Satellite Scenario Key Concepts
The Satellite Communications
object provides the ability to model and visualize satellites in orbit, compute access with
ground stations, and visualize and analyze communication links. This topic provides an
overview of the technical terms frequently encountered in scenario visualization.
A geodetic system uses coordinates (lat, lon, h) to represent position relative to a reference ellipsoid. All geodetic coordinates in a satellite scenario use the World Geodetic System, 1984 (WGS 84), as the reference ellipsoid. The coordinate origin of WGS 84 is located at the center of mass of the Earth.
lat is the latitude, which originates at the equator. More specifically, the latitude of a point is the angle normal to the ellipsoid at that point makes with the equatorial plane, which contains the center and equator of the ellipsoid. An angle of latitude is in the range [–90°, 90°]. Positive latitudes correspond to North and negative latitudes correspond to South.
lon is the longitude, which originates at the prime meridian. More specifically, the longitude of a point is the angle that a plane containing the ellipsoid center and the meridian containing that point makes with the plane containing the ellipsoid center and prime meridian. Positive longitudes are measured in a counterclockwise direction from a vantage point above the North Pole. Typically, longitude is in the range [–180°, 180°] or [0°, 360°].
h is the ellipsoidal height, which is measured along a normal of the reference spheroid.
Earth-Centered Earth-Fixed Coordinates
An Earth-centered Earth-fixed (ECEF) system uses Cartesian coordinates (X, Y, Z) to represent position relative to the center of the reference ellipsoid. The distance between the center of the ellipsoid and the center of the Earth depends on the reference ellipsoid. The Satellite scenario uses the WGS 84 reference ellipsoid, which has a center that coincides with the center of mass of the Earth.1
The positive X-axis intersects the surface of the ellipsoid at 0° latitude and 0° longitude, where the equator meets the prime meridian.
The positive Y-axis intersects the surface of the ellipsoid at 0° latitude and 90° longitude.
The positive Z-axis intersects the surface of the ellipsoid at 90° latitude.
Frame of Reference and North East Down (NED) Frame
To describe a point in space, you need a frame of reference that does not rotate with
respect to the stars. The Geocentric Celestial Reference Frame
(GCRF), with the origin at the center of the Earth and orthogonal vectors
I, J, and K, is used as the frame of reference when you add
Satellite objects to a
satelliteScenario object. The fundamental plane is the IJ-plane, which is closely aligned with the equator with a small offset that
changes over time because of precession and nutation of the rotation axis of the Earth.
When you use orbital elements to add satellites to the satellite scenario, the coordinates
are assumed to be defined in the geocentric celestial reference frame.
When you refer to the position, velocity, acceleration, orientation, and angular velocity, you must mention the coordinate system in which these quantities are expressed. Global systems such as GCRF and geodetic systems describe the position of an object using a triplet of coordinates. Local systems such as NED and Azimuth Elevation Range (AER) systems require two triplets of coordinates: one triplet describes the location of the origin, and the other triplet describes the location of the object with respect to the origin.
An NED system uses Cartesian coordinates (xNorth, yEast, zDown) to represent position relative to a local origin. The local origin is described by geodetic coordinates (lat0, lon0, h0). Typically, the local origin of an NED system is above the surface of the Earth.
The positive xNorth-axis points North along the meridian of longitude containing lon0.
The positive yEast-axis points East along the parallel of latitude containing lat0.
The positive zDown-axis points South along the ellipsoid normal.
An NED coordinate system is commonly used to specify location relative to a moving satellite. In this case, the coordinates are not fixed to the frame of the satellite, but to the point on the surface of the WGS 84 ellipsoid corresponding to the latitude and longitude of the satellite.
Roll, Pitch, and Yaw
Three lines run through a satellite and intersect at right angles at the center of mass of the satellite. These axes are fixed with respect to the satellite and are used to define the orientation of the satellite with respect to the NED frame. The orientation is defined by rotations in this sequence:
Rotation about the yaw axis by the yaw angle
Rotation about the pitch axis by the pitch angle
Rotation about the roll axis by the roll angle
The yaw, pitch, and roll angles have positive clockwise directions when looking in the positive direction of the axes. Unless otherwise specified, the Satellite Communications Toolbox uses the yaw-pitch-roll rotation order for these angles by default.
Azimuth-Elevation-Range (AER) Coordinates
An AER system uses spherical coordinates (az, elev, range) to represent position relative to a local origin. The local origin is described by geodetic coordinates (lat0, lon0, h0). Azimuth, elevation, and slant ranges are dependent on a local Cartesian system (for example, an NED system) with the origin centered at the center of mass of the satellite.
az is the azimuth, which is the clockwise angle in the (xNorth)(yEast)-plane from the positive yEast-axis to the projection of the object into the plane.
elev is the elevation, which is the angle from the (xNorth)(yEast)-plane to the object.
range is the slant range, which is the Euclidean distance between the object and the local origin.
