and an auxiliary mirror, an auto-collimation plane mirror is arranged on a lens cone between the main mirror and the auxiliary mirror, the normal line of the auto-collimation plane mirror is parallel to the optical axis of the main mirror, a CCD camera is arranged at the position of the auxiliary mirror focus at the rear end of a central hole of the main mirror, a semi-reflection semi-transmission mirror is arranged between the main mirror and the CCD camera, a slit plate is arranged on the optical axis of reflected light of the semi-reflection semi-transmission mirror, and an optical hole is formed in the slit plate.

The working process of the self-collimating plane mirror is as follows: a bulb is arranged behind a slit plate, light rays emitted by the bulb form a 1-point light source after passing through the slit plate, parallel light is formed after being reflected by a semi-reflecting and semi-transparent mirror, a secondary mirror and a main mirror, the parallel light is reflected by an auto-collimation plane perpendicular to an optical axis, and imaging is carried out on a focal plane of the main mirror, namely a photosensitive surface of a CCD photoelectric device after passing through the semi-reflecting and semi-transparent mirror. Due to the influence of gravity, when the telescope points to different heights, the primary mirror and the secondary mirror of the telescope can slightly deflect relative to the middle block, so that the optical axis of the main optical path deflects relative to the middle block, namely relative to the auto-collimation plane mirror, and the position of a point image on the CCD photosensitive surface moves.

As the preferred scheme of the utility model:

the front end and the rear end of the right fork arm are respectively provided with an electric level, the electric level comprises a collimator tube and a mercury disc, the collimator tube is vertically downward and is arranged on the right fork arm, and the mercury disc is arranged on an upper disc below the collimator tube;

the collimating tube is sequentially provided with a CCD camera, a semi-reflecting and semi-transmitting mirror and a collimating mirror from top to bottom along an optical axis, a light source slit plate is arranged on the optical axis of reflected light of the semi-reflecting and semi-transmitting mirror, three rows of light holes are formed in the light source slit plate, and three light holes are formed in each row.

The operation of the above electrical level is as follows: the light emitted from the light source slit plate forms a 3 x 3 point light source, and after passing through the half-reflecting and half-transmitting mirror and the collimating mirror, parallel light is formed, the parallel light is reflected by the mercury reflecting surface of the mercury disk perpendicular to the optical axis, and then passes through the half-reflecting and half-transmitting mirror, and forms an image on the photosensitive surface of the CCD camera on the focal plane of the collimating mirror, when the upper disk of the instrument drives the whole part above the upper disk of the instrument to tilt, the optical axis of the collimating tube represents the gravity direction relative to the mercury reflecting surface, which can be regarded as unchanged and slightly deflected, so that the position of a point image array formed on the CCD photosensitive surface changes. The electric water level substantially adopts a mercury surface to replace an auto-collimation plane mirror, and the electric water level is characterized in that: the amount of tilt can be detected by autocollimation measurements when the telescope is slightly tilted relative to the mercury surface, which is usually the same.

The utility model discloses multi-functional astronomical theodolite is a small-size, light, full-automatic celestial body measuring instrument that has multiple functions, and it is the small-size reflection telescope that has multiple error measuring device, and it can alternately survey in arbitrary a plurality of equipartition position to can survey in real time and eliminate the various error instantaneous values of instrument.

The multifunctional astronomical theodolite can be used for measuring astronomical longitude and latitude, extracting clean and reliable information of abnormal change of the plumb line direction, and extracting earthquake precursor information through a triangular monitoring network of abnormal change of the plumb line; meanwhile, the method is used for conventionally providing high-precision world time and latitude measurement values for reconstructing the earth rotation parameter ground optical measurement system in China; the device can also measure instantaneous astronomical atmospheric refraction in a plurality of uniformly distributed directions, establish a local multi-azimuth astronomical atmospheric refraction actual measurement model and an atmospheric refraction delay correction actual measurement model, eliminate various system errors caused by atmospheric factors in the change of plumb lines, be favorable for matching with GPS measurement, and be used as a measuring instrument produced by the requirements of relevant departments for establishing the local atmospheric refraction model in the future; in addition, according to the feasibility of the current pre-research, the device can also monitor the ground inclination around the fixed observation station for a long time, and acquire all-weather plumb line change images through the coordination of astronomical observation and non-astronomical observation of the device.

In the aspect of instrument structure, compared with a low latitude meridian ring, the low latitude meridian ring is improved in many aspects, and mainly comprises the following components: an annular grating encoder (annular grating for short) is adopted to replace an optical dial for controlling the rotation angle of an instrument and measuring the rotation angle with high precision, so that the digitization of angle measurement is realized, and the measurement precision is improved; the electric water level system adopts an area array CCD to replace a linear array CCD as a detector, and adopts a porous star point plate to replace a slit plate; the deflection of the height shaft is detected by adopting the two height code discs, so that the measurement automation is realized, the measurement precision is improved, and the precision requirement on machining is reduced.

