[tex]2.6×10^6\:\text{m}[/tex]
Explanation:
The acceleration due to gravity g is defined as
[tex]g = G\dfrac{M}{R^2}[/tex]
and solving for R, we find that
[tex]R = \sqrt{\dfrac{GM}{g}}\:\:\:\:\:\:\:(1)[/tex]
We need the mass M of the planet first and we can do that by noting that the centripetal acceleration [tex]F_c[/tex] experienced by the satellite is equal to the gravitational force [tex]F_G[/tex] or
[tex]F_c = F_G \Rightarrow m\dfrac{v^2}{r} = G\dfrac{mM}{r^2}\:\:\:\:\:(2)[/tex]
The orbital velocity v is the velocity of the satellite around the planet defined as
[tex]v = \dfrac{2\pi r}{T}[/tex]
where r is the radius of the satellite's orbit in meters and T is the period or the time it takes for the satellite to circle the planet in seconds. We can then rewrite Eqn(2) as
[tex]\dfrac{4\pi^2 r}{T^2} = G\dfrac{M}{r^2}[/tex]
Solving for M, we get
[tex]M = \dfrac{4\pi^2 r^3}{GT^2}[/tex]
Putting this expression back into Eqn(1), we get
[tex]R = \sqrt{\dfrac{G}{g}\left(\dfrac{4\pi^2 r^3}{GT^2}\right)}[/tex]
[tex]\:\:\:\:=\dfrac{2\pi}{T}\sqrt{\dfrac{r^3}{g}}[/tex]
[tex]\:\:\:\:=\dfrac{2\pi}{(1.44×10^4\:\text{s})}\sqrt{\dfrac{(5×10^6\:\text{m})^3}{(3.45\:\text{m/s}^2)}}[/tex]
[tex]\:\:\:\:= 2.6×10^6\:\text{m}[/tex]