Newton's Law of Universal Gravitation

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Kreshnik Angoni

  • The law of Universal Gravitation is formulated by Newton for two point particles with masses m1 and m2 at a distance r between them. The magnitude of force exerted on one particle by the other one is given by:
F12=F21=Gm1m2r2  

The measurements show that the universal constant of gravitation is G=6.67*1011Nm2/kg2

  • The gravitational force is a vector directed versus the source that exerts this force. So, its vector form is:
F12=Gm1m2r2r21r21 

where r21r21 (or, r^21) is the unit vector with tail at mass m2 – the source of F12.

F21=Gm1m2r2r12r12 

r12r12 (or, r^12) is the unit vector with tail at mass m1 – the source of F21.


  • To apply the gravitational law for two bodies close to each other one must use integration techniques and

the difficulty of calculi depends on the form of the two bodies. But, if the bodied are far enough to each other, one may model them as point particles and apply the law in its original form.

  • In particular, with some approximations, we are able to model the interaction of earth with an object on its surface as if the whole mass of the earth is concentrated at its center and the objects are at distance r=Rearth.

  • Many experiments have shown that; when several particles interact gravitationally between them the

principle of linear superposition applies. So, inside a system of particles m1,m2,m3,…mn , the force exerted on mass m1 is:

F1=i=2nF1i  

THE GRAVITATIONAL AND THE INERTIAL MASS

  • When expressing the second law of Newton we use the inertial mass:

FNET=mina  

When formulating the gravitation law, Newton was not sure that the mass of particles in this law is the same as their inertial mass. Let’s verify this issue.

We start by supposing that the mass in the gravitational law may be different from min. So, we call it mgr.

Let’s consider now a body in free fall close to earth surface. The earth will exert on it the gravitational force with magnitude:

Fgr=GmgrMEarthREarth2 

Here we assume that the body is close to the surface so that its distance form earth center is Earth ≅ REarth

As this is the net force exerted on the body we apply the second law of Newton

FNET=mina=Fgr=Fgr=GmgrMEarthREarth2

So, we get

mina=mgr(GMEarthREarth2)=mgrg, where GMEarthREarth2=g

Then,

a=mgrming 

A big number of measurements show that the acceleration of free bodies is equal to g=9.8m/s2. This means that mgr/min=1, and min=mgr.

So, the experiments confirm that the gravitational mass is the same as the inertial mass.

  • Let us apply the gravitation law for the force exerted by earth over a mass 1kg close to earth.
F=GMEarth(REarth+h)2*REarthREarthg 

So, the g-vector is equal to the gravitation force exerted on a mass 1kg.

By measuring the force exerted on the mass 1kg in different locations on the earth one gets a whole system of g-vectors (fig.2). The totality of these vectors forms the gravitational field of the earth.



Note that the g-vector magnitude decreases with the increase of distance “h” from the earth but it is always directed versus the center of the earth. The gravitational field of the earth has a spherical symmetry.

In fact, it is not exactly spherical, because the model of earth as a uniform density sphere is not very precise. Now, the object weight is equal to gravitational force exerted by this field



W=mg 

So, the weight of the same object is a vector that is different in different points of gravitational field of the earth.


KEPLER’S LAWS ON PLANETARY MOTION


  • First law: The planets move on elliptic orbits around the sun that is located at one of its focuses.

The minor axis is long 2b and the major axis is long 2a. The closest distance to sun is called perihelion and the biggest distance to sun is called aphelion (fig.3).






  • Second law: The line sun- planet sweeps out equal areas for equal interval of times.

TOP

  • Third law: The square of the period of planet motion is proportional to the cube of average distance from the sun. Calculations show that the average of distance sun-planet is equal to half of major axis a. Then, satellite motion tells that
T2=ka3 where
ksun=4π2GMsun 


Note : Kepler’s laws are valid for elliptical paths of any planet around a central body; for example the moon moving around the earth but in this case

kEarth=4π2GMEarth 



THE ENERGY OF PLANETS


  • As the mass of other planets is much smaller than the mass of sun

we neglect their action on the motion of the studied planet. We consider that the system sun-planet is a conservative system, i.e. the forces originated from outside it are zero.

In these circumstances:

a) The torque of exterior force is zero and we can apply the principle for conservation of angular momentum.

b) The work done by Net exterior force is zero and we can apply the principle of energy conservation for the system sun-planet.

  • The principle of angular momentum conservation tells that LA=LP

or rA×pA=rP×pP

The equality of magnitudes brings to condition

rApASin90o=rPpPSin90orAmplanetvA=rPmplanetvP

So, we get

rAvA=rPvP 
  • The principle of energy conservation tells that that EA=EP

As the mechanical energy is E = K + U where

K=mplvpl22  and 
U=GmplMSunrplsun 

we get

mplvA22GmplMSunrA=mplvP22GmplMSunrP 

This gives, on cancelling mpl from the equation:

vA22GMSunrA=vP22GMSunrP

which leads to:

2GMSun(1rP1rA)=vP2vA2

Now, we know rAvA=rPvP
and the fact that:

rA+rP=2a

Thus,

vA2=GMarPrA  and,

vP2=GMarArP 

Finally, by substituting one of this expressions at the expression of total energy (at perihelion or aphelion) we get

E=GmplMSun2a 


See also

EXERCISES

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