Pulsars, X-ray synchrotron nebulae, and guest stars

Abstract. We performed timing and spectral analyses for PSR B1929+10, one of the oldest (∼10 7 years) of the ordinary pulsars detected in X-rays, using archival ROSAT, ASCA and RXTE data. Pulsed emission was detected at a more than five sigma level for the combined ROSAT PSPC-B and previously unpublished HRI data. Our pulse profile is in agreement with that obtained by Yancopoulos et al. (1994, ApJ, 429, 832, ROSAT PSPC-B) but now with better statistics. The pulsed fraction in the ROSAT X-ray band is 0.25 ± 0.04. The pulsed signal has also been detected in the ASCA GIS data (0.5-5 keV) with a similar pulsed fraction of 0.36 ± 0.11. No significant timing signal is found in the RXTE PCA data (>2 keV). We found that the combined ROSAT PSPC-B and ASCA GIS spectrum can satisfactorily be described by a power-law as well as by a double black-body model but not by a single black-body model or black-body plus power law model. Fitting the combined ROSAT/ASCA 0.1-10 keV spectrum by a power-law model we obtain a photon index α of 2.54 ± 0.12 and a neutral hydrogen column density N H towards the source of 9.8 +1.4 −1.0 × 10 20 cm −2 . For a double black-body fit our results are T 1 = 2.0 +0.05 −0.05 × 10 6 K, T 2 = 6.9 +0.23 −0.35 × 10 6 K and N H = 4.4 +2.1 −1.1 × 10 20 cm −2 . In both cases the derived value of N H is higher than that adopted in earlier works, but our result is fully consistent with the larger distance estimate of 331 ± 10 pc from parallax measurements combined with the hydrogen distribution measurements in the direction to the pulsar.

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“…This value is compatible with e.g. the (L X, (0.1−2.4 keV) ,Ė) relation found by Seward et al (1988) and later confirmed by Verbunt et al (1996).…”

Section: Spectral Analysissupporting

confidence: 91%

PSR B1929+10 revisited in X-rays

Słowikowska¹,

Kuiper

Hermsen

2005

A&A

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“…The ratio L x /L r = 28, which is about a factor of 5 lower than that of the Crab but again similar to that of G21.5-0.9 (Helfand & Becker 1987). Seward & Wang (1988) have shown that a relation between X-ray luminosity L X of a plerionic SNR and rate of loss of rotational energy (Ė) of the central pulsar appears to exist. Using their relation we deriveĖ ∼1.6 10 37 erg s…”

Section: Distance and X-ray Luminosity Of G541+03supporting

confidence: 59%

Observations of the supernova remnant G54.1+0.3: X-ray spectrum and evidence for an X-ray jet

Aschenbach

Song

2001

A&A

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Abstract. We present analyses of the ROSAT PSPC and the ASCA SIS and GIS observations of the Crab-like supernova remnant (SNR) G54.1+0.3. The spectrum is best fitted by a power law model with a photon index of -1.9 , where d10 is the distance in 10 kpc. With an image restoration method, we have deconvolved the X-ray image of the remnant. There is evidence for an X-ray jet pointing to the north-east with a length of about 40 measured from the center of the nebula. Its X-ray luminosity in the 0.1-2.4 keV range is about 2.1 10 34 d 2 10 erg s −1 . The X-ray jet is consistent with the radio extension of G54.1+0.3 to the north-east in both direction and position.

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“…After correcting for the difference in distances to the two remnants, the inferred X-ray intensity for the putative plerionic clump in E0102.2-72.2 is about a factor of 10 less than the intensity of the known plerion in E0540-69.3. Using the empirical relationship between the spin-down energy loss rate for a pulsar, E, and the Xray luminosity of its associated plerion (Seward & Wang 1988) I estimate E to be ~10 37 -5 erg s" 1 for the putative pulsar in E0102.2-72.2. The period can also be estimated; a value of ~0.14 s is indicated, assuming an age of 1000 yr and the E given above.…”

Section: Discussionmentioning

confidence: 99%

ROSAT HRI observations of Magellanic Cloud supernova remnants

Hughes¹

1994

AIP Conference Proceedings

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Analysis of deep ROSAT high, resolution imager (HRI) observations of two oxygen-rich supernova remnants (SNRs) in the Magellanic Clouds is described. For N132D, I exploit the limited spectral information provided by the HRI to investigate arcsecond scale spectral variations. I find that there is a region of harder X-ray emission near the southern limb and regions of softer emission near the center and northwestern limb. The remnant is believed to be interacting with a molecular cloud and the harder emission to the south is explained as a result of increased absorption along the line-of-sight there. I argue that the softer emission comes from X-ray emitting material with an enhanced abundance of oxygen. For the second SNR, E0102.2-72.2, the spatial structure is investigated in detail using two-dimensional image fitting techniques. Evidence is found for a ring-like and a spherically symmetric shell-like component both of which were modeled as homogeneous regions. In addition, a significant fraction of the observed flux (~11%) must come from a resolved clumped component. A comparison with optical and radio imagery is made to provide a physical basis for the components identified in the X-ray analysis. The mass of X-ray emitting gas in the remnant is estimated and a value of ~75 MQ was determined. The dominant uncertainty on this quantity is the extent of unresolved clumping in the X-ray gas. Such clumping would tend to reduce the mass estimate by / a / 2 , where / is the mean volume filling factor of the gas.

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Pulsars, X-ray synchrotron nebulae, and guest stars

Cited by 173 publications

References 0 publications

PSR B1929+10 revisited in X-rays

PSR B1929+10 revisited in X-rays

Observations of the supernova remnant G54.1+0.3: X-ray spectrum and evidence for an X-ray jet

ROSAT HRI observations of Magellanic Cloud supernova remnants

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