A certain quaternary star system consists of three stars, each of mass m, moving in the same circular orbit of radius r about a central star of mass M. The stars orbit in the same sense, and arepositioned one-third of a revolution apart from each other. Show that the period of each of the three stars is given by the following expression. (Submit a file with a maximum size of 1 MB.)T = 2πG(M+Choose File No file chosen3m3

Step 1 : Understanding the systemIn this quaternary system: there is a central star of mass M and…

Answered: A certain quaternary star system…

Classical Dynamics of Particles and Systems

5th Edition

ISBN:9780534408961

Author:Stephen T. Thornton, Jerry B. Marion

Publisher:Stephen T. Thornton, Jerry B. Marion

Chapter2: Newtonian Mechanics-single Particle

Section: Chapter Questions

Problem 2.48P

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Calculate the effective gravitational field vector g at Earths surface at the poles and the equator. Take account of the difference in the equatorial (6378 km) and polar (6357 km) radius as well as the centrifugal force. How well does the result agree with the difference calculated with the result g = 9.780356[1 + 0.0052885 sin 2 0.0000059 sin2(2)]m/s2 where is the latitude?
Show that for eccentricity equal to one in Equation 13.10 for conic sections, the path is a parabola. Do this by substituting Cartersian coordinates, x and y, for the polar coordinates, r and , and showing that it has the general form for a parabola, x=ay2+by+c .
Let gM represent the difference in the gravitational fields produced by the Moon at the points on the Earths surface nearest to and farthest from the Moon. Find the fraction gM/g, where g is the Earths gravitational field. (This difference is responsible for the occurrence of the lunar tides on the Earth.)
Consider a satellite in elliptical orbit around a planet of mass M, and suppose that physical units are so chosen that GM D 1 (where G is the gravitational constant). If the planet is located at the origin in the xy-plane, then Explain the equations of motion of the satellite?
Consider a satellite in elliptical orbit around a planet of mass M, and suppose that physical units are so chosen that GM D 1 (where G is the gravitational constant). If the planet is located at the origin in the xy-plane, then Explain the equations of motion of the satellite? Let T denote the period of revolution of the satellite. Kepler’s third law says that the square of T is proportional to the cube of the major semiaxis a of its elliptical orbit. In particular, if GM D 1, then?
Two identical uniform spheres A and B, with mass M=M= 1.00 [kg], are placed 0.500 [m] away from another spherical mass C with mass m=m= 0.300 [kg] as shown: If mass C is released from rest, what is its net acceleration? Assume that only the gravitational forces from spheres A and B act on C. State also the direction if it is upward or downward.
In this problem, you are going to explore three different ways to determine the gravitational constant G. a) By observing that the centripetal acceleration of the Moon around the Earth is ac = 2.66 × 10-3 m/s2, what is the gravitatonal constant G, in cubic meters per kilogram per square second? Assume the Earth has a mass of ME = 5.96 × 1024 kg, and the mean distance between the centers of the Earth and Moon is rm = 3.81 × 108 m. b) Measuring the centripetal acceleration of an orbiting object is rather difficult, so an alternative approach is to use the period of the orbiting object. Find an expression for the gravitational constant in terms of the distance between the gravitating objects rm, the mass of the larger body (the earth) ME, and the period of the orbiting body T. c) The gravitational constant may also be calculated by analyzing the motion of an object, launched from the surface of the earth at an initial velocity of vi. Find an expression of the gravitational constant…
A 1.07 kg mass is at the center of a uniform spherical shell of mass 1.06 * 10 ^ 20 * kg and radius 1.02 * 10 ^ 6 * m Find the resultant gravitational force on the mass? Also find the resultant gravitational force of the mass if it is placed just outside the shell? Magnitude? Direction? Find the value of g just outside the shell?
Suppose an artificial satellite has been put into circular orbit about the Earth, at a distance from the center of the Earth equal to 1/4 the distance from the Earth's center to the Moon's center. In terms of the Moon's period Tm, what will be the period of the satellite?
Can someone please explain it to me ASAP?!!! A binary star system consists of two stars, M1 = 3M and M2 = M whose centers separated by distance R and rotating about their mutual center of mass. Find the period of the orbital motion in terms of G, M, and R.
Assume the earth is a uniform sphere of mass M and radius R. As strange as it may sound, if one can dig a long tunnel from one side of the Earth straight through the center and exit the other end, any object falling into the tunnel will appear at the other end (i.e. the opposite side of the Earth) in just 2530 s (42.2 min). Call that time t. Let t be a function of G, M, and R, where G = 6.67 x 10^-11 m3 kg−1 s−2 is the Universal Gravitational Constant, M = 5.98 x 10^24 kg, and R = 6400 km. (a) From dimensional analysis alone find the expression for t, up to a numerical constant c.(b) Determine the value of c by using the above values in the expression found in part (a).
One model for a certain planet has a core of radius R and mass M surrounded by an outer shell of inner radius R, outer radius 2R, and mass 4M. If M= 4.1 * 1024 kg and R = 6.0 *106 m, what is the gravitational acceleration of a particle at points (a) R and (b) 3R from the center of the planet?

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