The first confirmed detection came in 1992, with the discovery of several terrestrial-mass planets orbiting the pulsar PSR B1257 + 12.

Shemar claimed to have discovered a pulsar planet in orbit around PSR 1829-10, using pulsar timing variations.

On 21 April 1992, radio astronomers Aleksander Wolszczan and Dale Frail announced the discovery of two planets orbiting the pulsar PSR 1257 + 12.

For example, the planets that orbit the pulsar PSR 1257 are often referred to with capital rather than lowercase letters.

BO Microscopii is a rapidly rotating star, and PSR J2144-3933 is an unusual pulsar with an unusually long rotation period.

* First confirmed detection of extrasolar planets with the discovery of several terrestrial-mass planets orbiting the pulsar PSR B1257 + 12 by Aleksander Wolszczan and Dale Frail.

However, gravitational radiation has been indirectly observed as an energy loss over time in binary pulsar systems such as PSR B1913 + 16.

* 1982 – Joseph Taylor and Joel Weisberg show that the rate of energy loss from the binary pulsar PSR B1913 + 16 agrees with that predicted by the general relativistic quadrupole formula to within 5 %

* 1992 – First planetary system beyond our own Solar System detected, around the pulsar PSR B1257 + 12

In 1967, the first pulsar, PSR B1919 + 21, was discovered in Vulpecula by Antony Hewish and Jocelyn Bell, in Cambridge.

Fifteen years after the first pulsar was discovered, the first millisecond pulsar, PSR B1937 + 21, was also discovered in Vulpecula, only a few degrees in the sky away from PSR B1919 + 21.

Also lying within the constellation's field is the pulsar PSR B1509-58.

The first confirmed detection of a planetary system was in 1992, with the discovery of several terrestrial-mass planets orbiting the pulsar PSR B1257 + 12.

PSR B1257 + 12 was not only the first pulsar exoplanetary system but also the first planetary system discovered.

PSR B1620-26 is also confirmed, however many other pulsar systems remain unconfirmed.

Working with Dale Frail, Wolszczan carried out astronomical observations from the Arecibo Observatory in Puerto Rico which led them to the discovery of the pulsar PSR B1257 + 12 in 1990.

A planetary system around the millisecond pulsar PSR 1257 + 12.

Confirmation of Earth-mass planets orbiting the millisecond pulsar PSR B1257 + 12.

In 1974, Hulse and Taylor discovered the first pulsar in a binary system, named PSR B1913 + 16 after its position in the sky, during a survey for pulsars at the Arecibo Observatory in Puerto Rico.

In 1974, Hulse and Taylor discovered binary pulsar PSR B1913 + 16, which is made up of a pulsar and black companion star.

The development of instrumentation within the FCRAO labs contributed to the discovery of the binary pulsar system PSR B1913 + 16 by Joseph Taylor and Russell Hulse, for which they received the 1993 Nobel Prize in Physics.

* First confirmed detection of extrasolar planets with the discovery of several terrestrial-mass planets orbiting the pulsar PSR B1257 + 12 by Aleksander Wolszczan and Dale Frail.

PSR B1257 + 12, sometimes abbreviated as PSR 1257 + 12, is a pulsar located 1000 light years from the Sun.

In 1992, Aleksander Wolszczan and Dale Frail announced the discovery of a multi-planet planetary system around the millisecond pulsar PSR 1257 + 12.

It is currently believed to have originally been the planet of WD B1620-26 before becoming a circumbinary planet, and therefore, while discovered through the pulsar timing method, it did not form the way that PSR B1257 + 12's planets are thought to have.

The companion of one pulsar in 47 Tucanae, 47 Tuc W, seems to still be transferring mass towards the neutron star, indicating that this system is completing a transition from being an accreting low-mass X-ray binary to a millisecond pulsar.

These pulsar planets are believed to have formed from the unusual remnants of the supernova that produced the pulsar, in a second round of planet formation, or else to be the remaining rocky cores of gas giants that somehow survived the supernova and then decayed into their current orbits.

General relativity also predicts the existence of gravitational waves, which have since been observed indirectly ; a direct measurement is the aim of projects such as LIGO and NASA / ESA Laser Interferometer Space Antenna and various pulsar timing arrays.

The presence of a pulsar in the Crab means that it must have formed in a core-collapse supernova ; Type Ia supernovae do not produce pulsars.

Hulse, Taylor, and other colleagues have used this first binary pulsar to make high-precision tests of general relativity, demonstrating the existence of gravitational radiation.

Radio pulsars ( rotation-powered pulsars ) and X-ray pulsars exhibit very different spin behaviors and have different mechanisms producing their characteristic pulses although it is accepted that both kinds of pulsar are manifestations of a rotating magnetized neutron star.

One side regards the A / B convention of naming binary stars as having priority, so that the pulsar is PSR B1620-26 A, the white dwarf companion is PSR B1620-26 B and the planet is PSR B1620-26 c. The other side considers PSR to only apply to stars which are pulsars, not their companions, so the white dwarf should be named using the WD convention, making the pulsar PSR B1620-26, the white dwarf " WD J1623-266 ", and the planet " PSR B1620-26 b. " Early articles used the first convention, but star catalogs have been using the second.

It is a millisecond pulsar, a kind of neutron star, and was found to have anomalies in the pulsation period, which led to investigations as to the cause of the irregular pulses.

The discovery of pulsar planets was unexpected ; pulsars or neutron stars have previously gone supernova, and it was thought that any planets orbiting such stars would have been destroyed in the explosion.

There was doubt concerning the discovery because of the retraction of the previous pulsar planet, and questions about how pulsars could have planets.

In 2000, the millisecond pulsar PSR B1620-26 was found to have a circumbinary planet ( PSR B1620-26 b ) that orbits both it and its companion white dwarf, WD B1620-26.

The disk is thought to have formed from metal-rich debris left over from the supernova that formed the pulsar roughly 100, 000 years ago and is similar to those seen around Sun-like stars, suggesting it may be capable of forming planets in a similar fashion.

However, pulsar wind nebulae have also been found around older pulsars whose supernova remnants have disappeared, including millisecond radio pulsars ( e. g. Stappers et al.

It is the first planetary system around a normal star to have mutual inclination between planets measured ( previously the mutual inclination of the planets orbiting the pulsar PSR B1257 + 12 had been determined by measuring their gravitational interactions ).

) After these factors have been taken into account, deviations between the observed arrival times and predictions made using these parameters can be found and attributed to one of three possibilities: intrinsic variations in the spin period of the pulsar, errors in the realization of Terrestrial Time against which arrival times were measured, or the presence of background gravitational waves.

It was previously thought to have a period of 2. 84 seconds but is now known to have a period of 8. 51 s, which is among the longest known radio pulsar.