[ITAL]Chandra[/ITAL] Observation of Supernova Remnant G54.1+0.3: A Close Cousin of the Crab Nebula

Lu, F. J.; Wang, Q. Daniel; Aschenbach, B.; Durouchoux, Ph.; Song, Liming

doi:10.1086/340137

Cited by 112 publications

(139 citation statements)

References 14 publications

(30 reference statements)

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“…Similar geometric structures are observed in G54.1+0.3, for which Chandra observations reveal a central point-like source surrounded by an X-ray ring whose geometry suggests an inclination angle of about 45 • (Lu et al 2002). The X-ray emission is brightest along the eastern limb of the ring.…”

Section: Formation Of Tori Jets and Wispssupporting

confidence: 71%

The Evolution and Structure of Pulsar Wind Nebulae

Gaensler

Slane

2006

Annu. Rev. Astron. Astrophys.

822

809

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Pulsars steadily dissipate their rotational energy via relativistic winds.Confinement of these outflows generates luminous pulsar wind nebulae, seen across the electromagnetic spectrum in synchrotron and inverse Compton emission, and in optical emission lines when they shock the surrounding medium. These sources act as important probes of relativistic shocks, particle acceleration and of interstellar gas. We review the many recent advances in the study of pulsar wind nebulae, with particular focus on the evolutionary stages through which these objects progress as they expand into their surroundings, and on morphological structures within these nebulae which directly trace the physical processes of particle acceleration and outflow. We conclude by considering some exciting new probes of pulsar wind nebulae, including the study of TeV gamma-ray emission from these sources, and observations of pulsar winds in close binary systems.

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Section: Formation Of Tori Jets and Wispssupporting

confidence: 71%

The Evolution and Structure of Pulsar Wind Nebulae

Gaensler

Slane

2006

Annu. Rev. Astron. Astrophys.

822

809

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“…References.-(T) This paper; (1) Roberts et al 1993; (2) Gotthelf et al 2002;(19) Koribalski et al 1995;(20) Gaensler et al 2004;(21) Kaspi et al 2001;(22) Kargaltsev & Pavlov 2007;(23) Roberts et al 2003;(24) Green et al 1988;(25) Leahy & Tian 2008;(26) Petre et al 2002;(27) Cox et al 1999;(28) Lu et al 2002;(29) Strom & Stappers 2000;(30) Kothes et al 2006. In order to evaluate the significance level of the correlations of the two parameters concerned, we calculate the widely used Pearson correlation coefficient (r), the Spearman rank correlation coefficient (r S ), and the two-sided significance level ( p S ) of the Spearman rank test. The results are listed in Table 3.…”

Section: Analyses and Resultsmentioning

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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“…Using Chandra data, Lu et al (2002) clearly detected a torus of ∼10 in diameter, and a feature elongated in the E and W directions, which could be ascribed to X-ray jets. From these data, the size of the X-ray nebula appears ∼1 , but the outer part of the nebula is very faint, its edge being poorly defined.…”

Section: Introductionmentioning

confidence: 99%

XMM-NewtonandSUZAKUdetection of an X-ray emitting shell around the pulsar wind nebula G54.1+0.3

Bocchino¹,

Bandiera

Gelfand

2010

A&A

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Context. X-ray observations have proven to be very effective in detecting previously unknown supernova remnant shells around pulsar wind nebulae (PWNe), and in these cases the characteristics of the shell provide information about the evolutionary stage of the embedded PWN. However, it is not clear why some PWNe are "naked". Aims. We perform an X-ray observational campaign targeting the PWN G54.1+0.3, the "close cousin" of the Crab Nebula, to try to detect the associated SNR shell. Methods. We analyze XMM-Newton and Suzaku observations of G54.1+0.3 to model the contribution of a dust scattering halo. Results. We detecte an intrinsic faint diffuse X-ray emission surrounding the PWN out to ∼6 (∼10 pc) from the pulsar, characterized by a hard spectrum, which can be modeled with either a power law (γ = 2.9) or a thermal plasma model (kT = 2.0 keV.) Conclusions. Assuming the shell to be thermal, we derive an explosion energy E = 0.5−1.6 × 10 51 erg, a pre-shock ISM density of 0.2 cm −3 , and an age of ∼2000 yr. Using these results in the MHD model of PWN-SNR evolution, we obtain excellent agreement between the predicted and observed location of the shell and PWN shock.

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[ITAL]Chandra[/ITAL] Observation of Supernova Remnant G54.1+0.3: A Close Cousin of the Crab Nebula

Cited by 112 publications

References 14 publications

The Evolution and Structure of Pulsar Wind Nebulae

The Evolution and Structure of Pulsar Wind Nebulae

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

XMM-NewtonandSUZAKUdetection of an X-ray emitting shell around the pulsar wind nebula G54.1+0.3

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