author={Joel M. Weisberg and Y. S. Huang},
  journal={The Astrophysical Journal},
We present relativistic analyses of 9257 measurements of times-of-arrival from the first binary pulsar, PSR B1913+16, acquired over the last 35 years. The determination of the “Keplerian” orbital elements plus two relativistic terms completely characterizes the binary system, aside from an unknown rotation about the line of sight, leading to a determination of the masses of the pulsar and its companion: 1.438 ± 0.001 M☉ and 1.390 ± 0.001 M☉, respectively. In addition, the complete system… 

PSR J2234+0611: A New Laboratory for Stellar Evolution

We report the timing results for PSR J2234+0611, a 3.6 ms pulsar in a 32 day, eccentric (e = 0.13) orbit with a helium white dwarf. The precise timing and eccentric nature of the orbit allow

A Measurement of the Galactic Plane Mass Density from Binary Pulsar Accelerations

We use compiled high-precision pulsar timing measurements to directly measure the Galactic acceleration of binary pulsars relative to the solar system barycenter. Given the vertical accelerations, we

A VLBI Distance and Transverse Velocity for PSR B1913+16

Using the Very Long Baseline Array, we have made astrometric observations of the binary pulsar B1913+16 spanning an 18-month period in 2014–2015. From these observations we make the first

Gravity Tests with Radio Pulsars

The discovery of the first binary pulsar in 1974 has opened up a completely new field of experimental gravity. In numerous important ways, pulsars have taken precision gravity tests quantitatively

The ultracool helium-atmosphere white dwarf companion of PSR J0740+6620?

We report detection of the likely companion of the binary millisecond pulsar (MSP) J0740+6620 with the Gran Telescopio Canarias in the r′ and i′ bands. The position of the detected starlike source

Constraints of General Screened Modified Gravities from Comprehensive Analysis of Binary Pulsars

Testing gravity using binary pulsars has become a key contemporary focus. Screened modified gravity is a kind of scalar-tensor theory with a screening mechanism in order to satisfy the tight solar

PALFA Discovery of a Highly Relativistic Double Neutron Star Binary

We report the discovery and initial follow-up of a double neutron star (DNS) system, PSR J1946+2052, with the Arecibo L-Band Feed Array pulsar (PALFA) survey. PSR J1946+2052 is a 17 ms pulsar in a

Einstein@Home discovery of a Double-Neutron Star Binary in the PALFA Survey

We report here the Einstein@Home discovery of PSR J1913+1102, a 27.3 ms pulsar found in data from the ongoing Arecibo PALFA pulsar survey. The pulsar is in a 4.95 hr double neutron star (DNS) system

The Orbital-decay Test of General Relativity to the 2% Level with 6 yr VLBA Astrometry of the Double Neutron Star PSR J1537+1155

PSR J1537+1155, also known as PSR B1534+12, is the second discovered double neutron star (DNS) binary. More than 20 yr of timing observations of PSR J1537+1155 have offered some of the most precise

Tests of Conservation Laws in Post-Newtonian Gravity with Binary Pulsars

General relativity is a fully conservative theory, but there exist other possible metric theories of gravity. We consider nonconservative ones with a parameterized post-Newtonian parameter, ζ2. A



Studies of the Relativistic Binary Pulsar PSR B1534+12. I. Timing Analysis

We have continued our long-term study of the double neutron star binary pulsar PSR B1534+12, using new instrumentation to make very high precision measurements at the Arecibo Observatory. We have


We present results of more than three decades of timing measurements of the first known binary pulsar, PSR B1913+16. Like most other pulsars, its rotational behavior over such long timescales is

Tests of General Relativity from Timing the Double Pulsar

By measuring relativistic corrections to the Keplerian description of the orbital motion, it is found that the “post-Keplerian” parameter s agrees with the value predicted by general relativity within an uncertainty of 0.05%, the most precise test yet obtained.

A new test of general relativity - Gravitational radiation and the binary pulsar PSR 1913+16

Observations of pulse arrival times from the binary pulsar PSR 1913+16 between 1974 September and 1981 March are now sufficient to yield a solution for the component masses and the absolute size of

Strong-field tests of relativistic gravity and binary pulsars.

  • DamourTaylor
  • Physics
    Physical review. D, Particles and fields
  • 1992
A detailed account of the parametrized post-Keplerian'' (PPK) formalism, a general phenomenological framework designed to extract the maximum possible information from pulsar timing and pulse-structure data, and how it can be combined with the predictions of a rather generic class of tensor biscalar theories to bring together tests based on observations of several different pulsars.


PSR J1906+0746 is a young pulsar in the relativistic binary with the second-shortest known orbital period, of 3.98 hr. We here present a timing study based on five years of observations, conducted

The relativistic pulsar-white dwarf binary PSR J1738+0333 - II. The most stringent test of scalar-tensor gravity

We report the results of a 10-year timing campaign on PSR J1738+0333, a 5.85-ms pulsar in a low-eccentricity 8.5-h orbit with a low-mass white dwarf companion. We obtained 17 376 pulse times of

Gravitational radiation from an orbiting pulsar

We describe an experiment which establishes, with a high degree of confidence, the existence of gravitational radiation as predicted by general relativity. The experiment involves observations of

Determination of the Geometry of the PSR B1913+16 System by Geodetic Precession

New observations of the binary pulsar B1913+16 are presented. Since 1978 the leading component of the pulse profile has weakened dramatically by about 40%. For the first time, a decrease in component

Proper Motion of Binary Pulsars as a Source of Secular Variations of Orbital Parameters

The proper motion of a binary pulsar gradually changes the apparent geometrical orientation of its orbital plane. Consequently, the derived values of the projected semimajor axis of the orbit and the