Search for the optical counterparts of the<i>γ</i>-ray pulsars J2055+2539, J2043+2740, J1957+5033

Beronya, D. M.; Shibanov, Yu. A.; Zyuzin, D. A.; Komarova, V. N.

doi:10.1088/1742-6596/661/1/012001

Cited by 6 publications

(4 citation statements)

References 4 publications

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“…Note that the cyan triangles are lower limits on Fγ/Fopt in the right panel. Data are taken from Abdo et al (2013); Marelli et al (2015); Beronya et al (2015). Blue curves are the ratio Lcur/Lsyn in γγ scenario, which is calculated from equations ( 43) and ( 45).…”

Section: Luminosity Ratiomentioning

confidence: 99%

Efficiency of Synchrotron Radiation from Rotation-powered Pulsars

Kisaka

Tanaka

2017

ApJ

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Synchrotron radiation is widely considered as the origin of the pulsed non-thermal emissions from rotation-powered pulsars in optical and X-ray bands. In this paper, we study the synchrotron radiation emitted by the created electron and positron pairs in the pulsar magnetosphere to constrain on the energy conversion efficiency from the Poynting flux to the particle energy flux. We model two pair creation processes, two-photon collision which efficiently works in young γ-ray pulsars ( 10 6 yr), and magnetic pair creation which is the dominant process to supply pairs in old pulsars ( 10 6 yr). Using the analytical model, we derive the maximum synchrotron luminosity as a function of the energy conversion efficiency. From the comparison with observations, we find that the energy conversion efficiency to the accelerated particles should be an order of unity in the magnetosphere, even though we make a number of the optimistic assumptions to enlarge the synchrotron luminosity. In order to explain the luminosity of the non-thermal X-ray/optical emission from pulsars with low spin-down luminosity L sd 10 34 erg s −1 , non-dipole magnetic field components should be dominant at the emission region. For the γ-ray pulsars with L sd 10 35 erg s −1 , observed γ-ray to X-ray and optical flux ratios are much higher than the flux ratio between curvature and the synchrotron radiations. We discuss some possibilities such as the coexistence of multiple accelerators in the magnetosphere as suggested from the recent numerical simulation results. The obtained maximum luminosity would be useful to select observational targets in X-ray and optical bands.

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Section: Luminosity Ratiomentioning

confidence: 99%

Efficiency of Synchrotron Radiation from Rotation-powered Pulsars

Kisaka

Tanaka

2017

ApJ

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“…Therefore, the distance based on the dispersion measure is usually adopted: d = 1.8 kpc in early works (Becker et al 2004;Zavlin & Pavlov 2004;Zavlin 2009) or d = 1.48 kpc in more recent papers (Testa et al 2018). This pulsar has also been observed in gamma rays (Abdo et al 2013) and in optical bands (Beronya et al 2015;Testa et al 2018); its multiwavelength optical-to-gamma spectrum has been discussed by Testa et al (2018). There was only one 12-ks observation of this pulsar in X-rays by XMM-Newton in 2002, which gathered about one hundred counts.…”

Section: Upper Limits On Cooling-powered Thermal Emissionmentioning

confidence: 99%

Thermal luminosities of cooling neutron stars

Potekhin,

Zyuzin,

Yakovlev

et al. 2020

Preprint

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Ages and thermal luminosities of neutron stars, inferred from observations, can be interpreted with the aid of the neutron star cooling theory to gain information on the properties of superdense matter in neutron-star interiors. We present a survey of estimated ages, surface temperatures and thermal luminosities of middle-aged neutron stars with relatively weak or moderately strong magnetic fields, which can be useful for these purposes. The catalogue includes results selected from the literature, supplemented with new results of spectral analysis of a few cooling neutron stars. The data are compared with the theory. We show that overall agreement of theoretical cooling curves with observations improves substantially for models where neutron superfluidity in stellar core is weak.

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“…PSR J1813-1246 was discovered in a blind search during the first three months of Fermi/LAT scanning (Abdo et al 2009) (Beronya et al 2015), and no conclusive optical counterpart (V > 20.13) or H α bow shock emission could be identified. According to the timing parameters determined by Fermi data, PSR J1813-1246 is the known RQ γ-ray pulsar with the fastest spin period and the second most energetic spin-down power while PSR J2055+2539 has the lowest spin-down power (that is compatible to Morla) among the known Gemingalike pulsars.…”

Section: Rq γ-Ray Pulsar With Only Non-thermal X-ray Pulsation -Psr Jmentioning

confidence: 99%

Radio-quiet Gamma-ray Pulsars

Lin¹

2016

Journal of Astronomy and Space Sciences

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Search for the optical counterparts of theγ-ray pulsars J2055+2539, J2043+2740, J1957+5033

Cited by 6 publications

References 4 publications

Efficiency of Synchrotron Radiation from Rotation-powered Pulsars

Efficiency of Synchrotron Radiation from Rotation-powered Pulsars

Thermal luminosities of cooling neutron stars

Radio-quiet Gamma-ray Pulsars

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