CN102879013B - Method for correcting influences of atmosphere inclination on ground star observation values - Google Patents
Method for correcting influences of atmosphere inclination on ground star observation values Download PDFInfo
- Publication number
- CN102879013B CN102879013B CN201210366902.8A CN201210366902A CN102879013B CN 102879013 B CN102879013 B CN 102879013B CN 201210366902 A CN201210366902 A CN 201210366902A CN 102879013 B CN102879013 B CN 102879013B
- Authority
- CN
- China
- Prior art keywords
- star
- fixed star
- isodensity
- value
- sample fixed
- Prior art date
- Legal status (The legal status is an assumption and is not a legal conclusion. Google has not performed a legal analysis and makes no representation as to the accuracy of the status listed.)
- Active
Links
Abstract
A method of incline star observation value inclined to the ground of amendment atmosphere influences, influence for observing the astronomical longitude and latitude measured value that the sidereal time obtains on the ground is tilted for correcting atmosphere, belong to uranometry technical field, solves the problems, such as existing Correction for atmospheric refractive error inaccuracy, the following steps are included: step 1, several fixed stars are chosen as sample fixed star, establish sample fixed star
Regression model between each observation calculates the inclined influence amount of atmosphere isodensity layer as caused by the factors such as meteorology variation in every group of star observation; Step 2, star observation value is corrected according to the inclined resolving amount of atmosphere isodensity layer. The method of the present invention accurately can observe the apparent zenith distance measured value obtained to every star and the star overwriting moment makees the inclined amendment of atmosphere isodensity layer, improves the measurement accuracy of uranometry and geodetic instrument.
Description
Technical field
The invention belongs to uranometry technical field, particularly air isodensity layer modification method that fixed star is measured.
Background technology
When light is dredged and propagated in lower close air in density, can there is the phenomenon of flexion in path.In astrometry field, atmospheric refraction refers in particular to radiation that celestial body sends at the refraction effect produced through earth atmosphere, and the change in the astronomical observation direction of being caused by above-mentioned phenomenon.Its knots modification is called that atmospheric refraction affects, also referred to as atmospheric refraction.It has impact to radar fix, Doppler range rate measurement, communication, navigation.The precision of the result such as angle on target, distance, height measured in these work is all subject to the impact of atmospheric refraction.Atmospheric refraction impact can calculate according to atmospheric strument and obtain roughly, and this impact is also called refraction correction.
Before and after B.C. 2nd century, the Bo Xidongniwusi of Greece has just found atmospheric refraction phenomenon, recognizes that atmospheric refraction affects the accuracy of large measurement result.2nd century of the Christian era large astronomer Tuo Lemi of Greece further discuss atmospheric refraction problem in his works " optics " the 5th volume.Tuo Lemi, by the observation repeatedly to star place, finds the effect due to atmospheric refraction, the astrology position close to Horizon is raised to some extent.The reason of Tuo Lemi light refraction has set forth this phenomenon theoretically.In 16th century, large astronomer's tycho of Denmark also possesses some special knowledge to atmospheric refraction phenomenon, and he determines atmospheric refraction value.First the astronomer G.D. Cassini of France then establishes atmospheric refraction theory according to the law of sines in the 17th century.Some other famous astronomer, as the newton of Britain, Bradley obtain thunder, the people such as Laplce of France possesses some special knowledge to atmospheric refraction.The twenties in 19th century, astronomer's Bezier of Germany established the logarithmic formula calculating atmospheric refraction, had worked out the quite accurate Refraction Tables of portion.Within 1870, pul Ke Wo astronomical observatory of Russia has worked out a Refraction Tables, is still widely used so far.
Generally carry out atmospheric refraction calculating or when setting up atmospheric refraction model, assuming that atmospheric envelope is concentric spherical layering.Because this hypothesis can not describe atmospheric time of day completely, make Correction for atmospheric refractive error have inaccuracy, namely there is residual error in refraction correction.
