Physics for Scientists and Engineers, Vol. 1
6th Edition
ISBN: 9781429201322
Author: Paul A. Tipler, Gene Mosca
Publisher: Macmillan Higher Education
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Chapter 11, Problem 28P
To determine
Outbound time period.
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A comet of mass me is in an elliptical orbit around the sun (mass Mo), which is located
at one focus of the ellipse. The comet is a distance ra from the sun at its greatest distance
(aphelion) and rp at its closest pass (perihelion). Let G be the gravitational constant and recall
that F₁(r) = GMm and Ug(r) =
==
p²
GMm
r
1. What physical concepts would you need in order to calculate the speed of the comet at
aphelion and perihelion (va and vp)?
2. Apply these concepts to get two independent equations for the unknown quantities va and
Up in terms of G, mc, Mo, Tp, and rɑ. You do not need to solve these equations.
Plz asap
Will definitely upvote handwritten solution acceptable
2. (a) What are meant by gravitational potential and gravitational field? How far away fromthe earth does the acceleration due to gravity become 10% of its value on the earth’ssurface? NB:The radius of the earth is 6370 km. (b) What is meant by escape velocity? Show that the escape velocity from the surface of earthis √2 times the velocity of projection of an artificial satellite orbiting close around the earth.Obtain the escape velocity of an atmospheric particle 100 km above the earth’s surface. Giventhat ME = 5.98 × 1024 kg, RE = 6370 km, G = 6.67 × 10-11 N.m2/kg2.
Chapter 11 Solutions
Physics for Scientists and Engineers, Vol. 1
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- Check Your Understanding Assume you are in a spacecraft in orbit about the Sun at Earth’s orbit, but far away from Earth (so that it can be ignored). How could you redirect your tangential velocity to the radial direction such that you could then pass by Mars’s orbit? What would be required to change just the direction of the velocity?arrow_forwardUsing the technique shown in Satellite Orbits and Energy, show that two masses m1 and m2 in circular orbits about their common center of mass, will have total energy E=K+E=K1+K2Gm1m2r=Gm1m22r . We have shown the kinetic energy of both masses explicitly. (Hint: The masses orbit at radii r1 and r2 , respectively, where r=r1+r2 . Be sure not to confuse the radius needed for centripetal acceleration with that for the gravitational force.)arrow_forwardShow that the areal velocity for a circular orbit of radius r about a mass M is At=12GMr . Does your expression give the correct value for Earth’s areal vilocity about the Sun?arrow_forward
- Check Your Understanding The nearly circular orbit of Saturn has an average radius of about 9.5 AU and has a period of 30 years, whereas Uranus averages about 19 AU and has a period of 84 years. Is this consistent with our results for Halley’s comet?arrow_forwardFind the Hohmann transfer velocities, vEllipseEarth and vEllipseMars ,needed for a trip to Mars. Use Equation 13.7 to find the circular orbital velocities for Earth and Mars. Using Equation 13.4 and the total energy of the ellips (with semi-major asix a), given by E=GmMs2a , find the velocities at Earth (perihelion) and at Mars (aphelion) required to be on the transfer ellipse. The difference, v , at each point is the velocity boost or transfer velocity needed.arrow_forwardUsing Figure 13.9, carefull sketch a free body diagram for the case of a simple pendulum hanging at latitude lambda, labeling all forces acting on the point mass,m. Set up the equations of motion for equilibrium, setting one coordinate in the direction of the centripetal accleration (toward P in the diagram), the other perpendicular to that. Show that the deflection angle , defined as the angle between the pendulum string and the radial direction toward the center of Earth, is given by the expression below. What is the deflection angle at latitude 45 degrees? Assume that Earth is a perfect sphere. tan(+)=gg2REtan , where is the angular velocity of Earth.arrow_forward
- Check Your Understanding If we send a probe out of the solar system starting form Earth’s surface, do we only have to escape the Sun?arrow_forwardA geosynchronous Earth satellite is one that has an orbital period of precisely 1 day. Such orbits are sueful for communication and weather observation because the satellite remains above the same point on Earth (provided it orbits in the equatorial plane in the same direction as Earth’s rotation). Calculate the radius of such an orbit based on the data for Earth in Appendis D.arrow_forwardFollowing the technique used in Gravitation Near Earth’s Surface, find the value of g as a function of the radius r from the center of a spherical shell planet of constant density with inner and outer radii Rin and Rout . Find g for both eq and for RinrRout . Assuming the inside of the shell is kept airless, describe travel inside the spherical shell planet.arrow_forward
- Given the perihelion distance, p , and aphelion distance, q , for an elliptical orbit, show that the velocity at perihelion, vp , is given by vp=2GMSun(q+p)qp . (Hint: Use conservation of angular momentum to relate vp and vq , and then substitute into the conservation fo energy equation.)arrow_forwardIf a spacecraft is headed for the outer solar system, it may require several gravitational slingshots with planets in the inner solar system. If a spacecraft undergoes a head-on slingshot with Venus as in Example 11.6, find the spacecrafts change in speed vS. Hint: Venuss orbital period is 1.94 107 s, and its average distance from the Sun is 1.08 1011 m.arrow_forwardWhat is the orbital radius of an Earth satellite having a period of 1.00 h? (b) What is unreasonable about this result?arrow_forward
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