Figs. 49 - 63

Arons, R. R.

doi:10.1007/10013330_67

Cited by 14 publications

(21 citation statements)

References 7 publications

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“…This proportionality would be expected if either (1) all pulsars accelerate particles to the same energy but the particle current differs from pulsar to pulsar or (2) the particle flow is constant, with different pulsars accelerating particles to different energies (Thompson et al 1997). As noted by Arons (1996), this simple trend cannot extend to much lower values of V orṄ, because more than 100% efficiency for conversion of spin-down luminosity would be implied. Nevertheless, Fig.…”

Section: High-energy Luminositymentioning

confidence: 90%

Gamma Radiation from PSR B1055−52

Thompson¹,

Bailes²,

Bertsch³

et al. 1999

ApJ

129

107

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The telescopes on the Compton Gamma Ray Observatory (CGRO) have observed PSR B1055−52 a number of times between 1991 and 1998. From these data, a more detailed picture of the gamma radiation from this source has been developed, showing several characteristics which distinguish this pulsar: the light curve is complex; there is no detectable unpulsed emission; the energy spectrum is flat, with no evidence of a sharp high-energy cutoff up to >4 GeV. Comparisons of the gamma-ray data with observations at longer wavelengths show that no two of the known gamma-ray pulsars have quite the same characteristics; this diversity makes interpretation in terms of theoretical models difficult.

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Section: High-energy Luminositymentioning

confidence: 90%

Gamma Radiation from PSR B1055−52

Thompson¹,

Bailes²,

Bertsch³

et al. 1999

ApJ

129

107

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“…The wind from the Crab pulsar carries away most of the energy of rotation of the pulsar. The energy released in the form of electromagnetic emission of the pulsar, which peaks at g-ray energies, does not exceed 1 per cent of the total rotational losses (Arons 1996), therefore it can be neglected in the energy balance of the wind.…”

Section: H a R Ac T E R I S T I C S O F T H E W I N Dmentioning

confidence: 99%

“…This leads to a conclusion that most of the pulsar's rotational energy is carried off by the electromagnetic field (see e.g. (Arons 1996). The state of the wind is characterized by the so-called s-parameter, determined as the ratio of the electromagnetic energy flux to the kinetic energy flux of particles in the wind.…”

Section: H a R Ac T E R I S T I C S O F T H E W I N Dmentioning

confidence: 99%

Very-high-energy gamma radiation associated with the unshocked wind of the Crab pulsar

Bogovalov

Aharonian

2000

Monthly Notices of the Royal Astronomical Society

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We show that the relativistic wind of the Crab pulsar, which is commonly thought to be invisible in the region upstream of the termination shock at rrS∼0.1 pc, in fact could be directly observed through its inverse Compton (IC) γ‐ray emission. This radiation is caused by illumination of the wind by low‐frequency photons emitted by the pulsar, and consists of two, pulsed and unpulsed, components associated with the non‐thermal (pulsed) and thermal (unpulsed) low‐energy radiation of the pulsar, respectively. These two components of γ‐radiation have distinct spectral characteristics, which depend essentially on the site of formation of the kinetic‐energy‐dominated wind, as well as on the Lorentz factor and the geometry of propagation of the wind. Thus, the search for such specific radiation components in the spectrum of the Crab Nebula can provide unique information about the unshocked pulsar wind that is not accessible at other wavelengths. In particular, we show that the comparison of the calculated flux of the unpulsed IC emission with the measured γ‐ray flux of the Crab Nebula excludes the possibility of formation of a kinetic‐energy‐dominated wind within 5 light‐cylinder radii of the pulsar, Rw5RL. The analysis of the pulsed IC emission, calculated under reasonable assumptions concerning the production site and angular distribution of the optical pulsed radiation, yields even tighter restrictions, namely Rw30RL.

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“…It also reproduces the empirical trend in L γ for seven pulsars detected with Compton Gamma Ray Observatory (CGRO ) experiments. At the same time it avoids basic difficulties (Nel et al 1996, Arons 1996 faced by theoretical models when confronted with observational constraints.We show that the classical and millisecond pulsars form two distinct branches in the L γ -L sd diagram (where L sd is the spin-down luminosity). In particular, we explain why the millisecond pulsar J0437-4715 has not been detected with any of the CGRO instruments despite its very high position in the ranking list of spin-down fluxes (i.e.…”

mentioning

confidence: 96%

mentioning

confidence: 96%

The efficiency of gamma-ray emission from pulsars

Rudak

Dyks²

1998

Monthly Notices of the Royal Astronomical Society

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We present a modified scenario of gamma-ray emission from pulsars within the framework of polar cap models. Our model incorporates possible acceleration of electron-positron pairs created in magnetospheres, and their subsequent contribution to gamma-ray luminosity L_\gamma. It also reproduces the empirical trend in L_\gamma for seven pulsars detected with Compton Gamma Ray Observatory (CGRO) experiments. At the same time it avoids basic difficulties (Nel et al. 1996, Arons 1996) faced by theoretical models when confronted with observational constraints. We show that the classical and millisecond pulsars form two distinct branches in the L_gamma - L_sd diagram (where L_sd is the spin-down luminosity). In particular, we explain why the millisecond pulsar J0437-4715 has not been detected with any of the CGRO instruments despite its very high position in the ranking list of spin-down fluxes (i.e. L_sd/D^2, where D is a distance). The gamma-ray luminosity predicted for this particular object is about one order of magnitude below the upper limit set by EGRET.Comment: 7 pages, 4 figures, Latex, mn.sty, epsf.sty. MNRAS in the pres

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Figs. 49 - 63

Cited by 14 publications

References 7 publications

Gamma Radiation from PSR B1055−52

Gamma Radiation from PSR B1055−52

Very-high-energy gamma radiation associated with the unshocked wind of the Crab pulsar

The efficiency of gamma-ray emission from pulsars

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