Independent of their angular momentum J or electric charge Q, black holes are frequently categorized based on their mass.
The Schwarzschild radius, which measures the distance from the event horizon to the center of the black hole, is roughly equal to the black hole's mass M: R (Schwarzschild) = (2GM / C 2) = 2.95 M / MSole Km, where MSole is the sun's mass and R is the Schwarzschild radius.
This relationship can vary by up to a factor of 2 for more generic black holes, but it is only precise for black holes with null charge and angular momentum.
As a result, with the Sun's mass M remaining constant, the escape velocity Vf = (2GM / R) 1/2 is produced. From this, Vf 2 = 2GM / R, where G remains constant, M pure but R drastically drops, raising Vf.
A BN of 10 solar masses and a 30 km OdE Radius: As soon as it exits the ODE, gravity accelerates at a rate of (Ripeto, Newton): GM/R2 = 1.48 * 10 12 m / s 2.
An ODE with a radius of 30 million km surrounds a BN with 10 million solar masses. Its gravity is worth 1.48 * 10 6 m/s2 right outside the ODE.That is one million times less. Next, we expand the radius outside the first OD by one meter, at which point the acceleration DECREASES by one part in a billion, or 1500 m/s 2. Finally, we expand the radius outside the second OD by one meter, at which point the acceleration DECREASES by one part in a trillion, or one part in a trillion trillion.
Like every other celestial body, the enormous force of gravity DECREES with the square of the distance.
For instance, nothing would be 60,000 times smaller than the sun at a distance of 1 billion km with a mass of 4 million solar masses.
