Last weekend was a pretty big sporting weekend. Not only was there the Third and deciding test of the 2013 Lions’ tour of Australia, but there was also the men’s and women’s finals of Wimbledon, and the German Grand Prix. As far as I can tell there is no sport going on this weekend. Before someone comments below that England are playing Australia at cricket in the First Test of the Ashes, I should remind my readers (all 2 of you) that a bunch of overweight men standing around for 5 days not doing much does not constitute sport. So, with this lull in the sporting calendar, I thought I would write this post about black holes, which I have been meaning to do for a while.

Nearly every one has heard of black holes, but what actually are they? And do they actually exist? Well, a black hole gets its name because it is an object from which *not even light* can escape. The radiation (light and other forms of electromagnetic radiation) which the central part of the black hole gives off is not able to escape the extreme gravitational field the black hole creates.

## Calculating the escape velocity

Newton’s law of gravity allows us to calculate the force of gravitational attraction between two bodies of masses and . It is simply . Let us suppose is the mass of the Earth, which we are now going to call ; and is the mass of an object on the Earth’s surface, we are going to call this second mass just . In order for the object on the Earth’s surface to escape the Earth’s gravitational field we have to give it a velocity.

When something is moving it has kinetic energy, and that kinetic energy is given by where is the object’s velocity. The object also has gravitational potential energy, as it is in a gravitational field. The gravitational potential energy is related to the gravitational force, it is given by which is

Notice that the gravitational potential energy is negative, whereas the kinetic energy is *always* positive. The sum of the two, the total energy is given by . In order for an object to escape the gravitational pull of another object, it needs to be able to escape to infinity. If it does not escape to infinity but to a smaller distance then, technically, it has not escaped the gravitational field of the object.

At infinity the PE is as we are dividing by infinity. As the object travels further and further away from its parent body it will slow down (as it is having to do work against the gravitational force), and so the KE will get less and less. At infinity it will be zero. So we can say that, at infinity, . But is constant, so it is also going to be zero any distance from the gravitational object, including at the surface of the planet.

Let us suppose the planet has a radius of , we can then write . The on both sides can cancel giving us and so, rearranging, we can write . The escape velocity is then found by writing so finally .

## The escape velocity from Earth, a White Dwarf and a Neutron Star

The equations we have just derived allows us to calculate the escape velocity from any object. We are going to calculate the value for the Earth, a white dwarf and a neutron star.

### The escape velocity from the Earth

For the Earth, the mass is and its radius (note, the Earth is not spherical, it bulges at the equator, so this is an *average* value). Before we plug these values of into the equation above we need to note that the value I have quoted for the Earth’s radius is in *kilometres*. We cannot put it into the equation in these units, we have to convert it to metres. , so this is the number we can plug into the equation for . When we do this we get that, for the Earth,

### The escape velocity from a white dwarf

A white dwarf is the stellar remnant of a star like the Sun. They are typically about the size of the Earth, but with about the mass of the Sun. So, for we shall use the mass of the Sun, which is , and we shall use the radius of the Earth that we used above, . These numbers give us which is 2% of the speed of light.

### The escape velocity from a neutron star

A neutron star is the end produce of more massive stars. The Sun is not massive enough to become a neutron star, but a star which is more than about 3 times the mass of the Sun is. In a neutron star all the space that exits in atoms is squeezed out, so it is essentially a pure lump of nuclei. A typical neutron star may have the mass of 2 Suns, but squeezed down into something the size of a city! So, for our calculation, we are going to assume a 2 solar mass neutron star, . For the radius we will assume 10km, so . Plugging these values into the equation for the escape velocity gives which is 77% of the speed of light.

## The event horizon of a black hole

The escape velocity from a neutron star is still below the speed of light. Pulsars are produced by radiation from the surface of a neutron star being beamed past us as the neutron star rotates. So, we have direct observational evidence that we can see radiation from neutron stars.

But, in the same way that a star which is a few times the mass of the Sun will end its life as a neutron star rather than a white dwarf; an even more massive star will not end as a neutron star. This is because of something called the *neutron degeneracy pressure*. To put it simply, this is a physical law which says that neutrons do not all want to be in the same place. They resist this through a resistive component in the strong nuclear force. But, if a neutron star were to have more than about 3 times the mass of the Sun, the gravity is strong enough to overcome this neutron degeneracy pressure. There is no known force to stop the collapse of the neutron star, and this is what forms a black hole.

We can work out the radius at which the escape velocity becomes equal to the speed of light for an e.g. 2 solar mass black hole. This is the same mass as our neutron star example above. But, as we shall see, it will need to be smaller than the 10km size of a neutron star. The radius at which the escape velocity is equal to the speed of light is what we call the *event horizon* of black hole.

To do the calculation we just re-arrange our escape velocity equation to find when where is the speed of light. The re-arrangement is that . For , and we find the radius of the event horizon to be . Notice how close this is to the actual size of a typical neutron star, just a little over half the size. It shows how little mass has to be added to a neutron star to tip it over the edge into becoming a black hole.

Notice that all of the above calculations have been done assuming Newton’s law of gravity. Newton’s law of gravity is not actually correct, it has been superseded by Einstein’s, which we call the theory of *General Relativity*. To do the calculations properly we should use this theory, but it is rather complicated. No, it is *very* complicated. But to illustrate the basic idea, Newton’s laws are fine. It is surprisingly often said that Einstein’s work led to the prediction of black holes. This is not true, they had been suggested by a geologist by the name of John Michell in 1783. But we do need Einstein’s work to do the calculations properly.

Any radiation being emitted from inside of the event horizon will never get to us, the gravitational pull from the black hole stops it from escaping. How do we therefore even know that black holes exist? I will answer that question in a future blog, along with some discussion of what happens as matter crosses the event horizon of a black hole, and what might be right at the centre of a black hole.

on 19/10/2013 at 13:39 |icyscienceReally good article i would like to put this on http://www.icyscience .com

on 19/10/2013 at 14:02 |RhEvansThank you. As long as I am credited and there is a link to here, then I have no problem with that 🙂

on 23/02/2017 at 08:31 |Imaging the Galaxy’s supermassive blackhole – part 1 | thecuriousastronomer[…] In this blog here I showed that the radius of a blackhole’s event horizon can be calculated by using the equation for the escape velocity when that velocity is equal to the speed of light . That is […]