초록 ▼

A method for measuring a precision of a star sensor and a system using the same may be provided. The method may comprise steps of: 1) fixing the star sensor on the Earth; 2) inputting a current time (T) of a measuring start time relative to a J2000.0 time; 3) determining a directional vector of the

A method for measuring a precision of a star sensor and a system using the same may be provided. The method may comprise steps of: 1) fixing the star sensor on the Earth; 2) inputting a current time (T) of a measuring start time relative to a J2000.0 time; 3) determining a directional vector of the navigation star in a J2000.0 Cartesian coordinate system at the current time (T) according to a right ascension and a declination of the navigation star in the J2000.0 Cartesian coordinate system and visual movement parameters (α′, δ′) of the navigation star in the direction of the right ascension and the declination which are stored in the star sensor; 4) converting the directional vector of the navigation star in the J2000.0 Cartesian coordinate system into a directional vector of the navigation star in an ecliptic coordinate system; 5) converting the directional vector of the navigation star in the ecliptic coordinate system into a directional vector (vCRFT) of the navigation star in a celestial coordinate system; and 6) converting the directional vector (vCRFT) of the navigation star in the celestial coordinate system into a directional vector (vTRF) of the navigation star in a terrestrial coordinate system, and obtaining the precision of the star sensor based on the directional vector (vTRF) of the navigation star in the terrestrial coordinate system.

대표청구항 ▼

1. A method for measuring a precision of a star sensor, comprising steps of: 1) fixing the star sensor on the Earth so as to point a main axis of the star sensor towards the zenith, the star sensor being inputable with time parameters which is stored with a navigation star catalog and visual movemen

1. A method for measuring a precision of a star sensor, comprising steps of: 1) fixing the star sensor on the Earth so as to point a main axis of the star sensor towards the zenith, the star sensor being inputable with time parameters which is stored with a navigation star catalog and visual movement parameters associated with a navigation star in the navigation star catalog;2) inputting a current time (T) of a measuring start time relative to a J2000.0 time;3) determining a directional vector of the navigation star in a J2000.0 Cartesian coordinate system at the current time (T) according to a right ascension and a declination (α, δ) of the navigation star in the J2000.0 Cartesian coordinate system and visual movement parameters (α′, δ′) of the navigation star in the direction of the right ascension and the declination which are stored in the star sensor;4) converting the directional vector of the navigation star in the J2000.0 Cartesian coordinate system at the current time (T) into a directional vector of the navigation star in an ecliptic coordinate system;5) converting the directional vector of the navigation star in the ecliptic coordinate system into a directional vector (vCRFT) of the navigation star in a celestial coordinate system at the current time (T); and6) converting the directional vector (vCRFT) of the navigation star in the celestial coordinate system at the current time (T) into a directional vector (vTRF) of the navigation star in a terrestrial coordinate system at an actual shooting time (T+Δt) according to the actual shooting time (T+Δt), and obtaining the precision of the star sensor based on the directional vector (vTRF) of the navigation star in the terrestrial coordinate system. 2. The method according to claim 1, wherein in the step 3), the directional vector (vCRFJ2000) of the navigation star in the J2000.0 Cartesian coordinate system at the current time (T) is as follows: vCRFJ⁢⁢2000=[cos⁡(α+α′⁢T)⁢cos⁡(δ+δ′⁢T)sin⁡(α+α′⁢T)⁢cos⁡(δ+δ′⁢T)sin⁡(δ+δ′⁢T)]. 