see if the pulsar were moving at a constant distance and speed around its companion in a circular orbit, and what is actually observed. Prior to 2015 and the operation of Advanced LIGO, binary pulsars were the only tools scientists had to detect evidence of gravitational waves; Einstein's theory of general relativity predicts that two neutron stars would emit gravitational waves as they orbit a common center of mass, which would carry away orbital energy and cause the two stars to draw closer together and shorten their orbital period. A 10-parameter model incorporating information about the pulsar timing, the Keplerian orbits and three post-Keplerian corrections (the rate of periastron advance, a factor for gravitational redshift and time dilation, and a rate of change of the orbital period from gravitational radiation emission) is sufficient to completely model the binary pulsar timing. The measurements made of the orbital decay of the PSR B1913+16 system were a near perfect match to Einstein's equations. Relativity predicts that over time a binary system's orbital energy will be converted to gravitational radiation. Data collected by Taylor and Joel M. Weisberg and their colleagues of the orbital period of PSR B1913+16 supported this relativistic prediction; they reported in 1982 and subsequently that there was a difference in the observed minimum separation of the two pulsars compared to that expected if the orbital separation had remained constant. In the decade following its discovery the system's orbital period had decreased by about 76 millionths of a second per year - this means that the pulsar was approaching its maximum separation more than a second earlier than it would have if the orbit had remained the same. Subsequent observations continue to show this decrease. Intermediate mass binary pulsar An (IMBP) is a pulsar-white dwarf binary system with a relatively long spin period of around 10 - 200 ms consisting of a white dwarf with a relatively high mass of approximately The spin periods, magnetic field strengths, and orbital eccentricities of IMBPs are significantly larger than those of low mass binary pulsars (LMBPs). As of 2014, there are fewer than 20 known IMBPs. Examples of IMBPs include PSR J1802-2124 and PSR J2222−0137. The binary system PSR J2222−0137 has an orbital period of about 2.45 days and is found at a distance of 267 pc (approximately 870 light-years), making it the second closest known binary pulsar systems (as of 2014) and one