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A satellite mass 80kg is in orbit around the earth at a distance 7.5R where R is the mean radius of the earth. If the gravitational field is 9.8N/kg at the earth surface and R = 6400km. a)Centripetal force acting on the satellite b) The period of the satellite of the orbit in hours.

Physics

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Answers

2 parts
a

14 N\text{14 N}

b

29 hours\text{29 hours}

Step-by-step solution

7 steps

Here's the solution to your problem:

We are given the following information:

  • Mass of the satellite, m=80 kgm = 80 \text{ kg}
  • Orbital radius from the center of the Earth, r=7.5Rr = 7.5R, where RR is the mean radius of the Earth.
  • Gravitational field strength at the Earth's surface, g0=9.8 N/kgg_0 = 9.8 \text{ N/kg}
  • Mean radius of the Earth, R=6400 kmR = 6400 \text{ km}

First, let's convert RR and rr to meters:
R=6400 km=6400×103 m=6.4×106 mR = 6400 \text{ km} = 6400 \times 10^3 \text{ m} = 6.4 \times 10^6 \text{ m}
r=7.5R=7.5×6.4×106 m=48×106 m=4.8×107 mr = 7.5R = 7.5 \times 6.4 \times 10^6 \text{ m} = 48 \times 10^6 \text{ m} = 4.8 \times 10^7 \text{ m}

The gravitational field strength at the Earth's surface is g0=GMER2g_0 = \frac{GM_E}{R^2}, where GG is the gravitational constant and MEM_E is the mass of the Earth. From this, we can express GME=g0R2GM_E = g_0 R^2.

Part a· 3 steps

Calculate the centripetal force acting on the satellite

  1. Understand the force.

    The centripetal force required to keep the satellite in orbit is provided by the gravitational force between the Earth and the satellite.
    So, the centripetal force FcF_c is equal to the gravitational force FgF_g.

    Fc=Fg=GMEmr2F_c = F_g = \frac{GM_E m}{r^2}
  2. Substitute GMEGM_E and the given values.

    Substitute GME=g0R2GM_E = g_0 R^2 into the formula:

    Fc=g0R2mr2F_c = \frac{g_0 R^2 m}{r^2}

    Now, substitute the numerical values:

    Fc=(9.8 N/kg)×(6.4×106 m)2×(80 kg)(4.8×107 m)2F_c = \frac{(9.8 \text{ N/kg}) \times (6.4 \times 10^6 \text{ m})^2 \times (80 \text{ kg})}{(4.8 \times 10^7 \text{ m})^2}
  3. Calculate the force.

    Fc=9.8×80×(6.4×1064.8×107)2F_c = 9.8 \times 80 \times \left(\frac{6.4 \times 10^6}{4.8 \times 10^7}\right)^2 Fc=784×(6.448)2F_c = 784 \times \left(\frac{6.4}{48}\right)^2 Fc=784×(215)2F_c = 784 \times \left(\frac{2}{15}\right)^2 Fc=784×4225F_c = 784 \times \frac{4}{225} Fc=3136225F_c = \frac{3136}{225} Fc≈13.9377 NF_c \approx 13.9377 \text{ N}

    Rounding to two significant figures:

    14 N\boxed{\text{14 N}}

Part b

29 hours\text{29 hours}

Calculate the period of the satellite's orbit in hours

  1. Use the formula for the orbital period.

    The period TT of a satellite in orbit is given by Kepler's Third Law:

    T=2πr3GMET = 2\pi \sqrt{\frac{r^3}{GM_E}}
  2. Substitute GMEGM_E and the given values.

    Substitute GME=g0R2GM_E = g_0 R^2:

    T=2πr3g0R2T = 2\pi \sqrt{\frac{r^3}{g_0 R^2}}

    Now, substitute the numerical values:

    T=2π(4.8×107 m)3(9.8 m/s2)×(6.4×106 m)2T = 2\pi \sqrt{\frac{(4.8 \times 10^7 \text{ m})^3}{(9.8 \text{ m/s}^2) \times (6.4 \times 10^6 \text{ m})^2}}
  3. Calculate the period in seconds.

    T=2π(4.8)3×10219.8×(6.4)2×1012T = 2\pi \sqrt{\frac{(4.8)^3 \times 10^{21}}{9.8 \times (6.4)^2 \times 10^{12}}} T=2π110.592×10219.8×40.96×1012T = 2\pi \sqrt{\frac{110.592 \times 10^{21}}{9.8 \times 40.96 \times 10^{12}}} T=2π110.592×1021401.408×1012T = 2\pi \sqrt{\frac{110.592 \times 10^{21}}{401.408 \times 10^{12}}} T=2π0.27551×109T = 2\pi \sqrt{0.27551 \times 10^9} T=2π2.7551×108T = 2\pi \sqrt{2.7551 \times 10^8} T≈2π×1.65985×104T \approx 2\pi \times 1.65985 \times 10^4 T≈104283 sT \approx 104283 \text{ s}
  4. Convert the period from seconds to hours.

    There are 3600 seconds in an hour.

    Thours=104283 s3600 s/hourT_{\text{hours}} = \frac{104283 \text{ s}}{3600 \text{ s/hour}} Thours≈28.9675 hoursT_{\text{hours}} \approx 28.9675 \text{ hours}

    Rounding to two significant figures:

    29 hours\boxed{\text{29 hours}}
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