3. The method according to claim 2, wherein in the step 4), the directional vector (vERF) of the navigation star in the ecliptic coordinate system is acquired by rotating the J2000.0 Cartesian coordinate system around an X axis of the J2000.0 Cartesian coordinate system counterclockwise through 23° 26′21″ based on the directional vector (vCRFJ2000) of the navigation star in the J2000.0 Cartesian coordinate system: vERF=Rx(23°26′21″)vCRFJ2000. 4. The method according to claim 3, wherein converting the directional vector (vERF) of the navigation star in the ecliptic coordinate system into the directional vector (vCRFT) of the navigation star in the celestial coordinate system at the current time (T) is obtained by: rotating the directional vector (vERF) of the navigation star in the ecliptic coordinate system around a Z axis thereof clockwise through 50.29″×T;rotating the obtained vector of the navigation star around an X axis of a coordinate system after the first rotating clockwise through 23°26′21″;rotating the obtained vector of the navigation star around an X axis of a coordinate system after the second rotating counterclockwise through εA;rotating the obtained vector of the navigation star around a Z axis of a coordinate system after the third rotating clockwise through Δφ; androtating the obtained vector of the navigation star around an X axis of a coordinate system after the fourth rotating clockwise through εA+Δε, to obtain the directional vector (vCRFT) of the navigation star in the celestial coordinate system at the current time (T) containing nutation terms, wherein the Δφ and Δε represent a nutation in longitude and an oblique nutation respectively. 5. The method according to claim 4, wherein the directional vector (vCRFT) of the navigation star in the celestial coordinate system is acquired by following formulas: vCRFT=RX(−(εA+Δε))RZ(−Δφ)RX(εA)RX(−23 °26′21″)RZ(−50.29″×T)RX(23°26′21″)vCRFJ2000,where RX and RZ are coordination transformation bases. 6. The method according to claim 5, wherein according to the IAU2000B nutation model, εA, the nutation in longitude (Δφ) and the oblique nutation (Δε) are obtained by following formulas respectively: ɛA=ɛ0-46.84024″⁢t-0.00059″⁢t2+0.001813″⁢t3Δ⁢⁢φ=Δ⁢⁢φP+∑i=177⁢[(Ai⁢⁢1+Ai⁢⁢2⁢t)⁢sin⁢⁢αi+Ai⁢⁢3⁢cos⁢⁢αi]Δ⁢⁢ɛ=Δ⁢⁢ɛP+∑i=177⁢[(Ai⁢⁢4+Ai⁢⁢5⁢t)⁢sin⁢⁢αi+Ai⁢⁢6⁢cos⁢⁢αi⁢]where ΔφP=−0.135 m(″), ΔεP=0.388 m(″), ε0=84381.448″, t is a Julian century number starting from J2000.0 and is obtained based on the current time (T); andan argument αi is a linear combination of arguments which is determined as follows: αi=⁢∑k=15⁢nik⁢Fk=⁢ni⁢⁢1⁢l+ni⁢⁢2⁢l′+ni⁢⁢3⁢F+ni⁢⁢4⁢D+ni⁢⁢5⁢Ωwhere nik, is an integer, and Fk is a Delaunay argument related to positions of the Sun and the Moon. 7. The method according to claim 1, wherein the step 6) further comprises: (61) converting the directional vector (vCRFT) of the navigation star in the celestial coordinate system at the current time (T) into the directional vector (vTRF) of the navigation star in the terrestrial coordinate system at the actual shooting time (T+Δt) according to the actual shooting time (T+Δt);(62) solving an optimal attitude matrix (Aq(T+Δt)) of the star sensor by the QUEST method according to the directional vector (vTRF) of the navigation star in the terrestrial coordinate system;(63) calculating a pointing vector (p(T+Δt)) of the main axis of the star sensor at the actual shooting time (T+Δt); and(64) calculating an angle (αij) of the pointing vectors (p(T+Δt)) of the main axis of the star sensor at the actual shooting time (T+Δt) to obtain a pointing precision of the star sensor. 8. The method according to claim 7, wherein the directional vector (vTRF) of the navigation star in the terrestrial coordinate system is obtained by rotating the directional vector (vCRFT) of the navigation star in the celestial coordinate system around a Z axis of the celestial coordinate system counterclockwise at an angular velocity Ω of 7.292115×10−5 rad/s: vTRF=RZ(ΩΔt)RX(−(εA+Δε))RZ(−Δφ)RX(εA)RX(−23°26′21″)RZ(−50.29″×T)RX(23°26′21″)vCRFJ2000. 