X-ray emission from wind blown interstellar bubbles

Wrigge, M.; Wendker, H. J.

doi:10.1051/0004-6361:20020804

Cited by 30 publications

(52 citation statements)

References 17 publications

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“…There is only one more object, S308, that has been detected and studied in some detail. Analysis of the ROSAT (Wrigge et al 1994) and the XMMNewton (Chu et al 2003) observations of S308 showed that its X-ray spectrum is soft with plasma temperature of kT = 0.15 keV. Recent analysis of new XMM-Newton observations that completed coverage of this WBB observed in X-rays to 90% of its spatial extent confirmed the basic properties of the hot plasma in S308 (Toala et al 2012).…”

Section: Introductionmentioning

confidence: 87%

X-rays from wind-blown bubbles: an XMM–Newton detection of NGC 2359

Zhekov

2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the XMM-Newton observation of the wind-blown bubble NGC 2359. This is the first detection of this object in X-rays. The X-ray emission of NGC 2359 is soft and originates from a thermal plasma with a typical temperature of kT ∼ 0.2 keV. A direct comparison between the one-dimensional hydrodynamic model of wind-blown bubbles and the X-ray spectrum of NGC 2359 suggests a reduced massloss rate of the central star in order to provide the correct value of the observed flux. The central star of the nebula, WR 7, is an X-ray source. Its emission is similar to that of other presumably single Wolf-Rayet stars detected in X-rays. The WR 7 spectrum is well represented by the emission from a two-temperature plasma with a cool component of kT ∼ 0.6 keV and a hot component of kT ∼ 2.7 keV.

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Section: Introductionmentioning

confidence: 87%

X-rays from wind-blown bubbles: an XMM–Newton detection of NGC 2359

Zhekov

2014

Monthly Notices of the Royal Astronomical Society

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“…NGC 6888 was the first WBB that has been detected in X-rays, it was made with Einstein by Bochkarev (1988). The Wrigge et al (1994) X-ray observation did not detect a filled bubble emitting as models predicted, but a filamentary X-ray structure was instead found following the Hα features of the nebula. In addition, spectra in the shell were fit to a double-temperature plasma model with a high-temperature component at T ∼ 8.5 × 10 6 K and a low-temperature component at T ∼ 1.3 × 10 6 K without detecting significant temperature variation between different areas of the nebula (Wrigge et al 2005).…”

Section: Introductionmentioning

confidence: 94%

Ionization structure and chemical abundances of the Wolf-Rayet nebula NGC 6888 with integral field spectroscopy

Fernández-Martín¹,

Martín-Gordón²,

Vı́lchez³

et al. 2012

A&A

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Context. The study of nebulae around Wolf-Rayet (WR) stars gives us clues about the mass-loss history of massive stars, as well as about the chemical enrichment of the interstellar medium (ISM). Aims. This work aims to search for the observational footprints of the interactions between the ISM and stellar winds in the WR nebula NGC 6888 in order to understand its ionization structure, chemical composition, and kinematics. Methods. We have collected a set of integral field spectroscopy observations across NGC 6888, obtained with PPAK in the optical range performing both 2D and 1D analyses. Attending to the 2D analysis in the northeast part of NGC 6888, we have generated maps of the extinction structure and electron density. We produced statistical frequency distributions of the radial velocity and diagnostic diagrams. Furthermore, we performed a thorough study of integrated spectra in nine regions over the whole nebula. Results. The 2D study has revealed two main behaviours. We have found that the spectra of a localized region to the southwest of this pointing can be represented well by shock models assuming n = 1000 cm −3 , twice solar abundances, and shock velocities from 250 to 400 km s −1 . With the 1D analysis we derived electron densities ranging from <100 to 360 cm −3 . The electron temperature varies from ∼7700 K to ∼10 200 K. A strong variation of up to a factor 10 between different regions in the nitrogen abundance has been found: N/H appears lower than the solar abundance in those positions observed at the edges and very enhanced in the observed inner parts. Oxygen appears slightly underabundant with respect to solar value, whereas the helium abundance is found to be above it. We propose a scenario for the evolution of NGC 6888 to explain the features observed. This scheme consists of a structure of multiple shells: i) an inner and broken shell with material from the interaction between the supergiant and WR shells, presenting an overabundance in N/H and a slight underabundance in O/H; ii) an outer shell very intense in [OIII]λ5007 Å corresponding to the main sequence bubble broken up as a consequence of the collision between supergiant and WR shells. Nitrogen and oxygen do not appear enhanced here, but helium appears enriched; iii) and finally it includes an external and faint shell that surrounds the whole nebula like a thin skin representing the early interaction between the winds from the main sequence star with the ISM for which typical circumstellar abundances are derived.

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“…NGC 6888 around WR 136 (WN6) is often regarded as the archetypal WR bubble. It was first detected in the X-ray domain by the EINSTEIN satellite, but was more thoroughly studied using ROSAT data (Wrigge et al 1994, and references therein). The X-ray emission from NGC 6888 appears to be limb-brightened and is concentrated to the northeast and southwest parts of the nebula, where Hα appears the strongest.…”

Section: The Surrounding Nebula Rcw 58mentioning

confidence: 99%

AnXMM-Newtonlook at the Wolf-Rayet star WR 40

Gosset¹,

Nazé²,

Claeskens³

et al. 2004

A&A

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Abstract. We present the results of an XMM-Newton observation of the field of the Wolf-Rayet star WR 40. Despite a nominal exposure of 20 ks and the high sensitivity of the satellite, the star itself is not detected: we thus derive an upper limit on its X-ray flux and luminosity. Joining this result to recent reports of a non-detection of some WC stars, we suggest that the X-ray emission from single normal Wolf-Rayet stars could often be insignificant despite remarkable instabilities in the wind. On the basis of a simple modelling of the opacity of the Wolf-Rayet wind of WR 40, we show that any X-ray emission generated in the particular zone where the shocks are supposed to be numerous will indeed have little chance to emerge from the dense wind of the Wolf-Rayet star. We also report the non-detection of the ejecta nebula RCW 58 surrounding WR 40. Concerning the field around these objects, we detected 33 X-ray sources, most of them previously unknown: we establish a catalog of these sources and cross-correlate it with catalogs of optical/infrared sources.

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X-ray emission from wind blown interstellar bubbles

Cited by 30 publications

References 17 publications

X-rays from wind-blown bubbles: an XMM–Newton detection of NGC 2359

X-rays from wind-blown bubbles: an XMM–Newton detection of NGC 2359

Ionization structure and chemical abundances of the Wolf-Rayet nebula NGC 6888 with integral field spectroscopy

AnXMM-Newtonlook at the Wolf-Rayet star WR 40

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