Heated Polar Caps in PSR 0656+14 and PSR 1055−52

Greiveldinger, C.; Camerini, U.; Fry, William F.; Markwardt, C.; Öğelman, H.; Safi‐Harb, Samar; Finley, J. P.; Tsuruta, S.; Shibata, Shinpei; Sugawara, T.; Sano, Shigeru; Tukahara, M.

doi:10.1086/310132

Cited by 80 publications

(94 citation statements)

References 19 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We have assumed d ¼ 5 kpc, but the conclusion of a small emitting region R s TR ns holds even if the distance is twice that value. The ratio of source-emitting area to stellar surface area R s /R ns ð Þ 2 $ 10 À3 obtained here is comparable to that obtained for some field pulsars with magnetic field strengths below the magnetar range (e.g., Greiveldinger et al 1996), but is smaller than the typical ratio R s /R ns ð Þ 2 $ 10 À1 derived for the AXPs studied by Durant & van Kerkwijk (2006).…”

Section: Discussionsupporting

confidence: 82%

TheChandraX‐Ray Spectrum of the 10.6 s Pulsar in Westerlund 1: Testing the Magnetar Hypothesis

Skinner¹,

Perna²,

Zhekov³

2006

ApJ

View full text Add to dashboard Cite

Two sensitive Chandra X-ray observations of the heavily reddened Galactic starburst cluster Westerlund 1 in 2005 May and June detected a previously unknown X-ray pulsar (CXO J164710.20À455217). Its slow 10.6 s pulsations, moderate X-ray temperature, kT % 0:5 keV, and apparent lack of a massive companion tentatively suggest that it is an anomalous X-ray pulsar (AXP). An isothermal blackbody model yields an acceptable spectral fit, but the inferred source radius is much less than that of a neutron star, a result that has also been found for other AXPs. We analyze the X-ray spectra with more complex models, including a model that assumes the pulsar is a strongly magnetized neutron star (''magnetar'') with a light-element atmosphere. We conclude that the observed X-ray emission cannot be explained as global surface emission arising from the surface of a cooling neutron star or a magnetar. The emission likely arises in one or more localized regions (''hot spots'') covering a small fraction of the surface. We discuss these new results in the context of both accretion and magnetar interpretations for the X-ray emission.

show abstract

Section: Discussionsupporting

confidence: 82%

TheChandraX‐Ray Spectrum of the 10.6 s Pulsar in Westerlund 1: Testing the Magnetar Hypothesis

Skinner¹,

Perna²,

Zhekov³

2006

ApJ

View full text Add to dashboard Cite

show abstract

“…tospheric origin (Halpern & Wang 1997). Similar results have been reported for 1055-52 (Wang et al 1998) and PSR 0656+14 (Greiveldinger et al 1996), although in the latter case the limited photon statistics prevents a clear distinction between a thermal and non-thermal origin of the harder emission.…”

Section: T H E Cooling Neutron Starssupporting

confidence: 78%

X-ray emission characteristics of pulsars and their nebulae

Becker

2000

International Astronomical Union Colloquium

View full text Add to dashboard Cite

Recent X-ray observatories like ROSAT, ASCA, RXTE, BeppoSAX and Chandra have achieved important progress in neutron star and pulsar astronomy. The identification of Geminga as a rotation-powered pulsar, the discovery of X-ray emission from millisecond pulsars and the identification of cooling neutron stars are only few of the fascinating results. In the following I will give a brief review on the X-ray emission properties of rotation-powered pulsars and their wind nebulae.

show abstract

“…The X-ray spectrum is complex and at least two components are necessary to achieve an acceptable fit: one is a blackbody while the other is not safely established and can be either a power law or another blackbody with higher temperature. Greiveldinger et al (1996) prefer the two blackbody spectrum, with temperatures of 7.9 × 10 5 K and 3.7 × 10 6 K; the power-law component would have a photon index of 3-4 larger than the values measured in other pulsars. At variance, Wang et al (1998) give a flatter power-law fit with an index of 1.5 ± 0.3.…”

Section: Introductionmentioning

confidence: 83%

BeppoSAX observations of the three Gamma-ray pulsars PSR B0656+14, PSR B1055-52 and PSR B1706-44

Mineo

Massaro

Cusumano

et al. 2002

A&A

View full text Add to dashboard Cite

Abstract.We report the results of the observations of the three γ-ray pulsars PSR B0656+14, PSR B1055−52 and PSR B1706−44 performed with BeppoSAX. We detected a pulsed emission only for PSR B1055−52: in the range 0.1-6.5 keV the pulse profile is sinusoidal and the statistical significance is 4.5σ. The pulsed fraction was estimated 0.64 ± 0.17. This pulsation was detected also at energies greater than 2.5 keV suggesting either a non-thermal origin or a quite high temperature region on the neutron star surface. Spectral analysis showed that only the X-ray spectrum of PSR B1706−44 can be fitted by a single power-law component, while that of PSR B1055−52 requires also a blackbody component (kT = 0.075 keV) and that of PSR B0656+14 two blackbody components (kT 1 = 0.059, kT 2 = 0.12 keV).

show abstract

Heated Polar Caps in PSR 0656+14 and PSR 1055−52

Cited by 80 publications

References 19 publications

TheChandraX‐Ray Spectrum of the 10.6 s Pulsar in Westerlund 1: Testing the Magnetar Hypothesis

TheChandraX‐Ray Spectrum of the 10.6 s Pulsar in Westerlund 1: Testing the Magnetar Hypothesis

X-ray emission characteristics of pulsars and their nebulae

BeppoSAX observations of the three Gamma-ray pulsars PSR B0656+14, PSR B1055-52 and PSR B1706-44

Contact Info

Product

Resources

About