9. The method according to claim 8, wherein the optimal attitude matrix (Aq(T+Δt)) is obtained by minimizing a following objective function J(Aq(T+Δt): J⁡(Aq⁡(T+Δ⁢⁢t))=12⁢∑i=1n⁢αi⁢wi-Aq⁡(T+Δ⁢⁢t)⁢vi2where wi, vi represent a directional vector of the navigation star in a star sensor coordinate system and a directional vector of the navigation star in the terrestrial coordinate system respectively, αi represents a weighing coefficient, and Σαi=1. 10. The method according to claim 9, wherein the pointing vector (p(T+Δt)) of the main axis of the star sensor is as follows: p⁡(T+Δ⁢⁢t)=Aq⁡(T+Δ⁢⁢t)⁡[001], and the angle (αij) of the pointing vectors (p(T+Δt)) of the main axis of the star sensor is as follows: αij=a cos(p(T+Δti)T·p(T+Δtj)). 11. A system for measuring a precision of a star sensor, the star sensor comprising a navigation star catalogue comprising a navigation star and visual movement parameters associated with the navigation star, and a time input interface for inputting a measuring start time, the system comprising: a fixing device for fixing the star sensor on the Earth so as to point a main axis of the star sensor towards the zenith; anda star sensor precision measurement unit for measuring the precision of the star sensor, wherein a current time (T) of the measuring start time relative to a J2000.0 time is input through the time input interface, a directional vector of the navigation star in a J2000.0 Cartesian coordinate system at the current time (T) is determined according to a right ascension and a declination (α, δ) of the navigation star in the J2000.0 Cartesian coordinate system and visual movement parameters (α′, δ′) of the navigation star in the direction of the right ascension and the declination which are stored in the star sensor, the directional vector of the navigation star in the J2000.0 Cartesian coordinate system at the current time (T) is converted into a directional vector of the navigation star in an ecliptic coordinate system, the directional vector of the navigation star in the ecliptic coordinate system is converted into a directional vector (vCRFT) of the navigation star in a celestial coordinate system at the current time (T), the directional vector (vCRFT) of the navigation star in the celestial coordinate system at the current time (T) is converted into a directional vector (vTRF) of the navigation star in a terrestrial coordinate system at an actual shooting time (T+Δt) according to the actual shooting time (T+Δt), and the precision of the star sensor is obtained based on the directional vector (vTRF) of the navigation star in the terrestrial coordinate system. 12. The system according to claim 11, wherein the star sensor precision measurement unit further comprises: a Cartesian coordinate directional vector acquiring module for acquiring the directional vector (vCRFJ2000) of the navigation star in the J2000.0 Cartesian coordinate system at the current time (T) by the following formula: vCRFJ⁢⁢2000=[cos⁡(α+α′⁢T)⁢cos⁡(δ+δ′⁢T)sin⁡(α+α′⁢T)⁢cos⁡(δ+δ′⁢T)sin⁡(δ+δ′⁢T)]. 13. The system according to claim 12, wherein the star sensor precision measurement unit further comprises: an ecliptic coordinate system directional vector acquiring module for acquiring the directional vector (vERF) of the navigation star in the ecliptic coordinate system by rotating the J2000.0 Cartesian coordinate system around an X axis of the J2000.0 Cartesian coordinate system counterclockwise through 23°26′21″ based on the directional vector (vCRFJ2000) of the navigation star in the J2000.0 Cartesian coordinate system: vERF=RX(23°26′21″)vCRFJ2000. 