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NCERT Exemplar · Q14

Q.Supposing Newton's law of gravitation for gravitation forces F1\mathbf{F}_1 and F2\mathbf{F}_2 between two masses m1m_1 and m2m_2 at positions r1\mathbf{r}_1 and r2\mathbf{r}_2 read F1=−F2=−r12r123 GM02(m1m2M02)n\mathbf{F}_1 = -\mathbf{F}_2 = -\dfrac{\mathbf{r}_{12}}{r_{12}^{3}}\, G M_0^{2} \left(\dfrac{m_1 m_2}{M_0^{2}}\right)^{n} where M0M_0 is a constant of dimension of mass, r12=r1−r2\mathbf{r}_{12} = \mathbf{r}_1 - \mathbf{r}_2 and nn is a number. In such a case, (Note: more than one of the given options may be correct.)

(a) the acceleration due to gravity on earth will be different for different objects.
(b) none of the three laws of Kepler will be valid.
(c) only the third law will become invalid.
(d) for nn negative, an object lighter than water will sink in water.
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With the force scaling as (m1m2)n(m_1m_2)^n instead of m1m2m_1m_2, the acceleration of a body near Earth depends on its own mass unless n=1n=1 — so different objects fall differently, making option (A) correct. Kepler's first and second laws still hold (the force stays central and still falls off as 1/r21/r^2 in distance), but the third law breaks because the orbiting body's own mass no longer cancels out — so only the third law is invalidated, making (B) false and (C) correct. For nn negative, the weight-vs-buoyancy comparison flips the usual density inequality, so an object lighter than water can sink — (D) is correct.

Setting up

The modified force law is

F1=−F2=−r12r123 GM02(m1m2M02)n\mathbf{F}_1=-\mathbf{F}_2=-\frac{\mathbf{r}_{12}}{r_{12}^3}\,GM_0^2\left(\frac{m_1m_2}{M_0^2}\right)^n

In the usual case n=1n=1, this reduces to Newton's law, and the force is directly proportional to m1m2m_1m_2. For n≠1n\neq1, the force instead scales as (m1m2)n(m_1m_2)^n — a genuinely different dependence on mass.

(A) Acceleration due to gravity on Earth

For an object of mass mm on Earth's surface (mass MEM_E, radius RER_E), the force magnitude is

F=GM02RE2(MEmM02)nF=\frac{GM_0^2}{R_E^2}\left(\frac{M_Em}{M_0^2}\right)^n

so the acceleration is

a=Fm=GM02(1−n)RE2MEn mn−1a=\frac{F}{m}=\frac{GM_0^{2(1-n)}}{R_E^2}M_E^n\,m^{n-1}

Unless n=1n=1, this depends on the object's own mass mm — different objects would fall with different accelerations. (A) is correct.

(B) and (C) Kepler's laws

Kepler's first law (elliptical orbits) and second law (equal areas in equal times) both follow from the force being central and varying purely with distance as 1/r21/r^2 — neither property has changed here, only the mass-dependence has. So the first and second laws still hold.

Kepler's third law, however, comes from equating the force to the centripetal requirement for a planet of mass mm orbiting a star of mass MM:

m4π2T2r=GM02r2(MmM02)nm\frac{4\pi^2}{T^2}r = \frac{GM_0^2}{r^2}\left(\frac{Mm}{M_0^2}\right)^n …

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