Summary of the invention
For the atmospheric hypothesis solving existing concentric spherical layering can not describe atmospheric time of day completely, refraction correction is made to have inaccuracy, namely there is the problem of residual error in refraction correction, the invention provides a kind of method tilted to star observation value correction atmospheric envelope, its technical scheme is as follows:
Revise atmospheric envelope to tilt on a method for ground star observation value impact, it is characterized in that comprising the following steps:
Step 1, choose some fixed stars as sample fixed star i, use astronomical theodolite observation sample fixed star i, the telescope instrument of described astronomical theodolite is provided with CCD camera, the altitude axis of described astronomical theodolite is provided with height code-disc, for measuring the zenith distance of sample fixed star i; Set up the regression model between each observed reading of sample fixed star i that obtained by astronomical theodolite, calculate and change by meteorology the influence amount of air isodensity layer inclination to every sample fixed star i caused, comprise the following steps:
Step 1.1: the apparent declination δ gathering every sample fixed star i
i, the zenith distance reading z of height code-disc
i, the star image position finding value y in y direction on CCD camera target surface
i, the level error error of astronomical theodolite when measuring every sample fixed star i, optical axis point to the survey latitude component sum of variation error, altitude axis Run-out error and code-disc groove graduation error
and the adopted lattide of measuring station
substitute in following formula 1:
Formula 1:
In above formula
be stochastic error, represent the survey latitude residual error of every sample fixed star i, include the impact that air isodensity layer tilts on fixed star i measured value,
for target surface star image surveys the scale-up factor of latitude,
for the arithmetic mean of instantaneous latitude value and the adopted lattide of measuring station of whole sample fixed star i
difference, calculate by least square method
with every sample fixed star i's
Step 1.2: gather every sample fixed star i and do not considering that the star under the various error of astronomical theodolite and atmospheric envelope inclination conditions crosses moment calculated value T
i, star record value t at out-of-date quarter
i, the star image position finding value x in x direction on CCD camera target surface
i, and the level error error of astronomical theodolite when measuring every sample fixed star i, optical axis point to the survey real component sum (e of variation error, altitude axis Run-out error and code-disc groove graduation error
t)
i, substitute in following formula 2:
Formula 2:T
i=t
i+ k
tx
i+ (e
t)
i+ Δ λ+v
t(z
i);
V in above formula
t(z
i) be stochastic error, represent the time-measuring residual of every sample fixed star i, include the impact that air isodensity layer tilts on fixed star i measured value, k
tfor scale-up factor when target surface star image is surveyed, Δ λ is the arithmetic mean of the instantaneous longitude value of whole sample fixed star i and calculating T
itime measuring station adopted logitude λ
0difference, calculate the v of Δ λ and every sample fixed star i by least square method
t(z
i);
Step 1.3: by every sample fixed star i's calculating in step 1.1
and the zenith distance reading z of the height code-disc of every the sample fixed star i collected
i, substitute in following formula 3:
Formula 3:
From above formula, parameter Δ z is calculated by least square method
n, Δ z
nfor being changed the air isodensity layer that the causes tilt quantity along North and South direction by meteorology, if air isodensity layer northwards tilts, Δ z
nfor on the occasion of, if the south dip of air isodensity layer, then Δ z
nfor negative value;
Step 1.4: by the v of every sample fixed star i calculated in step 1.2
t(z
i), and the apparent declination δ of every the sample fixed star i collected
i, the zenith distance reading z of height code-disc
i, substitute in following formula 4:
Formula 4: Δ z
e=15v
t(z
i) cos δ
icos z
i/ (A sin 1 ");
From above formula, parameter Δ z is calculated by least square method
e, Δ z
efor meteorology changes the air isodensity layer tilt quantity eastwards caused;
Step 2, revise star observation value according to air isodensity layer tilt quantity, comprise the following steps:
Step 2.1: air isodensity layer step 1.3 calculated is along the tilt quantity Δ z of North and South direction
n, and the apparent zenith distance z of the fixed star to be measured obtained is observed by astronomical theodolite, substitute into following formula 5, calculate the true zenith distance Z of fixed star to be measured:
Formula 5:Z=z+A tan z+A × Δ z
n× sec
2z;
Step 2.2: the air isodensity layer tilt quantity Δ z eastwards that step 1.4 is calculated
e, and observe the fixed star to be measured obtained cross meridian moment t, the apparent zenith distance z of fixed star to be measured by astronomical theodolite, substitute in following formula 6, calculate fixed star to be measured and cross meridian correction moment T:
Formula 6:T=t+ Δ z
e× A/cos z;
A in above-mentioned steps 1.3, step 1.4, step 2.1 and step 2.2 represents the coefficient of the first term of atmospheric refraction series model.