14. The system according to claim 13, wherein the star sensor precision measurement unit further comprises: a celestial coordinate system directional vector acquiring module for converting the directional vector (vERF) of the navigation star in the ecliptic coordinate system into the directional vector (vCRFT) of the navigation star in the celestial coordinate system at the current time (T) by:rotating the directional vector (vERF) of the navigation star in the ecliptic coordinate system around a Z axis thereof clockwise through 50.29″×T;rotating the obtained vector of the navigation star around an X axis of a coordinate system after the first rotating clockwise through 23°26′21″;rotating the obtained vector of the navigation star around an X axis of a coordinate system after the second rotating counterclockwise through εA;rotating the obtained vector of the navigation star around a Z axis of a coordinate system after the third rotating clockwise through Δφ; androtating the obtained vector of the navigation star around an X axis of a coordinate system after the fourth rotating clockwise through εA+Δε, to obtain the directional vector (vCRFT) of the navigation star in the celestial coordinate system at the current time (T) containing nutation terms, whereinthe Δφ and Δε represent a nutation in longitude and an oblique nutation respectively. 15. The system according to claim 14, wherein the celestial coordinate system directional vector acquiring module is configured to acquire the directional vector (vCRFT) of the navigation star in the celestial coordinate system by following formulas: vCRFT=RX(−(εA+Δε))RZ(−Δφ)RX(εA)RX(−23°26′21″)RZ(−50.29″×T)RX(23°26′21″)vCRFJ2000,where RX and RZ are coordination transformation bases. 16. The system according to claim 15, wherein according to the IAU2000B nutation model, εA, the nutation in longitude (Δφ) and the oblique nutation (Δε) are respectively as follows: ɛA=ɛ0-46.84024″⁢t-0.00059″⁢t2+0.001813″⁢t3Δ⁢⁢φ=Δ⁢⁢φP+∑i=177⁢[(Ai⁢⁢1+Ai⁢⁢2⁢t)⁢sin⁢⁢αi+Ai⁢⁢3⁢cos⁢⁢αi]Δ⁢⁢ɛ=Δ⁢⁢ɛP+∑i=177⁢[(Ai⁢⁢4+Ai⁢⁢5⁢t)⁢sin⁢⁢αi+Ai⁢⁢6⁢cos⁢⁢αi⁢]where ΔφP=−0.135 m(″), ΔεP=0.388 m(″), ε0=84381.448″, t is a Julian century number starting from J2000.0 and is obtained based on the current time (T); andan argument αi is a linear combination of arguments which is determined as follows: αi=⁢∑k=15⁢nik⁢Fk=⁢ni⁢⁢1⁢l+ni⁢⁢2⁢l′+ni⁢⁢3⁢F+ni⁢⁢4⁢D+ni⁢⁢5⁢Ωwhere nik, is an integer, and Fk is a Delaunay argument related to positions of the Sun and the Moon. 17. The system according to claim 16, wherein the star sensor precision measurement unit is configured to: convert the directional vector (vCRFT) of the navigation star in the celestial coordinate system at the current time (T) into the directional vector (vTRF) of the navigation star in the terrestrial coordinate system at the actual shooting time (T+Δt) according to the actual shooting time (T+Δt);solve an optimal attitude matrix (Aq(T+Δt)) of the star sensor by the QUEST method according to the directional vector (vTRF) of the navigation star in the terrestrial coordinate system;calculate a pointing vector (p(T+Δt)) of the main axis of the star sensor at the actual shooting time (T+Δt), andcalculate an angle (αij) of the pointing vectors (p(T+Δt)) of the main axis of the star sensor at the actual shooting time (T+Δt) to obtain a pointing precision of the star sensor. 18. The system according to claim 17, wherein the star sensor precision measurement unit further comprises: a terrestrial coordinate system directional vector acquiring module for acquiring the directional vector (vTRF) of the navigation star in the terrestrial coordinate system by rotating the directional vector (VCRFT) of the navigation star in the celestial coordinate system around a Z axis of the celestial coordinate system counterclockwise at an angular velocity Ω of 7.292115×10−5 rad/s: vTRF=RZ(ΩΔt)(−(εA+Δε))RZ(−Δφ)RX(εA)RX(−23°26′21″)RZ(−50.29″×T)RX(23°26′21″)vCRFJ2000. 19. The system according to claim 18, wherein the optimal attitude matrix (Aq(T+Δt)) is obtained by minimizing a following objective function J⁡(Aq⁡(T+Δ⁢⁢t))=12⁢∑i=1n⁢αi⁢wi-Aq⁡(T+Δ⁢⁢t)⁢vi2where wi, vi represent a directional vector of the navigation star in a star sensor coordinate system and a directional vector of the navigation star in the terrestrial coordinate system respectively, αi represents a weighing coefficient, and Σαi=1. 20. The system according to claim 19, wherein the pointing vector (p(T+Δt)) of the main axis of the star sensor is as follows: p⁡(T+Δ⁢⁢t)=Aq⁡(T+Δ⁢⁢t)⁡[001], and the angle (αij) of the pointing vectors (p(T+Δt)) of the main axis of the star sensor is as follows: αij=a cos(p(T+Δti)T·p(T+Δtj)),where i≠j.