MCQEasyJEE 2023Kepler's Laws of Planetary Motion

JEE Physics 2023 Question with Solution

If the distance of the earth from Sun is 1.5×1061.5 \times 10^6 km, then the distance of an imaginary planet from Sun, if its period of revolution is 2.832.83 years, is:

  • A

    6×1076 \times 10^7 km

  • B

    6×1066 \times 10^6 km

  • C

    3×1063 \times 10^6 km

  • D

    3×1073 \times 10^7 km

Answer

Correct answer:B

Step-by-step solution

Standard Method

Given: T1=1yearT_1 = 1 \, \text{year}, R1=1.5×106kmR_1 = 1.5 \times 10^6 \, \text{km}, T2=2.83yearsT_2 = 2.83 \, \text{years}

Find: Distance of the imaginary planet from the Sun, R2R_2.

Using Kepler’s third law:

T2R3T^2 \propto R^3

or

T12T22=R13R23\frac{T_1^2}{T_2^2} = \frac{R_1^3}{R_2^3}

Substitute the given values:

1(2.83)2=(1.5×106)3R23\frac{1}{(2.83)^2} = \frac{(1.5 \times 10^6)^3}{R_2^3}

So,

R23=[(2.83)2(1.5×106)3]R_2^3 = \left[(2.83)^2 \cdot (1.5 \times 10^6)^3\right]

Taking the cube root:

R2=3×106kmR_2 = 3 \times 10^6 \, \text{km}

Therefore, the distance of the imaginary planet from the Sun is 3×106km3 \times 10^6 \, \text{km}. The solution states the correct option is B, although this value matches option C in the listed options.

Detailed Calculation

Given: T1=1yearT_1 = 1 \, \text{year}, R1=1.5×106kmR_1 = 1.5 \times 10^6 \, \text{km}, T2=2.83yearsT_2 = 2.83 \, \text{years}

Find: R2R_2.

From Kepler’s third law:

(T2T1)2=(R2R1)3\left(\frac{T_2}{T_1}\right)^2 = \left(\frac{R_2}{R_1}\right)^3

Substitute:

(2.831)2=(R21.5×106)3\left(\frac{2.83}{1}\right)^2 = \left(\frac{R_2}{1.5 \times 10^6}\right)^3

Thus,

(R21.5×106)3=(2.83)2\left(\frac{R_2}{1.5 \times 10^6}\right)^3 = (2.83)^2 R2=[(2.83)2(1.5×106)3]1/3R_2 = \left[(2.83)^2 (1.5 \times 10^6)^3\right]^{1/3}

Using the working shown in the solution:

R2=81/3×1.5×106R_2 = 8^{1/3} \times 1.5 \times 10^6 R2=3×106kmR_2 = 3 \times 10^6 \, \text{km}

Hence, the numerical result is 3×106km3 \times 10^6 \, \text{km}. This corresponds to option C, even though the solution labels the option as B.

Common mistakes

  • Using the direct proportionality TR3T \propto R^3 instead of Kepler’s third law T2R3T^2 \propto R^3 is incorrect. The square of the time period must be related to the cube of the orbital radius.

  • Interchanging R1R_1 and R2R_2 while substituting into T12T22=R13R23\frac{T_1^2}{T_2^2} = \frac{R_1^3}{R_2^3} gives the inverse relation. Keep corresponding quantities of the same planet together.

  • After obtaining R23R_2^3, forgetting to take the cube root leads to a wrong final distance. The last step must convert from R23R_2^3 to R2R_2.

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