In such scheme, described atmospheric refraction series model refers to:
A tan z-B tan
3z+C tan
5z-D tan
7z+…；
Z in above formula is apparent zenith distance, about three orders of magnitude less of A of the coefficient B due to Section 2, after every coefficient C, D etc. less, therefore, Data processing coefficient B here, C, D are all omitted.
As preferred version of the present invention:
A in described step 1.3, step 1.4, step 2.1 and step 2.2 is 60 " .2.
In such scheme, some fixed stars selected in step 1 can be the fixed stars in observational program.
The present invention proposes, air non-homogeneous concentric shell structure, but in some areas due to the change of meteorological condition, have the inclination of isodensity layer, namely refer to Air Close To The Earth Surface isodensity layer and ground level not parallel, its normal and the intersection point of celestial sphere be not at zenith, but hypothesis is at zenith north distance zenith Δ z
nplace, namely isodensity layer has small angle compared with even concentric shell.The existence of this angle, will the Fixed Initial Point of the zenith distance adopted in atmospheric refraction model be made to there occurs change, the refraction correction value calculated also exists the System level gray correlation changed with zenith distance.Therefore be necessary this angle to measure, revise atmospheric refraction calculated value.
Correction atmospheric refraction calculated value of the present invention, tilting with the simplest North and South direction to tilt on the impact in the star overwriting moment of meridian direction observation for foundation on the impact of meridian direction zenith distance measured value and east-west direction, perceives and solve more exactly meteorologically to change the tilt quantity Δ z that the air isodensity layer caused is tilted in both direction in the adjustment of observation
nwith Δ z
e.There is Δ z
nwith Δ z
e, the apparent zenith distance measured value that just can obtain every star observation respectively and star overwriting moment do the correction that air isodensity layer tilts, and improve the measuring accuracy of uranometry and geodetic instrument.
The inventive method is the accuracy of observation in order to improve the instrument newly developed, particularly the partner of cross discipline requires that measurement data is totally reliable, by the knowledge accumulation of oneself and forefathers, comprise the understanding to the air temperature and air pressure distribution plan analyzing weather situation in weather forecast, and the measurement data analyzing forefathers can not reach clean reason reliably, and a kind of new method proposed, it is a kind of one of new method got rid of atmospheric effect, improve accuracy of observation, and drafting of method is that too busy to get away starlight produces the bending natural law by atmospheric envelope.Its computing method are only for this new method is served.
Accompanying drawing explanation
Fig. 1 is true zenith, refraction zenith and tested star are the schematic diagram of the narrow right angle spherical triangle on summit.
Embodiment
The true zenith distance Z of the tested star of meridian direction is defined as: instantaneous latitude
deduct the apparent declination δ of tested star, that is:
like this, the just given sign of zenith distance: being just on the south zenith, is negative to the north of zenith.Observe the difference between apparent zenith distance z and true zenith distance Z obtained be instantaneous astronomy tide value R, and have: Z=z+R.
Here clearly several concept first: true zenith distance Z calculates, apparent zenith distance z observes the measured value obtained.The star catalogue of celestial body calculates position (referring to right ascension and declination respectively), i.e. apparent place is by star catalogue epoch (such as B2000.0) mean place, add the precession of the equinoxes, nutating and voluntarily, aberration, annual parallax etc. correct.
The series statement calculating atmospheric refraction value is:
R=A tan z-B tan
3z+C tan
5z-D tan
7z+……，
Coefficient B in formula three orders of magnitude less of coefficient A, coefficient is below less.This is forefathers conclude the out expression formula meeting the atmospheric refraction model of the natural law through studying for a long period of time.So-called " instantaneous astronomy tide value ", refer to the coefficient A of Section 1 in model, must be adopt the observation transient temperature T in moment and instantaneous air pressure P to make revised numerical value, because the atmospheric density of ground floor is along with this atmospheric latitude, air pressure and changing.Get A
0for standard ambient condition, (temperature is 0 ° of C, air pressure is 760 millimeter of mercuries or 1013.25 millibars) under the value of A, namely the model value of giving is (before Modling model, under instantaneous atmospheric refraction measured value will being converted to unified standard ambient condition), have according to Gay-Lussac's law and Boyle law:
Barometer reading in formula is respectively in units of millimeter of mercury or millibar.Due to B value 3 orders of magnitude less of A value, after everyly can not to revise.Preferably direct temperature, air pressure correction are done to R:
R
0for the value of R under standard ambient condition.These correction formulas embody: along with the increase of air pressure, and atmospheric density increases, by the increase of refractive index, instantaneous atmospheric refraction value is caused to increase, on the contrary, along with the rising of temperature, atmospheric density reduces, and by the reduction of refractive index, causes instantaneous atmospheric refraction value to reduce.
