Precision timing measurements of PSR J1012+5307

By Ch. Lange, F. Camilo, N. Wex, Michael Kramer, D. Backer, Andrew G. Lyne, O. Doroshenko. 2001

200 citations recorded by the source corpus.

We present results and applications of high-precision timing measurements of the binary millisecond pulsar J1012+5307. Combining our radio timing measurements with results based on optical observations, we derive complete 3D velocity information for this system. Correcting for Doppler effects, we derive the intrinsic spin parameters of this pulsar and a characteristic age of 8.6±1.9 Gyr. Our upper limit for the orbital eccentricity of only 8×10−7 (68 per cent confidence level) is the smallest ever measured for a binary system. We demonstrate that this makes the pulsar an ideal laboratory in which to test certain aspects of alternative theories of gravitation. Our precision measurements suggest deviations from a simple pulsar spin-down timing model, which are consistent with timing noise and the extrapolation of the known behaviour of slowly rotating pulsars.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/57fd0592301e1f899b6a258b2b4b50173ea90144

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Citations in the corpus

ASSESSING THE ROLE OF SPIN NOISE IN THE PRECISION TIMING OF MILLISECOND PULSARS (2010, background): “Lange et al. (2001) report a non-zero ν̈ that they attribute to TN.”
The Parkes Multibeam Pulsar Survey - V. Finding binary and millisecond pulsars (2004, background): “A detailed description of this binary model can be found in Lange et al. (2001).”
The NANOGrav 15 yr Data Set: Observations and Timing of 68 Millisecond Pulsars (2023, methodology): “If the Shapiro delay was marginally detected via the F-statistic as described below, we instead modeled low-eccentricity orbits with the ELL1H model, which is simply the ELL1 model with the addition of the h3 and h4 parameters from the orthometric Shapiro delay parameterization of Freire & Wex (2010”
The NANOGrav 11-year Data Set: High-precision Timing of 45 Millisecond Pulsars (2017, methodology): “In such cases, we used the small-e expansion (“ELL1”) binary model (Lange et al. 2001), which parameterizes the orbit by: Pb and x as in the DD model; two Laplace– Lagrange parameters, e sinh w= , and e cos ;k w= and the epoch of ascending-node passage, Tasc.”
Timing analysis for 20 millisecond pulsars in the Parkes Pulsar Timing Array (2015, methodology): “The ELL1 model (Lange et al. 2001) is used to describe such systems, since it uses a small-eccentricity approximation to avoid this high correlation.”
A 2.1 M☉ Pulsar Measured by Relativistic Orbital Decay (2005, background): “…at the smallest values of m1 and m2 that fall within the constraints, and corresponds to a difference in coupling strengths ( c1 c2)2 < 7 ; 10 5: ð12Þ This improves by a factor of a few on previously published upper limits from PSRs B0655+64 and J1012+5307 (Arzoumanian 2003; Lange et al. 2001).”
The relativistic pulsar-white dwarf binary PSR J1738+0333 - II. The most stringent test of scalar-tensor gravity (2012, methodology): “The orbit of PSR J1738+0333 has a very low eccentricity, so we use the “ELL1” orbital model (Lange et al. 2001) to model it.1 This yields Keplerian and post-Keplerian parameters that are very weakly correlated with each other.”
TEMPO2, a new pulsar-timing package - I. An overview (2006, methodology): “The ‘ELL1’ model of Wex (1998 unpublished work; see Lange et al. 2001) was developed for pulsars in such orbits.”