One degree of longitude has greatest value at the equator
One degree of longitude has greatest value at the poles
One degree of longitude has the same value everywhere
One degree of latitude decreases from the equator to the poles
A. One degree of longitude has greatest value at the equator
i = v. t. H/f
i = v. f/t. H
i = v. t. (f/H)
i = t. H/v. f
1 cm
2 cm
3 cm
4 cm
Every angle is less than two right angles
Sum of the three angles is equal to two right angles
Sum of the three angles less than six right angles and greater than two right angles
Sum of any two sides is greater than the third
λ = α
λ = 90° - α
λ = α - 90°
λ = 180° - α
sin z = sec φ . cos δ
cos z = sec φ . cos δ
tan z = sec φ . cos δ
None of these
Centre of the celestial sphere is taken as the position of the observer
Centre of the celestial sphere is taken as the centre of the earth
Stars move and maintain their relative positions
All the above
When the star momentarily moves vertically
When the angle at the star of the spherical triangle is 90°
When the star's declination is greater than the observer's latitude
All the above
sin H = tan φ . cot δ
cos H = tan φ . cot δ
tan H = tan φ . cot δ
None of these
365
365.2224
365.2422
366.2422
Ursa Minor's remains always north of pole star
Polar star remains always north of Polaris
Polaris remains always north of Ursa Minor's
Ursa Minor's pole star and Polaris are the names of the same star
24 hours 10 minutes
20 hours 25 minutes
24 hours 50 minutes
23 hours 50 minutes
Northward
Southward
From south to north of the equator
From north to south of the equator
22° 30'
23° 27'
23° 30'
24° 0'
March 21 to June 21
June 21 to September 21
September 21 to December 21
Both (a) and (b) of above
Is a good property
Is a function of tilt
Is not affected by the change of flying height between photographs
Is minimum when θ is 3°
2 mm
4 mm
6 mm
10 mm
Equator
Horizon
Pole
None of these
Sidereal time at any instant is equal to the hour angle of the first point of Aries
Local sidereal time of any place is equal to the right ascension of its meridian
Sidereal time is equal to the right ascension of a star at its upper transit
All the above
Co-declination
Co-latitude
Declination
Latitude
Parallel projection
Orthogonal projection
Central projection
None of these
Nadir
Isocenter
Principal point
Plumb point
1°
2°
3°
4°
Apparent solar time is measured from the lower transit of the true sun
Mean solar time is measured from the lower transit of the mean sun
Sidereal time is measured from the lower transit of the first point of Aries
Sidereal time is measured from the upper transit of the first point of Aries
Do not follow any definite mathematical law
Cannot be removed by applying corrections to the observed values
Are generally small
All the above
One less than mean solar days
One more than mean solar days
Equal to mean solar days
None of these
Altitude and azimuth system
Declination and hour angle system
Declination and right ascension system
Declination and altitude system
The area is divided into triangular figures
Control stations are located from which detailed surveys are carried out
Sides are not measured excepting the base line
All the above
Tension = (P - Ps)L/AE
Sag = L3w²/24P² where w is the weight of tape/m
Slope = (h²/2L) + (h4/8L3) where h is height difference of end supports
All the above
Nadir point
Iso centre
Principal point
All the above
sin λ
cos λ
tan λ
cot λ