Here the meteorology considered changes the air isodensity layer caused and tilts, only the inclination of instantaneous air isodensity layer relative to the quiet Atmospheric models in this locality (corresponding with local atmospheric refraction model), or the average magnitude that one group of star observation time is tilted, tilting as the air isodensity layer caused by local geographical environment, being excluded when adopting the apparent zenith distance measured value of local atmospheric refraction Model Measured to every star to do astronomy tide correction.Because the Section 1 in atmospheric refraction model is dominant term, the several order of magnitude larger than other several, consider to tilt affect time also only need consider Section 1.
If the tilt quantity northwards that the air isodensity layer that meteorological change causes is tilted in meridian direction is Δ z
n, the zenith point namely calculating astronomy tide moves Δ z northwards
n.Air isodensity layer mentioned here northwards tilts on meridian direction, refer to Air Close To The Earth Surface isodensity layer and ground level not parallel, its normal and the intersection point of celestial sphere not at zenith, but hypothesis on the zenith north apart from zenith Δ z
nplace, pedal line does not change.This point is only when calculating refraction correction value, as the Fixed Initial Point of the zenith distance of argument, so that the tested star to the north of zenith, the zenith distance calculating refraction correction value used reduces Δ z
n, on the south zenith, add Δ z
n.
Be z for zenith distance on the south zenith
ithe observation of tested star, the Section 1 of Refraction Corrections should be A
stan (z
i+ Δ z
n), (get the Section 1 coefficient of local atmospheric refraction model, on the south zenith He to the north of zenith, be respectively A
sand A
n), because do not know Δ z
nexistence, the Section 1 of actual corrected value is only A
stan z
i, according to approximate formula tan (the z+ Δ z recorded in " mathematics handbook "
n)=tan z+ Δ z
n× sec
2z, can draw following formula:
A tan(z+Δz
n)=A tan z+A×Δz
n×sec
2z
Obtaining the approximate value that this phenomenon makes apparent zenith distance measured value reduce is:
A
stan(z
i+Δz
n)-A
stan z
i=A
s×Δz
n×sec
2z
i，
Apparent zenith distance measured value mentioned here reduces, because true zenith distance is constant, the apparent zenith distance obtained is observed to add that Refraction Corrections value equals true zenith distance, because zenith northwards offsets, the atmospheric refraction value in observation zenith south star moment is large, the apparent zenith distance obtained is observed just to have diminished, in addition, because instantaneous latitude measured value is
this also makes the instantaneous latitude measured value observing this star obtain reduce A
s× Δ z
n× sec
2z
i.
Be z for zenith distance to the north of zenith
jthe observation of tested star, the Section 1 of Refraction Corrections should be A
ntan (z
j+ Δ z
n), z
jfor negative value, Δ z
nfor rotating forward value, (z
j+ Δ z
n) absolute value diminish, reduction is also negative value, and its absolute value also diminishes, and makes the absolute value of apparent zenith distance measured value become large, but because do not know Δ z after correction
nexistence, the Section 1 of actual corrected value is only A
ntan z
j, due to Δ z
nfor on the occasion of, z
jabsolute value ratio (the z of (negative value)
j+ Δ z
n) absolute value large, this makes Refraction Corrections value (negative value) add a negative value (-A
n× Δ z
n× sec
2z
j), namely make the absolute value of apparent zenith distance measured value (negative value) become greatly A approx
n× Δ z
n× sec
2z
j, at formula
in, δ
jbe greater than
on the occasion of so that the instantaneous latitude measured value that obtains of this star of observation reduces A
n× Δ z
n× sec
2z
j, the same with the observation on the south zenith.
