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29 March, 06:20

If it takes a planet 2.8 x 10 to orbit a star with a mass of 6.2x 10 kg, what is the average distance between the planet and the star

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Answers (2)
  1. 29 March, 06:29
    0
    9.36 * 10^11 m

    Explanation:

    The formula of general velocity can be used here = v=√{ (G*M) / R}.

    G = gravitational constant or 6.67*10^-11 m³ kg⁻¹ s⁻²

    M = Mass of the star

    R = radius

    To find v we use the formula v=ωR.

    Here ω is the angular velocity; ω = ω=2π/T

    Here T is the orbital period of the planet

    The formula is arranged likewise: (2π/T) * R=√{ (G*M) / R}

    Step 2: { (2π/T) * R}²=[√{ (G*M) / R}]²

    Step 3: (4π²/T²) * R² = (G*M) / R

    Step 4: (4π²/T²) * R³=G*M

    Step 5: R³ = (G*M*T²) / 4π²

    Step 6: R=∛{ (G*M*T²) / 4π²}

    Step 7: Add your numbers to the formula and we get the answer.
  2. 29 March, 07:13
    0
    The answer can be found be using the formula of orbital velocity v=√{ (G*M) / R}

    Here G = Gravitational constant (G=6.67*10^-11 m³ kg⁻¹ s⁻²)

    M = Mass of star

    R = The distance between planet and the star

    As we also know, v=ωR,

    Here, ω = angular velocity

    R = radius

    ωR=√{ (G*M) / R}, now, ω=2π/T, where T is the orbital period of the planet

    (2π/T) * R=√{ (G*M) / R}, we "put to the power of 2" both sides to get rid of the square root and get:

    { (2π/T) * R}²=[√{ (G*M) / R}]²,

    (4π²/T²) * R² = (G*M) / R, we multiply by R:

    (4π²/T²) * R³=G*M, now we solve for R and get:

    R³ = (G*M*T²) / 4π², we take the third root to get R:

    R=∛{ (G*M*T²) / 4π²}, inserting the values of time and mass (T = 2.8 x 10 s and Mass = 6.2x 10 kg)

    R=∛{ (G*M*T²) / 4π²},

    R=R=∛[{G=6.67*10^-11 x 6.2x 10 x (2.8 x 10^2) / 4x3.14²},

    R=9.36*10^11 m

    So this will be the average distance between the star and the planet.
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