Low-Energy Diffuse X-Rays

Bunner, A. N.; Coleman, P.L.; Kraushaar, W. L.; McCammon, D.

doi:10.1086/180749

Cited by 36 publications

(16 citation statements)

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“…The spatial profile of γ-ray emission around PSR B0656+14 was reported by HAWC along with that of Geminga, and the indicated diffusion coefficient is 5 times larger compared with the Geminga case (Abeysekara et al 2017a). While unlike Geminga, the associated SNR of PSR B0656+14, namely the Monogem Ring, is still observable in X-ray (Bunner et al 1971;Plucinsky et al 1996), as it is much younger than Geminga (∼100 kyr). The position of PSR B0656+14 on the sky map is well inside the Monogem Ring, while the observation of the PWN of PSR B0656+14 suggests that the motion of the pulsar is almost parallel to the line of sight (Bîrzan et al 2016).…”

Section: Other Tev Halosmentioning

confidence: 97%

Possible origin of the slow-diffusion region around Geminga

Fang

Yin

2019

Monthly Notices of the Royal Astronomical Society

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Geminga pulsar is surrounded by a multi-TeV γ-ray halo radiated by the high energy electrons and positrons accelerated by the central pulsar wind nebula (PWN). The angular profile of the γ-ray emission reported by HAWC indicates an anomalously slow diffusion for the cosmic-ray electrons and positrons in the halo region around Geminga. In the paper we study the possible mechanism for the origin of the slow diffusion. At first, we consider the self-generated Alfvén waves due to the streaming instability of the electrons and positrons released by Geminga. However, even considering a very optimistic scenario for the wave growth, we find this mechanism DOES NOT work to account for the extremely slow diffusion at the present day if taking the proper motion of Geminga pulsar into account. The reason is straightforward as the PWN is too weak to generate enough high energy electrons and positrons to stimulate strong turbulence at the late time. We then propose an assumption that the strong turbulence is generated by the shock wave of the parent supernova remnant (SNR) of Geminga. Geminga may still be inside the SNR, and we find that the SNR can provide enough energy to generate the slow-diffusion circumstance. The TeV halos around PSR B0656+14, Vela X, and PSR J1826-1334 may also be explained under this assumption.

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Section: Other Tev Halosmentioning

confidence: 97%

Possible origin of the slow-diffusion region around Geminga

Fang

Yin

2019

Monthly Notices of the Royal Astronomical Society

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“…Nevertheless, considerable evidence has accumulated for a soft excess of Galactic origin in the CXB spectrum (e.g. Bunner et al 1971;Garmire et al 1992). The fact that the EPIC cameras identify the spectral break in the CXB in such a convincingly and unambiguous fashion does, however, demonstrate the importance of broad spectral coverage for CXB measurements.…”

Section: Extragalactic Cosmic X-ray Backgroundmentioning

confidence: 99%

X-ray background measurements with XMM-Newton EPIC

Lumb

Warwick

Page

et al. 2002

A&A

376

466

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Abstract. We discuss the methods used to compile a high signal-to-noise dataset representative of both the instrumental and cosmic background signal measured at high galactic latitude by the XMM-Newton EPIC cameras. The characteristics of the EPIC background are described and the potential applications of the derived dataset in general science analysis are outlined. In the case of the cosmic X-ray background, the transition between a hard power-law spectrum (due to the integrated emission of unresolved, largely extragalactic, point sources) and a softer thermal spectrum (produced by hot plasma associated with the Galactic plane and halo) is unambiguously detected around ∼1 keV. We derive a value for the intensity of the power-law component of 2.15 ± 0.26 × 10 −11 erg cm −2 s −1 deg −2 in the 2-10 keV band (normalisation at 1 keV of 11.1 photons cmThe implication is that recent, very deep Chandra observations have resolved ∼70-90% of the 2-10 keV background into discrete sources. Our measurement is towards the higher end of the range of quoted background normalisations.

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“…In the 1-10 keV region there is very good agreement between various groups (Boldt et al, 1969;Ducros et al, 1970;Bunner et al, 1971;Shukla and Wilson, 1971;Shulman et al, 1971;and Toor et al, 1972) as to the spectrum of the diffuse back ground. A power law representation, A E~y photons (cm 2 s ster keV)" 1 , is fit by these groups to their data.…”

Section: Recent Observations Of the (01-1 Kev) X-ray Backgroundmentioning

confidence: 66%

The Soft X-Ray Background

Friedman¹,

Fritz²,

Shulman³

et al. 1973

Symp. - Int. Astron. Union

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Abstract. A survey of soft X-ray background observations in the 0.1-10 keV range is presented. In the region above 1 keV, recent results on point X-ray sources are discussed and their integrated contri bution to the diffuse background is estimated. However, the average luminosity of various classes of extragalactic X-ray sources is still not sufficiently well known to permit this estimate to be made with any certainty. A discussion is given of recent observations at energies below 1 keV where the effects of interstellar absorption are important. It is argued that although some fraction of the background radiation in the 0.1-1 keV range must be galactic in origin, there is still substantial evidence for an extragalactic component. Proposed theories for generating both the galactic and extragalactic X-ray background are briefly reviewed.

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Low-Energy Diffuse X-Rays

Cited by 36 publications

References 0 publications

Possible origin of the slow-diffusion region around Geminga

Possible origin of the slow-diffusion region around Geminga

X-ray background measurements with XMM-Newton EPIC

The Soft X-Ray Background

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