Chapter 3 · MCQ Read Mode

Geodesy and Gravity Field

The geoid is best defined as:

The surface used for the mathematical computation of geodetic positions is the:

The flattening of the WGS84 ellipsoid is approximately:

The height obtained directly from GNSS observations is:

The relation between ellipsoidal height h, orthometric height H and geoid undulation N is:

The angle between the plumb line and the ellipsoidal normal at a point is called the:

The meridian component of the deflection of the vertical is given by:

The Laplace condition relates the astronomical and geodetic azimuths by:

Orthometric height is measured from the:

The geoid undulation over the earth varies roughly within:

Geocentric Cartesian (ECEF) coordinates have their origin at the:

Satellite geodesy includes techniques such as:

The deflection of the vertical is largest:

The flattening of an ellipsoid is defined as:

The first eccentricity squared of an ellipsoid is related to the flattening by:

The radius of curvature in the prime vertical N compared with that in the meridian M is:

The radius of the parallel of latitude φ on an ellipsoid is:

A short arc along a meridian is given by:

The length of one degree of longitude at the equator is approximately:

The classical ellipsoid used for the geodetic system of Nepal and India is:

The shortest line between two points on the ellipsoid is called the:

The two reciprocal normal sections between two points differ because:

Computing the coordinates of a second point from a known point, an azimuth and a distance on the ellipsoid is called the:

Vincenty's formulae are used for:

A local (non-geocentric) ellipsoid is selected so that it:

GRS80 and WGS84 differ mainly in their:

A geodetic datum is defined by:

ITRF2014 is an example of a:

Coordinates in ITRF are always quoted with an epoch because:

A seven-parameter Helmert transformation consists of:

A rotation matrix used in coordinate transformation has a determinant of:

A reflection matrix is required when:

A projection that preserves angles and the shape of small features is called:

The width of each UTM zone is:

The scale factor at the central meridian of a UTM zone is:

The false easting assigned to the central meridian in UTM is:

Nepal's Modified UTM (MUTM) uses zones of width:

The ellipsoid used with Nepal's classical MUTM system is:

The angle between grid north and true north at a point is called the:

Gravity at a point on the earth is the resultant of:

The value of gravity is greatest:

One milligal (mGal) equals:

Level surfaces of the earth's gravity field are:

A plumb line is:

Normal gravity is the gravity of:

The free-air correction to observed gravity is about:

The Bouguer correction accounts for the:

The terrain correction applied to gravity observations is:

Bruns' formula relates the geoid undulation to the:

Stokes' integral is used to compute the:

A good national geoid model is important because it allows:

Isostatic gravity anomalies are close to zero where:

Outside the attracting masses, the gravitational potential satisfies:

The earth's external gravity field is conveniently represented by a series of:

Spherical harmonics with order m = 0 are called:

The coefficient C̄₂₀ of the spherical harmonic expansion is closely related to the earth's:

Clairaut's theorem allows the determination of the earth's flattening from:

A free-fall (ballistic) instrument that determines the value of g directly is an:

A spring-type LaCoste-Romberg or Scintrex instrument measures:

Readings of a relative gravimeter are repeated at a base station during a survey in order to:

The GRACE and GRACE-FO satellite missions are used mainly to observe:

In the Airy-Heiskanen model of isostasy:

The isostatic gravity anomaly in a region that is fully compensated is:

Complete Bouguer anomalies over high mountain ranges are typically:

The crustal root beneath the Himalaya is of the order of:

The obliquity of the ecliptic is approximately:

The point where the sun crosses the celestial equator moving northwards is the:

Which pair of celestial coordinates is independent of both the observer's position and time?

In the astronomical (PZS) triangle, the side from the pole to the star is:

Napier's rules of circular parts apply to:

The length of a sidereal day is:

The local sidereal time is equal to the:

The difference between apparent solar time and mean solar time is called the:

UTC differs from TAI and from GPS time because UTC:

Nepal standard time is based on the meridian:

The slow conical motion of the earth's axis with a period of about 26 000 years is called:

The Chandler wobble, with a period of about 435 days, is a component of:

Atmospheric refraction makes a celestial body appear: