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Center of gravity is also known as a center of mass. |
Centre of Gravity in physics, is a system of particles is a specific point at which, for many purposes, the system's mass behaves as if it was concentrated. The center of gravity is a function only of the positions and masses of the particles that comprise the system. In the case of a rigid body, the position of its center of mass is fixed in relation to the object (but not necessarily in contact with it). In the case of a loose distribution of masses in free space, such as shot from a shotgun, the position of the center of mass is a point in space among them that may not correspond to the position of any individual mass. In the context of an entirely uniform gravitational field, the center of mass is often called the center of gravity - the point where gravity can be said to act. The center of mass of a body does not always coincide with its intuitive geometric center, and one can exploit this freedom. Engineers try hard to make a sport car as light as possible, and then add weight on the bottom; this way, the center of mass is nearer to the street, and the car handles better. When high jumpers perform a "Fosbury Flop", they bend their body in such a way that it is possible for the jumper to clear the bar while his or her center of mass does not. The center of mass frame (also called the center of momentum frame) is an inertial frame defined as the frame in which the center of mass of a system is at rest. Definition of a center of gravity. The center of mass of a system of particles is defined as the average of their positions , weighted by their massesm_{i}: whereM is the total mass of the system, equal to the sum of the particle masses. For a continuous distribution with mass density , the sum becomes an integral: If an object has uniform density then its center of mass is the same as the centroid of its shape. Examples of a center of gravity.
History of center of gravity. The concept of center of gravity was first introduced by the ancient Greek mathematician, physicist, and engineer Archimedes of Syracuse. Archimedes showed that the torque exerted on a lever by weights resting at various points along the lever is the same as what it would be if all of the weights were moved to a single point - their center of gravity. In work on floating bodies he demonstrated that the orientation of a floating object is the one that makes its center of gravity as low as possible. He developed mathematical techniques for finding the centers of gravity of objects of uniform density of various well-defined shapes, in particular a triangle, a hemisphere, and a frustum of a circular paraboloid. In the Middle Ages, theories on the center of gravity were further developed by Abu Rayhan al-Biruni, al-Razi (Latinized as Rhazes), Omar Khayyám, and al-Khazini. Locating center of mass This is a method of determining the center of mass of an L-shaped object.
Locating the center of mass of an arbitrary 2D physical shape This method is useful when one wishes to find the center of gravity of a complex planar object with unknown dimensions.
Locating the center of mass of a composite shape This method is useful when you wish to find the center of gravity of an object that is easily divided into elementary shapes, whose centers of mass are easy to find (see List of centroids). We will only be finding the center of mass in the x direction here. The same procedure may be followed to locate the center of mass in the y direction. The shape. It is easily divided into a square, triangle, and circle. Note that the circle will have negative area. From the List of centroids, we note the coordinates of the individual centroids. From equation 1 above: units. The center of mass of this figure is at a distance of 8.5 units from the left corner of the figure. Locating the center of mass by tracing around the perimeter of the shape A direct development of the Planimeter known as an integraph, or integerometer, can be used to establish the position of the center of mass of an irregular shape. A better term is probably moment planimeter. This method can be applied to a shape with an irregular, smooth or complex boundary where other methods are too difficult. It was regularly used by ship builders to ensure the ship would not capsize. See Locating the center of mass by mechanical means.
Motion of a center of gravity. The following equations of motion assume that there is a system of particles governed by internal and external forces. An internal force is a force caused by the interaction of the particles within the system. An external force is a force that originates from outside the system, and acts on one or more particles within the system. The external force need not be due to a uniform field. For any system with no external forces, the center of mass moves with constant velocity. This applies for all systems with classical internal forces, including magnetic fields, electric fields, chemical reactions, and so on. More formally, this is true for any internal forces that satisfy the weak form of Newton's Third Law. The total momentum for any system of particles is given by Where M indicates the total mass, and v_{cm} is the velocity of the center of mass. This velocity can be computed by taking the time derivative of the position of the center of mass. An analogue to the famous Newton's Second Law is Where F indicates the sum of all external forces on the system, and a_{cm} indicates the acceleration of the center of mass. Rotation and centers of gravity. The center of mass is often called the center of gravity because any uniform gravitational field g acts on a system as if the mass M of the system were concentrated at the center of mass R. This is seen in at least two ways:
If the gravitational field acting on a body is not uniform, then the center of mass does not necessarily exhibit these convenient properties concerning gravity. As the situation is put in Feynman's influential textbook The Feynman Lectures on Physics:
Later authors are often less careful, stating that when gravity is not uniform, "the center of gravity" departs from the CM. This usage seems to imply a well-defined "center of gravity" concept for non-uniform fields, but there is no such thing. Even when considering tidal forces on planets, it is sufficient to use centers of mass to find the overall motion. In practice, for non-uniform fields, one simply does not speak of a "center of gravity". CM frame and the center of gravity. The angular momentum vector for a system is equal to the angular momentum of all the particles around the center of mass, plus the angular momentum of the center of mass, as if it were a single particle of massM: This is a corollary of the Parallel Axis Theorem. Engineering; Aeronautical significance and Center of gravity (aircraft). The center of mass is an important point on an aircraft, which significantly affects the stability of the aircraft. To ensure the aircraft is safe to fly, it is critical that the center of gravity fall within specified limits. This range varies by aircraft, but as a rule of thumb it is centered about a point one quarter of the way from the wing leading edge to the wing trailing edge (the quarter chord point). If the center of mass is ahead of the forward limit, the aircraft will be less maneuverable, possibly to the point of being unable to rotate for takeoff or flare for landing. If the center of mass is behind the aft limit, the moment arm of the elevator is reduced, which makes it more difficult to recover from a stalled condition. The aircraft will be more maneuverable, but also less stable, and possibly so unstable that it is impossible to fly. Barycenter in Astronomy. For barycenters in geometry, see centroid. The barycenter (or barycentre; from the Greek) is the point between two objects where they balance each other. In other words, the center of gravity where two or more celestial bodies orbit each other. When a moon orbits a planet, or a planet orbits a star, both bodies are actually orbiting around a point that lies outside the center of the greater body. For example, the moon does not orbit the exact center of the earth, instead orbiting a point outside the earth's center (but well below the surface of the Earth) where their respective masses balance each other. The barycenter is one of the foci of the elliptical orbit of each body. This is an important concept in the fields of astronomy, Astrophysics, and the like (see two-body problem). In a simple two-body case, r_{1}, the distance from the center of the first body to the barycenter is given by: where:
r_{1} is essentially the semi-major axis of the first body's orbit around the barycenter - and r_{2} = a - r_{1} the semi-major axis of the second body's orbit. Where the barycenter is located within the more massive body, that body will appear to "wobble" rather than following a discernible orbit. The following table sets out some examples from our Solar System. Figures are given rounded to three significant figures. The last two columns show R_{1}, the radius of the first (more massive) body, and r_{1}/R_{1}, the ratio of the distance to the barycenter and that radius: a value less than one shows that the barycenter lies inside the first body.
If m_{1} >> m_{2} - which is true for the Sun and any planet - then the ratio r_{1}/R_{1} approximates to: Hence, the barycenter of the Sun-planet system will lie outside the Sun only if: That is, where the planet is heavy and far from the Sun. If Jupiter had Mercury's orbit (57,900,000 km, 0.387 AU), the Sun-Jupiter barycenter would be only 5,500 km from the center of the Sun (r_{1}/R_{1} ~ 0.08). But even if the Earth had Eris' orbit (68 AU), the Sun-Earth barycenter would still be within the Sun (just over 30,000 km from the center). To calculate the actual motion of the Sun, you would need to sum all the influences from all the planets, comets, asteroids, etc. of the Solar System (see n-body problem). If all the planets were aligned on the same side of the Sun, the combined center of mass would lie about 500,000 km above the Sun's surface. The calculations above are based on the mean distance between the bodies and yield the mean value r_{1}. But all celestial orbits are elliptical, and the distance between the bodies varies between the apses, depending on the eccentricity, e. Hence, the position of the barycenter varies too, and it is possible in some systems for the barycenter to be sometimes inside and sometimes outside the more massive body. This occurs where: Note that the Sun-Jupiter system, with e_{Jupiter} = 0.0484, just fails to qualify: 1.05 ? 1.07 > 0.954. Animations of a center of gravity. Images are representative, not simulated. Go To Print Article |
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