Tests of General Relativity from Timing the Double Pulsar

Krämer, M.; Stairs, I. H.; Manchester, R. N.; McLaughlin, M. A.; Lyne, A. G.; Ferdman, R. D.; Burgay, M.; Lorimer, D. R.; Possenti, A.; D’Amico, N.; Sarkissian, John; Hobbs, G.; Reynolds, John E.; Freire, P. C. C.; Camilo, F.

doi:10.1126/science.1132305

Cited by 958 publications

(969 citation statements)

References 31 publications

Supporting

Mentioning

928

Contrasting

Unclassified

Order By: Relevance

“…It is also the most relativistic binary pulsar discovered so far with higher mean orbital velocities and accelerations than those of other binary pulsars. Precision tests of General Relativity observables in the strong-field regime have verified the theory at the 0.05% level [16].…”

Section: Tests Of General Relativitymentioning

confidence: 95%

The cosmological constant puzzle

Bass¹

2011

J. Phys. G: Nucl. Part. Phys.

217

291

View full text Add to dashboard Cite

Abstract. The accelerating expansion of the Universe points to a small positive vacuum energy density and negative vacuum pressure. A strong candidate is the cosmological constant in Einstein's equations of General Relativity. Possible contributions are zero-point energies and the condensates associated with spontaneous symmetry breaking. The vacuum energy density extracted from astrophysics is 10 56 times smaller than the value expected from quantum fields and Standard Model particle physics. Is the vacuum energy density time dependent ? We give an introduction to the cosmological constant puzzle and ideas how to solve it.Confidential: not for distribution.

show abstract

Section: Tests Of General Relativitymentioning

confidence: 95%

The cosmological constant puzzle

Bass¹

2011

J. Phys. G: Nucl. Part. Phys.

217

291

View full text Add to dashboard Cite

show abstract

“…The well-known double neutron star (DNS) system PSR B1913+16 provided the first observational evidence for the existence of gravitational waves (GWs; Taylor & Weisberg 1989;Weisberg et al 2010), and the double pulsar system J0737−3039 continues to place ever more stringent constraints on deviations from general relativity (GR) in the strong-field regime (Kramer et al 2006). Neutron star mass measurements can be used to study nuclear physics and the equation of state of ultradense matter (Demorest et al 2010) while also providing insight into the mass distribution of the neutron star population (Özel et al 2012;Kiziltan et al 2013;Antoniadis et al 2016) and, in turn, formation mechanisms and evolution (e.g., Lattimer & Prakash 2004;Tauris & Savonije 1999).…”

Section: Introductionmentioning

confidence: 99%

The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

Lynch

Swiggum

Kondratiev

et al. 2018

ApJ

View full text Add to dashboard Cite

We provide timing solutions for 45 radio pulsars discovered by the Robert C. Byrd Green Bank Telescope. These pulsars were found in the Green Bank North Celestial Cap pulsar survey, an all-GBT-sky survey being carried out at a frequency of 350 MHz. We include pulsar timing data from the Green Bank Telescope and Low Frequency Array. Our sample includes five fully recycled millisecond pulsars (MSPs, three of which are in a binary system), a new relativistic double neutron star system, an intermediate-mass binary pulsar, a mode-changing pulsar, a 138 ms pulsar with a very low magnetic field, and several nulling pulsars. We have measured two post-Keplerian parameters and thus the masses of both objects in the double neutron star system. We also report a tentative companion mass measurement via Shapiro delay in a binary MSP. Two of the MSPs can be timed with high precision and have been included in pulsar timing arrays being used to search for low-frequency gravitational waves, while a third MSP is a member of the black widow class of binaries. Proper motion is measurable in five pulsars, and we provide an estimate of their space velocity. We report on an optical counterpart to a new black widow system and provide constraints on the optical counterparts to other binary MSPs. We also present a preliminary analysis of nulling pulsars in our sample. These results demonstrate the scientific return of long timing campaigns on pulsars of all types.

show abstract

“…Verbiest et al 2009) and thus excellent tools in the ongoing endeavours of high precision gravity tests (Kramer et al 2006), neutron star equations of state Özel et al 2010), and gravitational wave detection (van Haasteren et al 2011;Yardley et al 2011;Demorest et al 2013;Shannon et al 2013). These experiments utilise the high precision timing of millisecond pulsars (MSPs), which are known for their rotational stability and the stability of their integrated pulse profiles (which do not change over many years).…”

Section: Introductionmentioning

confidence: 99%

Single-pulse and profile-variability study of PSR J1022+1001

Karuppusamy

Lee

et al. 2015

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Millisecond pulsars (MSPs) are known as highly stable celestial clocks. Nevertheless, recent studies have revealed the unstable nature of their integrated pulse profiles, which may limit the achievable pulsar timing precision. In this paper, we present a case study on the pulse profile variability of PSR J1022+1001. We have detected approximately 14,000 sub-pulses (components of single pulses) in 35-hr long observations, mostly located at the trailing component of the integrated profile. Their flux densities and fractional polarisation suggest that they represent the bright end of the energy distribution in ordinary emission mode and are not giant pulses. The occurrence of sub-pulses from the leading and trailing components of the integrated profile is shown to be correlated. For sub-pulses from the latter, a preferred pulse width of approximately 0.25 ms has been found. Using simultaneous observations from the Effelsberg 100-m telescope and the Westerbork Synthesis Radio Telescope, we have found that the integrated profile varies on a timescale of a few tens of minutes. We show that improper polarisation calibration and diffractive scintillation cannot be the sole reason for the observed instability. In addition, we demonstrate that timing residuals generated from averages of the detected sub-pulses are dominated by phase jitter, and place an upper limit of ∼ 700 ns for jitter noise based on continuous 1-min integrations.

show abstract

Tests of General Relativity from Timing the Double Pulsar

Cited by 958 publications

References 31 publications

The cosmological constant puzzle

The cosmological constant puzzle

The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

Single-pulse and profile-variability study of PSR J1022+1001

Contact Info

Product

Resources

About