Chandra observations of two pulsars PSR 0628-28 and PSR 1813-36

Öğelman, H.; Tepedelenlioǧlu, E.

doi:10.1016/j.asr.2003.02.018

Cited by 4 publications

(4 citation statements)

References 3 publications

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“…The 2.8-Myr-old pulsar B0628-28 is the most puzzling object of this group because it was found to be extremely luminous in the X-ray domain ( Ögelman & Tepedelenlioǧlu 2004). Our analysis of the 20-ks ACIS data of 2001 November shows that the source spectrum is best fitted with a PL model of Γ = 2.73, which is surprisingly steep for a spin-powered pulsar.…”

Section: X-rays From Other Old Pulsarsmentioning

confidence: 74%

“…Another 3-Myr-old pulsar, B1813-36, was not detected in a 30 ks Chandra ACIS exposure of 2001 October ( Ögelman & Tepedelenlioǧlu 2004). An upper limit on its X-ray efficiency, η nonth 2−10 keV < 4.4 × 10 −4 , is a factor of 2.5 lower than that for PSR B0950+08.…”

Section: X-rays From Other Old Pulsarsmentioning

confidence: 96%

“…The bolometric PC efficiency is defined as η pc = L pc bol /(2 Ė). The X-ray parameters of PSRs B1813-36 and B1929+10 are from Ögelman & Tepedelenlioǧlu (2004) and Wang & Halpern (1997), respectively, whereas those for the other pulsars are from this work. The upper limits on L nonth are derived with a PL model of photon index Γ = 1.5.…”

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confidence: 97%

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X‐Ray Emission from the Old Pulsar B0950+08

Zavlin

Pavlov

2004

ApJ

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We present the timing and spectral analyses of the XMM-Newton data on the 17-Myr-old, nearby radio pulsar B0950+08. This observation revealed pulsations of the X-ray flux of PSR B0950+08 at its radio period, P ≃ 253 ms. The pulse shape and pulsed fraction are apparently different at lower and higher energies of the observed 0.2-10 keV energy range, which suggests that the radiation cannot be explained by a single emission mechanism. The X-ray spectrum of the pulsar can be fitted with a power-law model with a photon index Γ = 1.75 ± 0.15 and an (isotropic) luminosity L X = (9.8 ± 0.2) × 10 29 erg s −1 in the 0.2-10 keV. Better fits are obtained with two-component, power-law plus thermal, models with Γ = 1.30 ± 0.10 and L X = (9.7 ± 0.1) × 10 29 erg s −1 for the power-law component that presumably originates from the pulsar's magnetosphere. The thermal component, dominating at E < ∼ 0.7 keV, can be interpreted as radiation from heated polar caps on the neutron star surface covered with a hydrogen atmosphere. The inferred effective temperature, radius, and bolometric luminosity of the polar caps are T pc ≈ 1 MK, R pc ≈ 250 m, and L pc ≈ 3 × 10 29 erg s −1 . Optical through X-ray nonthermal spectrum of the pulsar can be described as a single power-law with Γ = 1.3-1.4 for the two-component X-ray fit. The ratio of the nonthermal Xray (1-10 keV) luminosity to the nonthermal optical (4000-9000Å) luminosity, ≈ 360, is within the range of 10 2 -10 3 observed for younger pulsars, which suggests that the magnetospheric X-ray and optical emissions are powered by the same mechanism in all pulsars, independent of age and spin-down power. Assuming a standard neutron star radius, the upper limit on the temperature of the bulk of the neutron star surface, inferred from the optical and X-ray data, is about 0.15 MK. We also analyze X-ray observations of several other old pulsars, B2224+65, J2043+2740, B0628-28, B1813-36, B1929+10, and B0823+26, and compare their properties with the those of PSR B0950+08.

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Section: X-rays From Other Old Pulsarsmentioning

confidence: 74%

Section: X-rays From Other Old Pulsarsmentioning

confidence: 96%

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X‐Ray Emission from the Old Pulsar B0950+08

Zavlin

Pavlov

2004

ApJ

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“…In Table 2 Camilo et al (2004) suggested that PSR J1016À5857 is too faint to be resolved from its background PWN in the Chandra observation, and Hessels et al (2004) found that the spectrum of PSR J2021+3651 can be fit by a BB model and is thus dominated by thermal components. On the other hand, 5 out of the 27 RPP samples in Table 1 are not listed in Table 2 for PWNe, because 5 pulsars have no PWN reported: B0628À28, B0656+14, B0823+26, B0950+08, and B1055À52 (Ö gelman & Tepedelenlioǧlu 2004;Becker et al 2004;De Luca et al 2005).…”

Section: Sample and Data Processingmentioning

confidence: 99%

Nonthermal X‐Ray Properties of Rotation‐powered Pulsars and Their Wind Nebulae

2008

ApJ

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We present a statistical study of the nonthermal X-ray emission of 27 young rotation-powered pulsars (RPPs) and 24 pulsar wind nebulae ( PWNe) using the Chandra and XMM-Newton observations, whose high spatial resolutions enable us to resolve pulsars from their surrounding PWNe. We obtain the X-ray luminosities and spectra separately for RPPs and PWNe, and then investigate their distribution and relation to each other, as well as their relation to the pulsar rotational parameters. In pair-correlation analysis we find that (1) the X-ray (2-10 keV) luminosities of both pulsar and PWN (L X; psr and L X; pwn ) display a strong correlation with the pulsar spin-down powerĖ and characteristic age . The scalings resulting from a simple linear fit to the data are L X; psr /Ė 0:92AE0:04 and L X; pwn /Ė 1:45AE0:08 (68% confidence level ), respectively; however, neither fit is statistically acceptable. (2) L X; psr also shows a possible weak correlation with the pulsar period P and period derivativeṖ, whereas L X; pwn manifests a similar weak correlation withṖ only. (3) The PWN photon index À pwn is positively correlated with L X; pwn and L X; pwn /Ė. We also found that the PWN X-ray luminosity is typically 1 to 10 times larger than that from the underlying pulsar, and the PWN photon indices span a range of 1:5 P À pwn P 2:1. The statistical study of PWN spectral properties supports a particle wind model in which the X-rayemitting electrons are accelerated by the termination shock of the wind.

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Chandra and XMM - Newton Observations of the Exceptional Pulsar B0628-28

Tepedelenlioǧlu¹,

Öğelman²

2005

ApJ

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Chandra observations of two pulsars PSR 0628-28 and PSR 1813-36

Cited by 4 publications

References 3 publications

X‐Ray Emission from the Old Pulsar B0950+08

X‐Ray Emission from the Old Pulsar B0950+08

Nonthermal X‐Ray Properties of Rotation‐powered Pulsars and Their Wind Nebulae

Chandra and XMM - Newton Observations of the Exceptional Pulsar B0628-28

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