Re-examining the X-ray versus spin-down luminosity correlation of rotation powered pulsars

Possenti, A.; Cerutti, Raffaele; Colpi, M.; Mereghetti, S.

doi:10.1051/0004-6361:20020472

Cited by 307 publications

(361 citation statements)

References 49 publications

Supporting

Mentioning

296

Contrasting

Order By: Relevance

“…For a distance kpc), the inferred isotropic X-ray plus-nebula X-ray luminosity of other spin-powered pulsars, this is somewhat high but is within the observed scatter (Possenti et al 2002;Chevalier 2000). The pulsar's positional coincidence with the error box of the hard-spectrum, low-variability EGRET g-ray source GeV J2020ϩ3658 coupled with the high inferred spin-down luminosity strongly suggests this pulsar emits pulsed g-rays.…”

Section: Psr J2021ϩ3651supporting

confidence: 53%

PSR J2021+3651: A Young Radio Pulsar Coincident with an Unidentified EGRET γ-Ray Source

Roberts

Hessels

Ransom

et al. 2002

The Astrophysical Journal

View full text Add to dashboard Cite

We report on a deep search for radio pulsations toward five unidentified ASCA X-ray sources coincident with EGRET g-ray sources. This search has led to the discovery of a young and energetic pulsar using data obtained with the new Wideband Arecibo Pulsar Processor. PSR J2021ϩ3651 is likely associated with the X-ray source AX J2021.1ϩ3651, which in turn is likely associated with the COS B high-energy g-ray source 2CG 075ϩ00, also known as GeV J2020ϩ3658 or 3EG J2021ϩ3716. PSR J2021ϩ3651 has a rotation period of ms P ∼ 104 and , implying a characteristic age of kyr and a spin-down luminosity of . This DM suggests a distance kpc and a high g-ray efficiency of ∼15%, but 55Њ ! l ! 80Њ d տ 10 the true distance may be closer if there is a significant contribution to the DM from excess gas in the Cygnus region. The implied luminosity of the associated X-ray source suggests the X-ray emission is dominated by a pulsar wind nebula unresolved by ASCA.

show abstract

Section: Psr J2021ϩ3651supporting

confidence: 53%

PSR J2021+3651: A Young Radio Pulsar Coincident with an Unidentified EGRET γ-Ray Source

Roberts

Hessels

Ransom

et al. 2002

The Astrophysical Journal

View full text Add to dashboard Cite

show abstract

“…Rotational energy of the NS converted into radiation through the emission from a rotating magnetic dipole, a fraction of which can be emitted in X-rays (e.g., Possenti et al 2002;Campana et al 1998a, and references therein).…”

Section: Discussionmentioning

confidence: 99%

ABeppoSAXObservation of KS 1731−260 in Its Quiescent State: Constraints on the Magnetic Field of the Neutron Star

Burderi

Salvo

Stella

et al. 2002

ApJ

View full text Add to dashboard Cite

We report here the results of a 90 ks BeppoSAX observation of the low-mass X-ray binary and atoll source KS 1731À260 during a quiescent phase. From this observation we derive a source X-ray luminosity of $10 33 ergs s À1 (for a source distance of 7 kpc). If the neutron star is spinning at a period of a few milliseconds, as inferred from the nearly coherent oscillations observed during type I X-ray bursts, the quiescent X-ray luminosity constrains the neutron star magnetic field strength. We consider all the mechanisms that have been proposed to explain the quiescent X-ray emission of neutron star X-ray transients and compare the corresponding expectations with the measured upper limit on the X-ray luminosity. We find that, in any case, the neutron star magnetic field is most probably less than $10 9 G. We have also observed KS 1731À260, still in its quiescent state, at 1.4 GHz with the Parkes radio telescope to search for radio pulses. We found that no radio signals with millisecond periods are present with an upper limit on the flux of 0.60 mJy using a 4 minute integration time (optimal for a close system with an orbital period smaller than a few hours) and of 0.21 mJy using a 35 minute integration time (optimal for a wide-orbit system).

show abstract

“…Despite the majority of rotation-powered pulsars is observed at radio wavelengths (over 2,000), their energy output in this band is only a very small fraction ofĖ rot . The efficiency is higher in the X-ray band, where non-thermal emission is observed in about one hundred pulsars, with an average efficiency ∼10 −3 , but with a large dispersion around this value [158,119].…”

Section: Rotationmentioning

confidence: 93%

Pulsars and Magnetars

Mereghetti

2013

Braz J Phys

View full text Add to dashboard Cite

The high-energy sources known as anomalous X-ray pulsars (AXPs) and soft γ-ray repeaters (SGRs) are well explained as magnetars: isolated neutron stars powered by their own magnetic energy. After explaining why it is generally believed that the traditional energy sources at work in other neutron stars (accretion, rotation, residual heat) cannot power the emission of AXPs/SGRs, I review the observational properties of the twenty AXPs/SGRs currently known and describe the main features of the magnetar model. In the last part of this review I discuss the recent discovery of magnetars with low external dipole field and some of the relations between AXPs/SGRs and other classes of isolated neutron stars.

show abstract

Re-examining the X-ray versus spin-down luminosity correlation of rotation powered pulsars

Cited by 307 publications

References 49 publications

PSR J2021+3651: A Young Radio Pulsar Coincident with an Unidentified EGRET γ-Ray Source

PSR J2021+3651: A Young Radio Pulsar Coincident with an Unidentified EGRET γ-Ray Source

ABeppoSAXObservation of KS 1731−260 in Its Quiescent State: Constraints on the Magnetic Field of the Neutron Star

Pulsars and Magnetars

Contact Info

Product

Resources

About