Drawings

Fig. 1 is a front view of the multifunctional astronomical theodolite of the present invention;

FIG. 2 is a view of the reading head A of FIG. 1₁、B₁、C₁、D₁A projection diagram on a dial in the W direction;

FIG. 3 is a view of the reading head A of FIG. 1₂、B₂、C₂、D₂A projection schematic diagram on a second dial in the E direction;

FIG. 4 is a schematic diagram showing four diametrically orthogonal readheads mounted along the periphery of the azimuth code wheel of FIG. 1;

FIG. 5 is an optical path diagram of the telescope of FIG. 1;

fig. 6 is a light path diagram of the electrical levels in fig. 1.

Detailed Description

The multifunctional astronomical theodolite as shown in fig. 1 comprises a theodolite base and a reflecting telescope 8 arranged on the theodolite base;

the reflection telescope 8 is arranged on a middle block 9 between a left horizontal shaft 5 and a right horizontal shaft 6 of the longitude and latitude seat, shaft heads of the left horizontal shaft 5 and the right horizontal shaft 6 are respectively arranged on a left fork arm 3 and a right fork arm 4 on an upper disc 20, the upper disc 20 is sleeved on an azimuth shaft 15 on a middle disc 19, an azimuth coded disc 16 is arranged on the shaft end of the azimuth shaft 15, a plane bearing 13 is arranged between the upper disc 20 and the middle disc 19, the middle disc 19 is arranged on a supporting seat 14 on a base disc 18, and the base disc 18 is arranged on a foundation pier 17;

a vertical worm wheel 11 is arranged on the left horizontal shaft 5 or the right horizontal shaft 6 close to the middle block 9, the vertical worm wheel 11 is meshed with a worm, and the worm is connected with a servo motor through a transmission system;

a micrometer with a CCD camera is arranged at the rear end of the reflecting telescope 8;

the shaft heads of the left horizontal shaft 5 and the right horizontal shaft 6 are cylindrical and are respectively arranged on deep groove ball bearings 7 arranged on the left fork arm 3 and the right fork arm 4;

a first number disk 1 is arranged on the left horizontal shaft 5, a second number disk 2 is arranged on the right horizontal shaft 6, and the first number disk 1 and the second number disk 2 are both annular grating angle encoders;

as shown in figure 2, two pairs of reading heads which are distributed in a radial orthogonal way are arranged on a left fork arm 3 positioned outside a dial 1 and are respectively a reading head A in a clockwise arrangement₁、B₁、C₁、D₁Wherein the reading head A₁Is positioned at the top in the vertical direction, the included angle between two adjacent reading heads is 90 degrees, and the reading head A₁、C₁Is arranged in a diameter-matching way and a reading head B₁、D₁Is arranged in a diameter-matching way and is provided with a reading head A₁、C₁The connecting line and the reading head B₁、D₁The connecting lines of (A) are orthogonal;

as shown in figure 3, two pairs of reading heads which are distributed in a radial orthogonal way are arranged on the right fork arm 4 positioned outside the second code disc 2 and are respectively a reading head A in a clockwise arrangement₂、B₂、C₂、D₂Wherein the reading head A₂Is positioned at the top in the vertical direction, the included angle between two adjacent reading heads is 90 degrees, and the reading head A₂、C₂Is arranged in a diameter-matching way and a reading head B₂、D₂Is arranged in a diameter-matching way and is provided with a reading head A₂、C₂The connecting line and the reading head B₂、D₂The connecting lines of (a) are orthogonal.

As shown in FIG. 4, two pairs of reading heads 12 are arranged on the upper disc 20 along the periphery of the azimuth code disc 16 in a diametrically orthogonal manner, and the included angle between two adjacent reading heads 12 is 90 degrees.

As shown in fig. 1, the shaft body of the left horizontal shaft 5 between the left yoke 3 and the middle block 9 is in a circular truncated cone shape, and the shaft body of the right horizontal shaft 6 between the right yoke 4 and the middle block 9 is in a circular truncated cone shape.

As shown in fig. 5, the reflection telescope 8 is a cassegrain telescope, and includes a main mirror 23 and a secondary mirror 24, an auto-collimation plane mirror 25 is arranged on a lens barrel between the main mirror 23 and the secondary mirror 24, a normal line of the auto-collimation plane mirror 25 is parallel to an optical axis of the main mirror 23, a CCD camera 28 is arranged at a secondary mirror focus at a rear end of a central hole of the main mirror 23, a half-reflecting and half-transmitting mirror 26 is arranged between the main mirror 23 and the CCD camera 28, a slit plate 27 is arranged on an optical axis of reflected light of the half-reflecting and half-transmitting mirror 26, and an optical hole is arranged on the slit plate 27.

As shown in fig. 1, an electric level is respectively installed at the front end and the rear end of the right yoke 4, the electric level comprises a collimator 22 and a mercury disc 21, the collimator 22 is vertically downward and is installed on the right yoke 4, and the mercury disc 21 is arranged on an upper disc 20 below the collimator 22;

as shown in fig. 6, the collimator 22 is provided with a CD camera 29, a half-reflecting and half-transmitting mirror 30 and a collimator 31 from top to bottom along an optical axis, a light source slit plate 32 is provided on the optical axis of the reflected light of the half-reflecting and half-transmitting mirror 30, three rows of light holes are provided on the light source slit plate 32, and three light holes are provided on each row.

