An advanced physics question
While performing calculations of a probe approaching a black hole ( http://chebmaster.ru/downloads/bhgravit.exe ) I got some unexpected results:
from https://en.wikipedia.org/wiki/Circular_orbit
orbital period T = 2 * Pi * square_root( r^3 / mu)
where mu = G * M
Practical calculations show: a circular orbits in the danger zone of a black hole may range from one revolution per a few seconds to 10 orbits per second (!), thus a probe has to rotate around its axis once per orbit (emulating being a tidally locked body) otherwise it will experience a brutal vibration with frequency of a few Hertz from the spaghettification force rapidly rotating relative to the probe.
But that adds a centripetal force summing with the spaghettification force trying to pull our probe apart:
From http://en.wikipedia.org/wiki/Centripetal_force
for a material point, Fc = mr * 4 * Pi^2 / (T^2)
for a solid rod, tensile force in the center is Fct = m * (integral of r where r is 0..L/2) * 4 * Pi^2 / (T^2)
where L is length of the rod.
We take only a half of the rod, because if each end pulls with the force of one kilogram, the total tensile force (in the center) is one kilogram.
Integral of r for r from 0 to L/2 = L/4.
So, Fct = m * (L / 4) * 4 * Pi^2 / (2^2 * Pi^2 * (r^3 / mu)) = m * L * mu / (4 * r^3)
From http://en.wikipedia.org/wiki/Spaghettification
for a solid rod, Ft = mu * L * m / (4 * r^3)
Do you see it? THEY ARE FRAKKING EQUAL! Keeping "tidally locked" to avoid vibration precisely *doubles* the force pulling the probe apart. HOW COMES THEY ARE EQUAL!!!
Or did I miss something?
P.S. Some interesting consequences: no, you cannot take a scenic look of a normal stellar-mass black hole. If you approach it closer than where it looks approximately as big as Moon when viewed from Earth, you go splat. And even a sturdiest, most compact probe can't approach the event horizon without going splat. Close to a BH of 10 sun masses a probe 10 centimeters in diameter would make more than a thousand orbits per second while experiencing tensile force of 250 thousand times its mass.
from https://en.wikipedia.org/wiki/Circular_orbit
orbital period T = 2 * Pi * square_root( r^3 / mu)
where mu = G * M
Practical calculations show: a circular orbits in the danger zone of a black hole may range from one revolution per a few seconds to 10 orbits per second (!), thus a probe has to rotate around its axis once per orbit (emulating being a tidally locked body) otherwise it will experience a brutal vibration with frequency of a few Hertz from the spaghettification force rapidly rotating relative to the probe.
But that adds a centripetal force summing with the spaghettification force trying to pull our probe apart:
From http://en.wikipedia.org/wiki/Centripetal_force
for a material point, Fc = mr * 4 * Pi^2 / (T^2)
for a solid rod, tensile force in the center is Fct = m * (integral of r where r is 0..L/2) * 4 * Pi^2 / (T^2)
where L is length of the rod.
We take only a half of the rod, because if each end pulls with the force of one kilogram, the total tensile force (in the center) is one kilogram.
Integral of r for r from 0 to L/2 = L/4.
So, Fct = m * (L / 4) * 4 * Pi^2 / (2^2 * Pi^2 * (r^3 / mu)) = m * L * mu / (4 * r^3)
From http://en.wikipedia.org/wiki/Spaghettification
for a solid rod, Ft = mu * L * m / (4 * r^3)
Do you see it? THEY ARE FRAKKING EQUAL! Keeping "tidally locked" to avoid vibration precisely *doubles* the force pulling the probe apart. HOW COMES THEY ARE EQUAL!!!
Or did I miss something?
P.S. Some interesting consequences: no, you cannot take a scenic look of a normal stellar-mass black hole. If you approach it closer than where it looks approximately as big as Moon when viewed from Earth, you go splat. And even a sturdiest, most compact probe can't approach the event horizon without going splat. Close to a BH of 10 sun masses a probe 10 centimeters in diameter would make more than a thousand orbits per second while experiencing tensile force of 250 thousand times its mass.