One-dimensional electric field structure of an outer gap accelerator -- III. Location of the gap and the gamma-ray spectrum

Hirotani, Kouichi; Shibata, Shinpei

doi:10.1046/j.1365-8711.2001.04565.x

Cited by 40 publications

(40 citation statements)

References 68 publications

(104 reference statements)

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“…All spectra are corrected for interstellar absorption (unabsorbed). (Cheng et al 1986a,b;Romani 1996;Hirotani & Shibata 2001). Both approaches encountered problems, e.g.…”

Section: Psr J1846−0258 As a Rotation-powered Pulsarmentioning

confidence: 99%

High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

Kuiper

Hermsen

2009

A&A

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Aims. PSR J1846−0258 is a young rotation-powered pulsar with one of the highest surface magnetic field strengths, located in the centre of SN-remnant Kes-75. In June 2006 a magnetar-like outburst took place. Using multi-year RXTE and INTEGRAL observations covering the epoch of the outburst, we aim to study the temporal and spectral characteristics of PSR J1846−0258 over a broad ∼3-300 keV energy range to derive constraints on theoretical scenarios aiming to explain this schizophrenic behaviour. Methods. We explored all publically available RXTE observations of PSR J1846−0258 to generate accurate ephemerides over the period January 30, 2000-November 7, 2007. Phase-folding procedures yielded pulse profiles for RXTE PCA (∼3-30 keV), RXTE HEXTE (∼15-250 keV) and INTEGRAL ISGRI (∼20-300 keV). The pulsed spectrum over the full ∼3-300 keV energy range was derived, as well as the total spectrum (including the pulsar wind nebula) over the 20-300 keV band with the ISGRI. The timing, spatial, and spectral analyses were applied for epochs before, during, and after the magnetar-like outburst to study the evolution of the high-energy characteristics. Results. ISGRI detected PSR J1846−0258/Kes-75 before outburst during 2003-2006 with a power-law-shape spectrum over the 20-300 keV energy range with photon index Γ = 1.80 ± 0.06 and energy flux (20-300 keV) of (6.62 ± 0.35) × 10 −11 erg/cm 2 s. More than 90 days after the onset of the outburst, still during the decay phase, the same spectral shape was measured (Γ = 1.75 +0.27 −0.31 ) with an indication for a 52% (2.3σ) enhanced total emission, while one year after the outburst the hard X-ray non-thermal emission of PSR J1846−0258/Kes-75 was found to be back to its pre-outburst values. PCA monitoring of PSR J1846−0258 before the outburst yielded phase-coherent ephemerides confirming the earlier derived breaking index of the spindown. During the outburst, incoherent solutions have been derived. We show that the radiative outburst was triggered by a major spin-up glitch near MJD 53 883 ± 3 with a glitch size Δν/ν in the range (2.0−4.4) × 10 −6 . Using all pre-outburst observations of ISGRI and HEXTE for the first time pulse profiles have been obtained up to 150 keV with a broad single asymmetric pulse. The pulse shape did not vary with energy over the 2.9-150 keV energy range, nor did it change during the magnetar-like outburst. The time-averaged pre-outburst ∼3-300 keV pulsed spectrum measured with the PCA, HEXTE, and ISGRI was fitted with a power-law model with Γ = 1.20 ± 0.01. A fit with a curved power-law model gives an improved fit. Around 150 keV the pulsed fraction approaches 100%. For the first 32 days of the magnetarlike outburst, the 3-30 keV pulsed spectrum can be represented with two power laws, a soft component with index Γ s = 2.96 ± 0.06 and a hard component with the pre-outburst value Γ h ∼ 1.2. Above ∼9 keV, all spectra during outburst are consistent with the latter single power-law shape with index ∼1.2. The 2-10 keV flux increased by a factor ∼5 and the 10...

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“…All spectra are corrected for interstellar absorption (unabsorbed). (Cheng et al 1986a,b;Romani 1996;Hirotani & Shibata 2001). Both approaches encountered problems, e.g.…”

Section: Psr J1846−0258 As a Rotation-powered Pulsarmentioning

confidence: 99%

High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

Kuiper

Hermsen

2009

A&A

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“…• ) or when the inner boundary of outer gap can extend to 10 stellar radii (Hirotani et al 2003;Hirotani & Shibata 2001).…”

Section: Theoretical Calculations In Thementioning

confidence: 99%

NON-DETECTION IN A FERMI /LAT OBSERVATION OF AXP 4U 0142+61: MAGNETARS?

Tong

Song

2010

ApJ

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Significant research in compact stars is currently focused on two kinds of enigmatic sources: anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs). Although AXPs and SGRs are popularly thought to be magnetars, other models (e.g., the accretion model) for understanding the observations can still not be ruled out. It is worth noting that a non-detection in a Fermi/LAT observation of AXP 4U 0142+61 has been reported recently by Sasmaz Mus & Gogus. We propose here that Fermi/LAT observations may distinguish between the magnetar model and the accretion model for AXPs and SGRs. We explain how this null observation of AXP 4U 0142+61 favors the accretion model. Future Fermi/LAT observations of AXP 1E 1547.0−5408 and AXP 1E 1048.1−5937 are highly recommended.

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“…The polar cap/slot gap and the outer gap models both use curvature radiation to produce the primary γ rays with energies around 50 GeV to initiate the cascades [24] [7], but they differ in the pair creation process: magnetic onephoton production in the intense field at low altitude, and two-photon creation in the outer regions. Due to screening of the E by the pair cascades, the maximum Lorentz factor γ e,max saturates at several 10 7 for both the polar cap and outer gap and is very insensitive to Ω andΩ.…”

Section: Cascades and Radiationmentioning

confidence: 99%

Pulsar twinkling and relativity

Grenier¹,

Harding²

2006

AIP Conference Proceedings

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Abstract. The number of pulsars with detected emission at X-ray and γ-ray energies has been steadily growing, showing that beams of high-energy particles are commonly accelerated in pulsar magnetospheres, even though the location and number of acceleration sites remain unsettled. Acceleration near the magnetic poles, close to the polar cap surface or to higher altitudes in the slot gap along the last open field lines, involves an electric field component due to inertial-frame dragging. Acceleration can also take place in the outer magnetosphere where charge depletion due to global currents causes a large electric field along the magnetic field lines. All models require a detailed knowledge of the open magnetosphere geometry and its relativistic distortions. Observational trends with age, spin-down power and magnetic field as well as population synthesis studies in the Galactic disc and the nearby Gould Belt provide useful, however not yet conclusive, constraints on the competing models.

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One-dimensional electric field structure of an outer gap accelerator -- III. Location of the gap and the gamma-ray spectrum

Cited by 40 publications

References 68 publications

High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

NON-DETECTION IN A FERMI /LAT OBSERVATION OF AXP 4U 0142+61: MAGNETARS?

Pulsar twinkling and relativity

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