Claims (5)

1. The multifunctional astronomical theodolite comprises a theodolite base and a reflecting telescope (8) arranged on the theodolite base;

the reflection telescope (8) is arranged on a middle block (9) between a left horizontal shaft (5) and a right horizontal shaft (6) of the longitude and latitude seat, shaft heads of the left horizontal shaft (5) and the right horizontal shaft (6) are respectively arranged on a left fork arm (3) and a right fork arm (4) on an upper disc (20), the upper disc (20) is sleeved on an azimuth shaft (15) on a middle disc (19), an azimuth coded disc (16) is arranged at the shaft end of the azimuth shaft (15), a plane bearing (13) is arranged between the upper disc (20) and the middle disc (19), the middle disc (19) is arranged on a supporting seat (14) on a chassis (18), and the chassis (18) is arranged on a foundation pier (17);

a vertical worm wheel (11) is arranged on the left horizontal shaft (5) or the right horizontal shaft (6) close to the middle block (9), the vertical worm wheel (11) is meshed with a worm, and the worm is connected with a servo motor through a transmission system;

the method is characterized in that:

a micrometer with a CCD camera is arranged at the rear end of the reflecting telescope (8);

the shaft heads of the left horizontal shaft (5) and the right horizontal shaft (6) are cylindrical and are respectively arranged on deep groove ball bearings (7) arranged on the left fork arm (3) and the right fork arm (4);

a first number disk (1) is arranged on the left horizontal shaft (5), a second number disk (2) is arranged on the right horizontal shaft (6), and the first number disk (1) and the second number disk (2) are both annular grating angle encoders;

two pairs of reading heads which are distributed in a diameter-matching orthogonal way are arranged on a left fork arm (3) positioned on the outer side of a dial (1) and are respectively a reading head A according to clockwise arrangement₁、B₁、C₁、D₁Wherein the reading head A₁Is positioned at the top in the vertical direction, the included angle between two adjacent reading heads is 90 degrees, and the reading head A₁、C₁Is arranged in a diameter-matching way and a reading head B₁、D₁Is arranged in a diameter-matching way and is provided with a reading head A₁、C₁The connecting line and the reading head B₁、D₁The connecting lines of (A) are orthogonal;

two pairs of reading heads which are distributed in a diameter-matching orthogonal way are arranged on a right fork arm (4) positioned on the outer side of the second code disc (2), and the reading heads A are respectively arranged clockwise₂、B₂、C₂、D₂Wherein the reading head A₂Is positioned at the top in the vertical direction, the included angle between two adjacent reading heads is 90 degrees, and the reading head A₂、C₂Is arranged in a diameter-matching way and a reading head B₂、D₂Is arranged in a diameter-matching way and is provided with a reading head A₂、C₂The connecting line and the reading head B₂、D₂Is connected withAre orthogonal.

2. The multi-functional astronomical theodolite of claim 1, wherein:

two pairs of reading heads (12) which are distributed in a diameter-to-diameter orthogonal mode are mounted on an upper disc (20) along the periphery of an azimuth coded disc (16), and an included angle between every two adjacent reading heads (12) is 90 degrees.

3. Multifunctional astronomical theodolite according to claim 1 or 2, wherein:

the shaft body of the left horizontal shaft (5) between the left fork arm (3) and the middle block (9) is in a circular truncated cone shape, and the shaft body of the right horizontal shaft (6) between the right fork arm (4) and the middle block (9) is in a circular truncated cone shape.

4. The multi-functional astronomical theodolite of claim 3, wherein:

the telescope reflector (8) is a Cassegrain telescope and comprises a main mirror (23) and an auxiliary mirror (24), wherein an auto-collimation plane mirror (25) is arranged on a lens cone between the main mirror (23) and the auxiliary mirror (24), the normal line of the auto-collimation plane mirror (25) is parallel to the optical axis of the main mirror (23), a CCD camera (28) is arranged at the auxiliary mirror focus position at the rear end of a central hole of the main mirror (23), a semi-reflecting and semi-transmitting mirror (26) is arranged between the main mirror (23) and the CCD camera (28), a slit plate (27) is arranged on the optical axis of reflected light of the semi-reflecting and semi-transmitting mirror (26), and an optical hole is formed in the slit plate (27).

5. The multi-functional astronomical theodolite of claim 4, wherein:

the front end and the rear end of the right fork arm (4) are respectively provided with an electric level, the electric level comprises a collimator (22) and a mercury disc (21), the collimator (22) is vertically downward and is arranged on the right fork arm (4), and the mercury disc (21) is arranged on an upper disc (20) positioned below the collimator (22);

the collimating tube (22) is internally provided with a CCD camera (29), a semi-reflecting and semi-transmitting mirror (30) and a collimating mirror (31) from top to bottom along an optical axis in sequence, a light source slit plate (32) is arranged on the optical axis of reflected light of the semi-reflecting and semi-transmitting mirror (30), and a plurality of light holes are formed in the light source slit plate (32).

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