THE X-RAY SPECTRUM OF A PLANETARY NEBULA AT HIGH RESOLUTION:<i>CHANDRA</i>GRATINGS SPECTROSCOPY OF BD +30°3639

Yu, Young Sam; Nordon, R.; Kastner, Joel H.; Houck, J. C.; Behar, E.; Soker, Noam

doi:10.1088/0004-637x/690/1/440

Cited by 32 publications

(106 citation statements)

References 39 publications

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“…The low plasma temperature, however, needs large amounts of material from the cold nebular shell to have been incorporated into the hot bubble. This problem, similar to that found in other PNe such as BD+30 • 3639 (Yu et al 2009), NGC 2392 (Guerrero et al 2005), and NGC 6543 , may require mechanisms for the production of X-ray emission in PNe other than mixing and heat conduction as summarized by Soker et al (2010).…”

Section: Discussionsupporting

confidence: 62%

Physical Structure of the Planetary Nebula NGC 3242 From the Hot Bubble to the Nebular Envelope

Ruiz¹,

Guerrero²,

Chu³

et al. 2011

The Astronomical Journal

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One key feature of the interacting stellar winds model of the formation of planetary nebulae (PNe) is the presence of shock-heated stellar wind confined in the central cavities of PNe. This so-called hot bubble should be detectable in X-rays. Here we present XMM-Newton observations of NGC 3242, a multiple-shell PN whose shell morphology is consistent with the interacting stellar winds model. Diffuse X-ray emission is detected within its inner shell with a plasma temperature ∼2.35×10 6 K and an intrinsic X-ray luminosity ∼2×10 30 ergs s −1 at the adopted distance of 0.55 kpc. The observed X-ray temperature and luminosity are in agreement with "ad-hoc" predictions of models including heat conduction. However, the chemical abundances of the X-ray-emitting plasma seem to imply little evaporation of cold material into the hot bubble, whereas the thermal pressure of the hot gas is unlikely to drive the nebular expansion as it is lower than that of the inner shell rim. These inconsistencies are compounded by the apparent large filling factor of the hot gas within the central cavity of NGC 3242.

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Section: Discussionsupporting

confidence: 62%

Physical Structure of the Planetary Nebula NGC 3242 From the Hot Bubble to the Nebular Envelope

Ruiz¹,

Guerrero²,

Chu³

et al. 2011

The Astronomical Journal

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“…Even though it is a short-lived phase, and even shorter in the most massive cases, there is one observed object, BD+30 • 3639, that requires stellar abundances, since C and Ne are enhanced. Yu et al (2009) analyzed Chandra Low Energy Transmission Gratings (LETG) spectra in conjunction with the ACIS-S data. The high-quality LETG/ACIS-S spectra enabled the authors to conclude unambiguously that the diffuse X-ray emission in this PN has abundances close to those of the CSPN.…”

Section: Discussionmentioning

confidence: 99%

“…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%

“…Detailed spectral analysis of some of the detected objects indicates that the temperature of the X-ray-emitting gas lies in the narrow range (1-3) × 10 6 K with electronic densities of the order of 1-10 2 cm −3 (e.g., Ruiz et al 2013; Kastner et al 2012, and references therein). Some of the objects detected in diffuse emission can be described using the abundances of that of c 0000 RAS the nebular material, while others require stellar abundances (e.g., Yu et al 2009). …”

Section: Introductionmentioning

confidence: 99%

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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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“…Although the carbon abundance and plasma emission measure (EM) parameter values deduced from our spectral fitting of the K 1-16 X-ray source are degenerate (Section 2.3.2), some constraints on plasma density can be obtained from considerations of the likely emission region location and geometry, given a carbon abundance that lies somewhere between the C/O ratio of the photosphere (C/O ∼ 3; Werner & Herwig 2006) and that characteristic of the "hot bubble" plasma within the [WC] CSPN BD+303639 (C/O in the range 15-45; Yu et al 2009). The X-ray spectral fitting then suggests log EM [cm −3 ] in the range 53-54.…”

Section: Origin Of the Mk Plasmamentioning

confidence: 99%

Serendipitous Detection of X-Ray Emission From the Hot Born-Again Central Star of the Planetary Nebula K 1-16

Montez

Kastner

2013

ApJ

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We report the serendipitous detection of point-like X-ray emission from the hot, PG1159-type central star of the planetary nebula (CSPN) K 1-16 by the XMM-Newton and Chandra X-Ray Observatories. The CSPN lies superimposed on a galaxy cluster that includes an X-ray-bright quasar, but we have successfully isolated the CSPN X-ray emission from the strong diffuse background contributed by the quasar and intracluster gas. We have modeled the XMM-Newton and Chandra X-ray data, taking advantage of the contrasting detection efficiencies of the two observatories to better constrain the low-energy spectral response of Chandra's Advanced CCD Imaging Spectrometer. We find that the CSPN X-ray spectrum is well characterized by the combination of a non-local thermodynamic equilibrium model atmosphere with T ∼ 135 kK and a carbon-rich, optically thin thermal plasma with T X ∼ 1 MK. These results for X-ray emission from the K 1-16 CSPN, combined with those obtained for other PG1159-type objects, lend support to the "born-again" scenario for Wolf-Rayet and PG1159 CSPNe, wherein a late helium shell flash dredges up carbon-rich intershell material and ejects this material into the circumstellar environment.

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THE X-RAY SPECTRUM OF A PLANETARY NEBULA AT HIGH RESOLUTION:CHANDRAGRATINGS SPECTROSCOPY OF BD +30°3639

Cited by 32 publications

References 39 publications

Physical Structure of the Planetary Nebula NGC 3242 From the Hot Bubble to the Nebular Envelope

Physical Structure of the Planetary Nebula NGC 3242 From the Hot Bubble to the Nebular Envelope

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

Serendipitous Detection of X-Ray Emission From the Hot Born-Again Central Star of the Planetary Nebula K 1-16

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