The nature of the PSR J2051--0827 eclipses

Stappers, B. W.; Bailes, M.; Lyne, A. G.; Camilo, F.; Manchester, R. N.; Sandhu, J. S.; Toscano, Maurizio; Bell, Jonathan

doi:10.1046/j.1365-8711.2001.04074.x

Cited by 63 publications

(76 citation statements)

References 29 publications

(56 reference statements)

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“…A simultaneous dual-frequency study is also fundamental for clarifying the physical mechanisms underlying the eclipses, for which several competing models have been proposed (e.g., Phinney et al 1988;Rasio et al 1989Rasio et al , 1991Stappers et al 2001;Gedalin & Eichler 1993;Thompson et al 1994;Khechinashvili et al 2000).…”

Section: Pulsar Studiesmentioning

confidence: 99%

The Sardinia Radio Telescope

Prandoni

Murgia

Tarchi

et al. 2017

A&A

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Context. The Sardinia Radio Telescope (SRT) is the new 64 m dish operated by the Italian National Institute for Astrophysics (INAF).Its active surface, comprised of 1008 separate aluminium panels supported by electromechanical actuators, will allow us to observe at frequencies of up to 116 GHz. At the moment, three receivers, one per focal position, have been installed and tested: a 7-beam K-band receiver, a mono-feed C-band receiver, and a coaxial dual-feed L/P band receiver. The SRT was officially opened in September 2013, upon completion of its technical commissioning phase. In this paper, we provide an overview of the main science drivers for the SRT, describe the main outcomes from the scientific commissioning of the telescope, and discuss a set of observations demonstrating the scientific capabilities of the SRT. Aims. The scientific commissioning phase, carried out in the 2012-2015 period, proceeded in stages following the implementation and/or fine-tuning of advanced subsystems such as the active surface, the derotator, new releases of the acquisition software, etc. One of the main objectives of scientific commissioning was the identification of deficiencies in the instrumentation and/or in the telescope subsystems for further optimization. As a result, the overall telescope performance has been significantly improved. Methods. As part of the scientific commissioning activities, different observing modes were tested and validated, and the first astronomical observations were carried out to demonstrate the science capabilities of the SRT. In addition, we developed astronomeroriented software tools to support future observers on site. In the following, we refer to the overall scientific commissioning and software development activities as astronomical validation. Results. The astronomical validation activities were prioritized based on technical readiness and scientific impact. The highest priority was to make the SRT available for joint observations as part of European networks. As a result, the SRT started to participate (in shared-risk mode) in European VLBI Network (EVN) and Large European Array for Pulsars (LEAP) observing sessions in early 2014. The validation of single-dish operations for the suite of SRT first light receivers and backends continued in the following year, and was concluded with the first call for shared-risk early-science observations issued at the end of 2015. As discussed in the paper, the SRT capabilities were tested (and optimized when possible) for several different observing modes: imaging, spectroscopy, pulsar timing, and transients.

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Section: Pulsar Studiesmentioning

confidence: 99%

The Sardinia Radio Telescope

Prandoni

Murgia

Tarchi

et al. 2017

A&A

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“…The eclipses occur when the pulsar passes behind its degenerate, 0.1-M companion, which is being ablated by the pulsar wind. At the discovery frequency, the pulsar is eclipsed ∼10% of the time, but this eclipse fraction scales strongly with wavelength (Stappers et al 2001). …”

Section: Psr J1959+2048mentioning

confidence: 99%

Low-frequency spectral turn-overs in millisecond pulsars studied from imaging observations

Kuniyoshi

Verbiest

Lee

et al. 2015

Mon. Not. R. Astron. Soc.

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Measurements of pulsar flux densities are of great importance for understanding the pulsar emission mechanism and for predictions of pulsar survey yields and the pulsar population at large. Typically these flux densities are determined from phase-averaged "pulse profiles", but this method has limited applicability at low frequencies because the observed pulses can easily be spread out by interstellar effects like scattering or dispersion, leading to a non-pulsed continuum component that is necessarily ignored in this type of analysis. In particular for the class of the millisecond pulsars (MSPs) at frequencies below 200 MHz, such interstellar effects can seriously compromise detectability and measured flux densities. In this paper we investigate MSP spectra based on a complementary approach, namely through investigation of archival continuum imaging data. Even though these images lose sensitivity to pulsars since the on-pulse emission is averaged with off-pulse noise, they are insensitive to effects from scattering and provide a reliable way to determine the flux density and spectral indices of MSPs based on both pulsed and unpulsed components. Using the 74 MHz VLSSr as well as the 325 MHz WENSS and 1.4 GHz NVSS catalogues, we investigate the imaging flux densities of MSPs and evaluate the likelihood of spectral turn-overs in this population. We determine three new MSP spectral indices and identify six new MSPs with likely spectral turn-overs.

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“…Data lying in the range of orbital phases between 0.20 and 0.35 1994 1995 1996 1997 1998 1999 2000 2001 Year were excluded from the fit because of the additional modulation of the excess column density on the TOAs in the eclipsing region (Stappers et al 1998(Stappers et al , 2001a. From the fit we obtained precise estimates of the pulsar's parameters and those of the orbit.…”

Section: Data Reduction and Timing Solutionmentioning

confidence: 99%

Orbital variability of the PSR J2051-0827 binary system

Doroshenko

Löhmer

Krämer

et al. 2001

A&A

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Abstract.We have carried out high-precision timing measurements of the binary millisecond pulsar PSR J2051−0827 with the Effelsberg 100-m radio telescope of the Max-Planck-Institut für Radioastronomie and with the Lovell 76-m radio telescope at Jodrell Bank. The 6.5-yrs radio timing measurements have revealed a significant secular variation of the projected semi-major axis of the pulsar at a rate ofẋ ≡ d(a1 sin i)/dt = (−0.23 ± 0.03) × 10 −12 , which is probably caused by the Newtonian spin-orbit coupling in this binary system leading to a precession of the orbital plane. The required misalignment of the spin and orbital angular momenta of the companion are evidence for an asymmetric supernova explosion. We have also confirmed that the orbital period is currently decreasing at a rate ofṖ b = (−15.5 ± 0.8) × 10 −12 s s −1 and have measured second and third orbital period derivatives d 2 P b /dt 2 = (+2.1 ± 0.3) × 10 −20 s −1 and d 3 P b /dt 3 = (3.6 ± 0.6) × 10 −28 s −2 , which indicate a quasi-cyclic orbital period variation similar to those found in another eclipsing pulsar system, PSR B1957+20. The observed variation of the orbital parameters constrains the maximal value of the companion radius to Rc max ∼ 0.06 R and implies that the companion is underfilling its Roche lobe by 50%. The derived variation in the quadrupole moment of the companion is probably caused by tidal dissipation similar to the mechanism proposed for PSR B1957+20. We conclude that the companion is at least partially non-degenerate, convective and magnetically active.

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The nature of the PSR J2051--0827 eclipses

Cited by 63 publications

References 29 publications

The Sardinia Radio Telescope

The Sardinia Radio Telescope

Low-frequency spectral turn-overs in millisecond pulsars studied from imaging observations

Orbital variability of the PSR J2051-0827 binary system

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