If observe n on the south zenith
sstar, observes n to the north of zenith
nstar, this group star observes the instantaneous latitude measured value obtained will be less than normal measured value
Here air isodensity layer inclination Δ z is northwards defined
n, on the occasion of, if south dip, then Δ z
nfor negative value.
About
magnitude: due to A
sand A
ndiffer very little, even if difference 0.5%, in estimation
magnitude time, also can regard as equal, be taken as 60 approx "; If observation zenith distance is controlled within 45 °, then sec
2z
iand sec
2z
iall change between 1 and 2, its mean value can be taken as 1.3, like this, supposes at Δ z
nfor+5 ' when, then have
.Numerical value 3437.75 is the angle mark of a radian.
The situation that the additional residual tilting to cause about this isodensity layer distributes with zenith distance: the additional residual amount that every star measures instantaneous latitude is
still suppose Δ z
nfor+5 ', on the south zenith or to the north of by the observation of equally distributed 10 stars of zenith distance, with regard to their z, sec
2z,
with residual error v(unit: rad), list in table one:
Table one:
Here observation zenith distance span is larger, 50 °,
mean value also larger, be-0.129 ".
In real work, be adopt fixed star apparent declination, data such as height code wheel reading, star image position finding value etc., add the various error determine value correction of instrument, adjustment obtains the residual error of every star, as calculating Δ z
nfoundation.And be only to describe the problem here, adopt given Δ z
nwith zenith distance calculate.
In the inclination of meridian direction (North and South direction), spending the meridian record moment to star does not affect.Isodensity layer, to the inclination in any direction, can be decomposed into two components tilting in North and South direction and tilt at east-west direction.Then spend the meridian record moment to star in the inclination of east-west direction to have a direct impact, namely impact is had on the mensuration of astronomical longitude, and latitude determination be there is no that impact is (when tilt quantity is 5 ', influence amount be Refraction Corrections amount 100,000/, tilt quantity reaches when being 10 ', and influence amount is 4/100000ths of Refraction Corrections amount).
If the amount that the air isodensity layer that meteorological change causes tilts eastwards is Δ z
e, namely reflect the vertex of displacement, namely calculate the zenith point (being called refraction zenith) of astronomy tide, move Δ z eastwards
e.To be observed example on the south zenith, as shown in Figure 1, with Δ z
ewith zenith distance z
ifor right-angle side, in the narrow right angle spherical triangle being summit with true zenith, refraction zenith and tested star, cut-off arm of angle Δ z
ediagonal angle be θ
i, by spherical trigonometry formula, have tan θ
i=tan Δ z
e/ sin z
i, Δ z
eand θ
ibe all in a small amount, have θ approx
i=Δ z
e/ sin z(Δ z
eand θ
iunit must be consistent).The atmospheric refraction displacement of this tested star is moved along the hypotenuse of narrow right angle spherical triangle to refraction zenith, and value is approximately A tan z
i, as shown in Figure 1; Isodensity layer tilts to be calculated as follows the influence amount Δ t in star overwriting moment: sin (Δ t)=sin (A tan z
i) sin θ
i, the "=A tan z that has Δ t approx
i× θ
i(Δ t " represent that the isodensity layer represented with rad unit tilts star to be crossed to the influence amount in moment), the unit due to A is rad, and Δ t is " also in units of rad.And then have: Δ t "=A tan z
i× Δ z
e/ sin z
i=Δ z
e× A/cos z
i.This impact in units of rad, except depending on tilt quantity, only relevant with zenith distance, and get the cosine function of zenith distance, so influence amount is symmetrical relative to zenith.
In order to find out the impact of tilting on the star overwriting moment, also Δ t " must be converted into the second of time, because magnitude is smaller, preferably in units of millisecond, namely get Δ t
ms=Δ t " × 1000/ (15cos δ
i), here conveniently, get
and
calculate.Δ t
msvalue be asymmetric on zenith both sides.
In order to see clearly in meridian direction observation, the situation that the record moment additional residual that this isodensity layer tilts to cause distributes with zenith distance, the same with table one, get Δ z
e=5 ' and A=60 ", zenith north and south is respectively got by equally distributed 10 stars of zenith distance, lists Δ t respectively in table two ", Δ t
mswith residual error v(the former in units of rad, rear both in units of one millisecond):
Table two-1
Table two-2
Δ t in table two
msmean value be-9.8
ms.