Orbital elements are parameters required to uniquely identify a specific orbit. Uniquely defining an orbit and the position of a satellite within satellite orbit requires at least six parameters. Three of the parameters describe what the orbital plane looks like and the position of the satellite in the ellipse. The other three parameters describe how that plane is oriented in the celestial inertial reference frame and the location of the satellite in that plane. These six parameters are called the Keplerian elements or orbital elements.
In this diagram, the orbital plane (yellow) intersects a reference plane (gray). For Earth-orbiting satellites, the reference plane is usually the IJ-plane of the GCRF.
These two elements define the shape and size of the ellipse:
Eccentricity (e) — Describe how elongated the shape of the ellipse is when compared to a circle.
Semimajor axis (a) — The sum of the periapsis and apoapsis distances divided by 2. Periapsis is the point at which an orbiting object is closest to the center of mass of the body it is orbiting. Apoapsis is the point at which an orbiting object is farthest away from the center of mass of the body it is orbiting. For classic two-body orbits, the semimajor axis is the distance between the centers of the bodies.
These two elements define the orientation of the orbital plane in which the ellipse is embedded:
Inclination (i) — The vertical tilt of the ellipse with respect to the reference plane measured at the ascending node. The ascending node is the location where the orbit passes upward through the reference plane (the green angle i in the diagram). The tilt angle is measured perpendicular to the line of intersection between orbital plane and the reference plane. Any three points on an ellipse defines the ellipse orbital plane.
Starting with an equatorial orbit, the orbital plane can be tilted up. The angle it is tilted up from the equator is referred to as the inclination angle, i, in the range [0,180]. Because the center of the Earth must always be in the orbital plane, the point in the orbit where the satellite passes the equator on its way up north-bound through the orbit is the ascending node, and the point where the satellite passes the equator on its way down south-bound is the descending node. Drawing a line through these two points on the equator defines the line of nodes.
Right ascension of ascending node (Ω) — The horizontal orientation of the ascending node of the ellipse (where the orbit passes upward through the reference plane) with respect to the I-axis of the reference frame. The rotation of the right ascension of the ascending node (RAAN) can be any number between 0° and 360°.
The remaining two elements are:
Argument of periapsis (ω) — The orientation of the ellipse in the orbital plane, as an angle measured from the ascending node to the periapsis in the range [0, 360).
True Anomaly (v) — The position of the orbiting body along the ellipse at a specific time. The position of the satellite on the path is measured counterclockwise from the periapsis and is called the true anomaly, ν, in the range [0, 360).
Two Line Element (TLE) Files
The Satellite Communications
satellite function accepts a TLE file as a possible input to initialize the
satellite. To download TLE files, see the Space track website.
A TLE set is a data format encoding a list of orbital elements of an Earth orbiting object for a given point in time, the epoch. Orbital element parameters can be encoded as text in a variety of formats. The most common format is the National Aeronautics and Space Administration (NASA) or North American Aerospace Defense Command (NORAD) TLE format. In this format, each satellite has three rows: the first row contains the name of the satellite, and the next two rows are the standard TLE.
Data for each satellite consists of three lines, as this example shows.
Satellite 1 1 25544U 98067A 04236.56031392 .00020137 00000-0 16538-3 0 9993 2 25544 51.6335 344.7760 0007976 126.2523 325.9359 15.70406856328906
Row 1 is an eleven-character satellite name.
Rows 2 and 3 are the standard TLE set format identical to that used by NORAD and NASA.
This table describes the columns in row 2.
Column Description Example 1
Element set epoch (UTC)
First derivative of the mean motion with respect to time
Second derivative of the mean motion with respect to time (decimal point assumed)
BSTAR drag term
Element set type
Check sum (modulo 10)
This table describes the columns in row 3.
Column Description Example 1
Line number of element data
Inclination (in degrees)
Right ascension of the ascending node (in degrees)
Eccentricity (leading decimal point assumed)
Argument of perigee (in degrees)
Mean anomaly (in degrees)
Mean motion (in revs per day)
Revolution number at epoch (in revs)
Check sum (modulo 10)
Depending on the application and object orbit, the data derived from TLEs older than 30 days can become unreliable. Calculate the orbital positions from TLEs using the Simplified General Perturbations-4 (SGP4) and Simplified Deep-Space Perturbations-4 (SDP4) algorithms.
 “Basics of Space Flight” https://solarsystem.nasa.gov/basics/chapter5-1/.
 “CelesTrak. Frequently Asked Questions: Two-Line Element Set Format.” Accessed March 26, 2016. https://celestrak.com/columns/v04n03/.
- Multi-Hop Satellite Communications Link Between Two Ground Stations
- Satellite Constellation Access to Ground Station
- Comparison of Orbit Propagators
- Modeling Satellite Constellations Using Ephemeris Data
- Estimate GNSS Receiver Position with Simulated Satellite Constellations
- Model, Visualize, and Analyze Satellite Scenario
- Satellite Scenario Basics
1 Alignment of boundaries and region labels are a presentation of the feature provided by the data vendors and do not imply endorsement by MathWorks®.