Our radio astronomers have recently discovered the heaviest pulsar ever found: it is two times the mass of the Sun. No other massive pulsar has ever been weighed so accurately as this one.
How did we weigh a pulsar from a thousand light years away?
With the planet's largest fully-steerable radio telescope, the world's fastest stopwatch, and Albert Einstein. OK, the math of Albert Einstein.
But first, we need a pulsar. What's one of those?
From the Earth, it looks like a star that has a pulse, a rapid beat picked up only by radio telescopes. Discoverers Jocelyn Bell and Antony Hewish noticed that these beats were so regular that they seemed manmade. For a while, these cosmic radio sources were called LGM - Little Green Men!
Now, we know that a pulsar is a neutron star, the superdense, no-longer-shining core of a large star that got fatally compressed in a supernova implosion.
Neutron stars are so called because normal atoms inside them no longer exist. They have had all the space squeezed out of them, collapsing electrons onto protons, leaving a sphere of neutral neutrons and possibly simpler particles, such as quarks.
Where do their pulses come from?
Shining or not, stars spin. If you squash a big spinning star, its spin speeds up. If an ice skater tucks in her arms as she twirls, her spin will also speed up (see this video for a demonstration). Conservation of angular momentum is a basic law of physics that can make neutron stars the size of cities spin over 300 times per second.
Shining or not, stars also have magnetic fields. If you squash a big spinning star, its magnetic field bunches up and becomes super concentrated, super strong -- a billion times the strength of planet Earth's magnetic field. The magnetic poles on a neutron star act like fountains, an escape valve for charged particles that get trapped in the star's enormously strong magnetic field.
As a neutron star spins, its polar fountains turn with it, like an interstellar lighthouse beam. From Earth, we see the beam as it quickly sweeps past us -- there, gone, there, gone -- many times a second. That looks like a pulse from here. Hence the name, "pulsar."
How can a neutron star's pulse give us its weight?
A neutron star's pulses can come at us hundreds of times a second, ticking like a superfast clock with a millisecond hand. We can use such a fast and distant clock to time a pulsar's daily activities. If the pulsar is in orbit around another star, we can use the pulsar as a clock to time their tug-of-war and learn the weights behind their pulls on each other.
Albert Einstein figured out that an object's weight can affect how light travels near it. A really massive object like a planet or a star curves space around itself. Light traveling along through space will follow that curve.
If a pulsar is in orbit around a massive companion star, its pulses of light will follow the space curve caused by that star. From our view of their orbit, when the companion white dwarf star is in front of the pulsar, the pulses take a little longer to reach us than when the white dwarf is clear of the pulsar.
This kind of delay was predicted by Einstein and first tested by astronomer Irwin Shapiro. Now called the "Shapiro Delay," the effect can be measured with a superfast stopwatch and a lot of light. Why bother? Well, the amount of delay tells you the amount of mass of the star causing the delay. Sweet, but very difficult to measure: A Shapiro Delay can be only a millionth of a second!
Thankfully, the Green Bank Telescope is the largest telescope that can be steered to see pulsars and other radio objects around most of the sky. It has over two acres of collecting area, meaning it can capture lots and lots of radio waves at once. The more waves we grab, the easier it is to catch all of the superfast on and off radio pulses of a pulsar.
Gaming computers have pushed processor chip development into peta-op speeds, meaning that they can perform 1,000,000,000,000,000 operations per second. The Green Bank Ultimate Pulsar Processing Instrument, or GUPPI for short, is an array of eight computers outfitted with these chips. They can polish the signals coming from the Universe's fastest known pulsars so finely that we can easily spot any Shapiro Delays in their beats.
So, why should we care about a Shapiro Delay?
The amount of Shapiro Delay measured in a pulsar's beat tells us the amount of curved space causing the delay. The amount of the curved space tells us the amount of mass making the curved space. In a nutshell, the Shapiro Delay gives us the weight of the companion star! Factor in the time it takes the pulsar to go around the companion, and we can figure out the pulsar's mass, too. Tah-dah!