Find out from table one and table two, although the amplitude of variation of additional residual, this isodensity layer is only had to tilt on about measuring half that astronomical latitude and star overwriting moment (mensuration astronomical longitude) affect, but they are clearly with the rule of zenith distance change, the particularly observation of the star that zenith distance is larger.So, can say for certain, after adopting local astronomy tide Model Measured, can perceive in the adjustment of observation and solve more exactly and meteorological change the tilt quantity Δ z that the air isodensity layer caused is tilted in both direction
nwith Δ z
e.There is Δ z
nwith Δ z
e, the apparent zenith distance measured value that just can obtain every star observation respectively and star overwriting moment do the correction that air isodensity layer tilts.
Δ z in above-described embodiment
nwith Δ z
evalue, can be utilize the residual error of observation data adjustment gained calculate tilt quantity service to illustrate, only taken the intermediate value analyzed from observation data at ordinary times here, its tilt quantity may reach more than 10 ' sometimes.The value of A is the mean value of current existing atmospheric refraction model.
After achieving the correction of local air isodensity layer tilt quantity, the measuring accuracy of uranometry and geodetic instrument can be improved.
Claims (2)
1. revise atmospheric envelope to tilt on a method for ground star observation value impact, it is characterized in that comprising the following steps:
Step 1, choose some fixed stars as sample fixed star i, use astronomical theodolite observation sample fixed star i, the telescope instrument of described astronomical theodolite is provided with CCD camera, the altitude axis of described astronomical theodolite is provided with height code-disc, for measuring the zenith distance of sample fixed star i; Set up the regression model between each observed reading of sample fixed star i that obtained by astronomical theodolite, calculate and change by meteorology the influence amount of air isodensity layer inclination to every sample fixed star i caused, comprise the following steps:
Step 1.1: the apparent declination δ gathering every sample fixed star i
i, the zenith distance reading z of height code-disc
i, the star image position finding value y in y direction on CCD camera target surface
i, the level error error of astronomical theodolite when measuring every sample fixed star i, optical axis point to the survey latitude component sum of variation error, altitude axis Run-out error and code-disc groove graduation error
and the adopted lattide of measuring station
substitute in following formula 1:
Formula 1:
In above formula
be stochastic error, represent the survey latitude residual error of every sample fixed star i, include the impact that air isodensity layer tilts on fixed star i measured value,
for target surface star image surveys the scale-up factor of latitude,
for the arithmetic mean of instantaneous latitude value and the adopted lattide of measuring station of whole sample fixed star i
difference, calculate by least square method
with every sample fixed star i's
Step 1.2: gather every sample fixed star i and do not considering that the star under the various error of astronomical theodolite and atmospheric envelope inclination conditions crosses moment calculated value T
i, star record value t at out-of-date quarter
i, the star image position finding value x in x direction on CCD camera target surface
i, and the level error error of astronomical theodolite when measuring every sample fixed star i, optical axis point to the survey real component sum (e of variation error, altitude axis Run-out error and code-disc groove graduation error
t)
i, substitute in following formula 2:
Formula 2:T
i=t
i+ k
tx
i+ (e
t)
i+ Δ λ+v
t(z
i);
V in above formula
t(z
i) be stochastic error, represent the time-measuring residual of every sample fixed star i, include the impact that air isodensity layer tilts on fixed star i measured value, k
tfor scale-up factor when target surface star image is surveyed, Δ λ is the arithmetic mean of the instantaneous longitude value of whole sample fixed star i and calculating T
itime measuring station adopted logitude λ
0difference, calculate the v of Δ λ and every sample fixed star i by least square method
t(z
i);
Step 1.3: by every sample fixed star i's calculating in step 1.1
