[ITAL]Chandra[/ITAL] Reveals the X-Ray Glint in the Cat’s Eye

Chu, You‐Hua; Guerrero, M. A.; Gruendl, R. A.; Williams, R. M.; Kaler, J. B.

doi:10.1086/320495

Cited by 110 publications

(166 citation statements)

References 17 publications

(17 reference statements)

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“…18 shows similar spectral features to Chandra observations reported by Chu et al (2001), Gruendl et al (2006), and Ruiz et al (2013) for the PNe NGC 6543, NGC 7026 and NGC 2392, although differences in the binning make a direct comparison difficult. In this paper, a single set of abundances has been used for both fast stellar wind and nebular components but it should be appreciated that if different abundance sets are used for the two components, then this would also have an effect on the evolution of the spectral shape.…”

Section: Correction For Absorption and Convolution With Instrumental supporting

confidence: 71%

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Formation and X-ray emission from hot bubbles in planetary nebulae – II. Hot bubble X-ray emission

Toalá¹,

Arthur²

2016

Mon. Not. R. Astron. Soc.

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We present a study of the X-ray emission from numerical simulations of hot bubbles in planetary nebulae (PNe). High-resolution, two-dimensional, radiation-hydrodynamical simulations of the formation and evolution of hot bubbles in PNe, with and without thermal conduction, are used to calculate the X-ray emission and study its timedependence and relationship to the changing stellar parameters. Instabilities in the wind-wind interaction zone produce clumps and filaments in the swept-up shell of nebular material. Turbulent mixing and thermal conduction at the corrugated interface can produce quantities of intermediate temperature and density gas between the hot, shocked wind bubble and the swept-up photoionized nebular material, which can emit in soft, diffuse X-rays. We use the chianti software to compute synthetic spectra for the models and calculate their luminosities. We find that models both with conduction and those without can produce the X-ray temperatures and luminosities that are in the ranges reported in observations, although the models including thermal conduction are an order of magnitude more luminous than those without. Our results show that at early times the diffuse X-ray emission should be dominated by the contribution from the hot, shocked stellar wind, whereas at later times the nebular gas will dominate the spectrum. We analyse the effect of sampling on the resultant spectra and conclude that a minimum of 200 counts is required to reliably reproduce the spectral shape. Likewise, heavily smoothed surface-brightness profiles obtained from low-count detections of PNe do not provide a reliable description of the spatial distribution of the X-ray emitting gas.

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Section: Correction For Absorption and Convolution With Instrumental supporting

confidence: 71%

“…Since the spectra of PNe are generally quite soft, extinction plays an important rôle in the shape of the spectrum at lower energies. Even so, there are some PNe for which an important count rate has been measured at low energies (e.g., NGC 6543 and BD +30 • 3639; Kastner et al 2000;Chu et al 2001;Yu et al 2009). …”

Section: Absorptionmentioning

confidence: 99%

Formation and X-ray emission from hot bubbles in planetary nebulae – II. Hot bubble X-ray emission

Toalá¹,

Arthur²

2016

Mon. Not. R. Astron. Soc.

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“…However, the image alignment in Figure 2, while suggestive, is not unique and cannot be used to conclude that the central star is an Xray source. Such emission, if present, is not nearly so prominent as in the case of the central star of NGC 6543 (Chu et al 2001). …”

Section: Observations and Data Reductionmentioning

confidence: 91%

Discovery of Extended X-Ray Emission from the Planetary Nebula NGC 7027 by the [ITAL]Chandra X-Ray Observatory[/ITAL]

Kastner

Vrtilek

Soker

2001

The Astrophysical Journal

116

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We report the discovery of X-ray emission from NGC 7027, a prototypical object for the study of the formation and evolution of planetary nebulae. Observations with the Advanced CCD Imaging Spectrometer (ACIS) aboard the Chandra X-Ray Observatory show that the X-ray emission from NGC 7027 is extended and is bipolar in morphology. The ACIS spectrum displays strong emission from highly ionized Ne and weaker emission features, which we attribute to O, Mg, and Si. Model fits to this spectrum suggest a characteristic temperature T ∼ 3 # X K and an intrinsic (unabsorbed) X-ray luminosity of ergs s Ϫ1 . The intranebular absorption of 6 32 10 L ∼ 1.3 # 10 X X-ray emission is highly nonuniform, but the modeling indicates an average column density cm Ϫ2 , 21 N ∼ 6 # 10 H consistent with previous measurements of relatively large visual extinction within the nebula. We suggest that the X-ray emission from NGC 7027 is or was generated by a hitherto undetected fast wind from the central star of NGC 7027 or from a companion to this star. Chandra's detection of extended, high-temperature X-ray emission from BD ϩ30Њ3639, NGC 6543, and now NGC 7027 suggests that such emission is a common feature of young planetary nebulae.

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“…The great advantage of clusters is that the ICM are transparent to both X-ray, where the ambient gas is seen, and to radio that reveals the interior of the bubbles in many cases. In PNe the ambient region is always seen in visible, but only in rare cases do we see the inner region of bubbles because of the weak X-ray emission, e.g., in the PN NGC 6543 (the Cat's Eye Nebula, Chu et al 2001). X-ray have been found in the PN Hb 5 that is presented in Figure 2 (Montez et al 2009;Freeman et al 2014), and in a handful of other PNe (Freeman et al 2014).…”

Section: Jet-inflated Bubblesmentioning

confidence: 97%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

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[ITAL]Chandra[/ITAL] Reveals the X-Ray Glint in the Cat’s Eye

Cited by 110 publications

References 17 publications

Formation and X-ray emission from hot bubbles in planetary nebulae – II. Hot bubble X-ray emission

Formation and X-ray emission from hot bubbles in planetary nebulae – II. Hot bubble X-ray emission

Discovery of Extended X-Ray Emission from the Planetary Nebula NGC 7027 by the [ITAL]Chandra X-Ray Observatory[/ITAL]

The jet feedback mechanism (JFM) in stars, galaxies and clusters

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