and the zenith distance reading z of the height code-disc of every the sample fixed star i collected
i, substitute in following formula 3:
Formula 3:
From above formula, parameter Δ z is calculated by least square method
n, Δ z
nfor being changed the air isodensity layer that the causes tilt quantity along North and South direction by meteorology, if air isodensity layer northwards tilts, Δ z
nfor on the occasion of, if the south dip of air isodensity layer, then Δ z
nfor negative value;
Step 1.4: by the v of every sample fixed star i calculated in step 1.2
t(z
i), and the apparent declination δ of every the sample fixed star i collected
i, the zenith distance reading z of height code-disc
i, substitute in following formula 4:
Formula 4: Δ z
e=15v
t(z
i) cos δ
icos z
i/ (A sin 1 ");
From above formula, parameter Δ z is calculated by least square method
e, Δ z
efor meteorology changes the air isodensity layer tilt quantity eastwards caused;
Step 2, revise star observation value according to air isodensity layer tilt quantity, comprise the following steps:
Step 2.1: air isodensity layer step 1.3 calculated is along the tilt quantity Δ z of North and South direction
n, and the apparent zenith distance z of the fixed star to be measured obtained is observed by astronomical theodolite, substitute into following formula 5, calculate the true zenith distance Z of fixed star to be measured:
Formula 5:Z=z+A tan z+A × Δ z
n× sec
2z;
Step 2.2: the air isodensity layer tilt quantity Δ z eastwards that step 1.4 is calculated
e, and observe the fixed star to be measured obtained cross meridian moment t, the apparent zenith distance z of fixed star to be measured by astronomical theodolite, substitute in following formula 6, calculate fixed star to be measured and cross meridian correction moment T:
Formula 6:T=t+ Δ z
e× A/cos z;
A in above-mentioned steps 1.3, step 1.4, step 2.1 and step 2.2 represents the coefficient of the first term of atmospheric refraction series model.
2. a kind of atmospheric envelope of revising according to claim 1 tilts on the method for ground star observation value impact, it is characterized in that:
A in described step 1.3, step 1.4, step 2.1 and step 2.2 is 60 " .2.
Priority Applications (1)
| Application Number | Priority Date | Filing Date | Title |
|---|---|---|---|
| CN201210366902.8A CN102879013B (en) | 2012-09-27 | 2012-09-27 | Method for correcting influences of atmosphere inclination on ground star observation values |
Applications Claiming Priority (1)
| Application Number | Priority Date | Filing Date | Title |
|---|---|---|---|
| CN201210366902.8A CN102879013B (en) | 2012-09-27 | 2012-09-27 | Method for correcting influences of atmosphere inclination on ground star observation values |
Publications (2)
| Publication Number | Publication Date |
|---|---|
| CN102879013A CN102879013A (en) | 2013-01-16 |
| CN102879013B true CN102879013B (en) | 2015-02-25 |
Family
ID=47480430
Family Applications (1)
| Application Number | Title | Priority Date | Filing Date |
|---|---|---|---|
| CN201210366902.8A Active CN102879013B (en) | 2012-09-27 | 2012-09-27 | Method for correcting influences of atmosphere inclination on ground star observation values |
Country Status (1)
| Country | Link |
|---|---|
| CN (1) | CN102879013B (en) |
Families Citing this family (5)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN103512555B (en) * | 2013-09-28 | 2015-08-05 | 中国科学院云南天文台 | The measuring method that a kind of atmospheric envelope tilts |
| CN103499331B (en) * | 2013-09-28 | 2015-08-05 | 中国科学院云南天文台 | A kind of Novel astrolabe |
| CN104458653B (en) * | 2014-11-07 | 2017-05-17 | 中国科学院上海天文台 | Method and system for measuring atmospheric refraction value at large zenith distance |
| CN109033026B (en) * | 2018-07-23 | 2022-07-08 | 中国人民解放军63920部队 | Calibration method and device for atmospheric density detection data |
| CN111879299B (en) * | 2020-08-17 | 2022-04-15 | 中国科学院上海天文台 | Full-automatic satellite pointing method for ground-based telescope |
Citations (3)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| US5686719A (en) * | 1994-09-27 | 1997-11-11 | Elkin; David | Method for finding viewing intervals for the control of instruments, star trackers, and sensors on earth and solar system object orbiting platforms |
| CN101450716A (en) * | 2008-12-26 | 2009-06-10 | 中国科学院国家天文台 | Fault photo-detection method for earth synchronous transfer orbit satellite in orbit |
| CN102261921A (en) * | 2011-06-14 | 2011-11-30 | 哈尔滨工业大学 | Method for correcting influence of atmospheric refraction on precision of star sensor |
Family Cites Families (1)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| US7199872B2 (en) * | 2004-05-18 | 2007-04-03 | Leica Geosystems Ag | Method and apparatus for ground-based surveying in sites having one or more unstable zone(s) |
-
2012
- 2012-09-27 CN CN201210366902.8A patent/CN102879013B/en active Active
Patent Citations (3)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| US5686719A (en) * | 1994-09-27 | 1997-11-11 | Elkin; David | Method for finding viewing intervals for the control of instruments, star trackers, and sensors on earth and solar system object orbiting platforms |
| CN101450716A (en) * | 2008-12-26 | 2009-06-10 | 中国科学院国家天文台 | Fault photo-detection method for earth synchronous transfer orbit satellite in orbit |
| CN102261921A (en) * | 2011-06-14 | 2011-11-30 | 哈尔滨工业大学 | Method for correcting influence of atmospheric refraction on precision of star sensor |
Non-Patent Citations (1)
| Title |
|---|
| 组合大视场星敏感器自主定轨中的星光折射;薛申芳等;《光学学报》;20060731;第26卷(第7期);第971-974页 * |
Also Published As
| Publication number | Publication date |
|---|---|
| CN102879013A (en) | 2013-01-16 |
Similar Documents
| Publication | Publication Date | Title |
|---|---|---|
| CN102879013B (en) | Method for correcting influences of atmosphere inclination on ground star observation values | |
| CN104913780B (en) | The high-precision deviation of plumb line method for fast measuring of integrated GNSS and CCD zenith telescopes | |
| Chekole | Surveying with GPS, total station and terresterial laser scaner: a comparative study | |
| KR102140000B1 (en) | Method of Satellite Precise Orbit Determination using parallactic refraction scale factor estimation | |
| CN105783944B (en) | sun sensor calibration method and system | |
| Zhan et al. | High‐accuracy absolute positioning for the stationary planetary rover by integrating the star sensor and inclinometer | |
| CN105424060B (en) | A kind of measurement method of aircraft star sensor and strapdown inertial measurement unit installation error | |
| CN109855652A (en) | Spaceborne laser altimeter system instrument is directed toward on-orbit calibration method when angle error is non-constant | |
| Halicioglu et al. | Digital astro-geodetic camera system for the measurement of the deflections of the vertical: Tests and results | |
| Pierros | Stand-alone celestial navigation positioning method | |
| Gaifillia et al. | Empirical modelling of refraction error in trigonometric heighting using meteorological parameters | |
| CN105760688A (en) | Method for determining celestial body position or spherical target position by longitude and latitude assumption method | |
| Shi et al. | Automatic astronomical survey method based on video measurement robot | |
| Bagherbandi et al. | Physical and geometric effects on the classical geodetic observations in small-scale control networks | |
| Shen et al. | Inversion method of atmospheric refraction coefficient based on trigonometric leveling network | |
| Xu et al. | Approach to minimizing the influence of changeable observational environment on long-distance sea-crossing trigonometric leveling | |
| Studman | Agricultural and Horticultural Engineering: Principles, Models, Systems and Techniques | |
| Kumar Ghosh et al. | Determination of geoid undulation by astro-geodetic method | |
| Zhang et al. | Image-assisted total station camera mounting error correction model and analysis | |
| Mao et al. | Constructing an observational model of the neutral atmospheric refraction delay from measured values of the astronomical refraction | |
| Vishal et al. | Computation of Reduce Level Using Modern Survey Equipment at Sub-level from Vembakottai to PSR Engineering College Sivakasi. | |
| Malys et al. | How gravity and continuity in UT1 moved the Greenwich meridian | |
| KR100496811B1 (en) | Method for obtaining height information of buildings and producing digital map using gps measurement | |
| Ali | An error modeling framework for the sun azimuth obtained at a location with the hour angle method | |
| Kolkos et al. | Accuracy of topographical instruments and Unmanned Aerial Systems for mapping and surveying environmental projects. |
Legal Events
| Date | Code | Title | Description |
|---|---|---|---|
| C06 | Publication | ||
| PB01 | Publication | ||
| C10 | Entry into substantive examination | ||
| SE01 | Entry into force of request for substantive examination | ||
| C14 | Grant of patent or utility model | ||
| GR01 | Patent grant |