High-resolution X-ray Spectroscopy of BD +30°3639

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

doi:10.1017/s1743921306002936

Cited by 4 publications

(3 citation statements)

References 13 publications

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“…Furthermore, our robust determination of a Ne overabundance of ∼ 3 to ∼ 6 relative to solar is consistent with the predictions of models describing H-deficient central stars of PNe (Werner & Herwig 2006). Hence, as also pointed out by Murashima et al (2006) and Kastner et al (2006), the nonsolar composition of the X-ray-emitting plasma in BD+30 • 3639 appears to be the direct result of nucleosynthesis processes in the precursor AGB star (e.g., Herwig 2005 and references therein).…”

Section: Plasma Abundances: Constraints On the Origin Of The X-ray-em...supporting

confidence: 87%

“…We selected LETG/ACIS-S (as opposed to HETG/ACIS-S or LETG/HRC-S) for Chandra gratings observations of BD+30 • 3639 on the basis of the superior background rejection, soft X-ray sensitivity, and order-sorting capabilities of this configuration. In addition to the dispersed spectrum of BD+30 • 3639 (for which preliminary results were presented in Kastner et al 2006), the LETG/ACIS-S observations produced a highly sensitive, undispersed 0th-order image of the PN. In this paper, we present a comprehensive analysis of the dispersed LETG/ACIS-S spectrum of BD+30 • 3639.…”

Section: Introductionmentioning

confidence: 97%

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

Nordon

Kastner

et al. 2008

ApJ

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We present the results of the first X-ray gratings spectroscopy observations of a planetary nebula (PN), the X-ray-bright, young BD+30 • 3639. We observed BD+30 • 3639 for a total of 300 ks with the Chandra X-ray Observatory's Low Energy Transmission Gratings in combination with its Advanced CCD Imaging Spectrometer (LETG/ACIS-S). The LETG/ACIS-S spectrum of BD+30 • 3639 is dominated by H-like resonance lines of O viii and C vi and the He-like triplet line complexes of Ne ix and O vii. Other H-like resonance lines, such as N vii, as well as lines of highly ionized Fe, are weak or absent. Continuum emission is evident over the range 6-18Å. Spectral modeling indicates the presence of a range of plasma temperatures from T x ∼ 1.7 × 10 6 K to 2.9 × 10 6 K and an intervening absorbing column N H ∼ 2.4 × 10 21 cm −2 . The same modeling conclusively demonstrates that C and Ne are highly enhanced, with abundance ratios of C/O ∼15-45 and Ne/O ∼3.3-5.0 (90% confidence ranges, relative to the solar ratios), while N and Fe are depleted, N/O ∼0.0-1.0 and Fe/O ∼0.1-0.4. The intrinsic luminosity of the X-ray source determined from the modeling and the measured flux (F X = 4.1 × 10 −13 ergs cm −2 s −1 ) is L X ∼ 8.6 × 10 32 erg s −1 (assuming D = 1.2 kpc).These gratings spectroscopy results are generally consistent with earlier results obtained from X-ray CCD imaging spectroscopy of BD+30 • 3639, but are

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Section: Plasma Abundances: Constraints On the Origin Of The X-ray-em...supporting

confidence: 87%

Section: Introductionmentioning

confidence: 97%

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

Nordon

Kastner

et al. 2008

ApJ

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“…Unfortunately, these lines were not detected, which set an upper limit on the iron composition of the X-ray emitting gas, a limit far below the solar metallicity. This result was confirmed by Kastner et al (2006), who did not detect iron lines in their high-resolution X-ray spectrum of BD +30 36939. The peculiar chemical composition of the X-ray-emitting gas leads to a possible trace of its origin.…”

Section: Introductionmentioning

confidence: 59%

Non–Local Thermodynamic Equilibrium Model of NGC 6543’s Central Star and Its Relation to the Surrounding Planetary Nebula

Георгиев

Peimbert

Hillier

et al. 2008

ApJ

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We analyze the chemical composition of the central star of the planetary nebula NGC 6543 based on a detailed NLTE model of its stellar wind. The logarithmic abundances by number are H ¼ 12:00, He ¼ 11:00, C ¼ 9:03, N ¼ 8:36, O ¼ 9:02, Si ¼ 8:19, P ¼ 5:53, S ¼ 7:57, and Fe ¼ 7:24. Compared with the solar abundances, most of the elements have solar composition with respect to hydrogen, except C, which is overabundant by 0.28 dex, and Fe, which is depleted by $0.2 dex. Contrary to most previous work, we find that the star is not H-poor and has a normal He composition. These abundances are compared with those found in the diffuse X-ray plasma and the nebular gas. Compared to the plasma emitting in diffuse X-rays, the stellar wind is much less depleted in iron. Since the iron depletions in the nebular gas and X-ray plasma are similar, we conclude that the plasma emitting diffuse X-rays is derived from the nebular gas rather than the stellar wind. Excellent agreement is obtained between the abundances in the stellar wind and the nebular recombination line abundances for He, C, and O relative to H. On the other hand, the derived stellar N abundance is smaller than the nebular N abundance derived from recombination lines and agrees with the abundance found from collisionally excited lines. The mean temperature variation determined by five different methods indicates that the difference in the nebular abundances between the recombination lines and collisionally excited lines can be explained as due to the temperature variations in a chemically homogeneous medium. Subject headingg s: planetary nebulae: individual ( NGC 6543)

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SerendipitousChandraX-Ray Detection of a Hot Bubble within the Planetary Nebula NGC 5315

Kastner

Montez

Balick

et al. 2008

ApJ

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157

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We report the serendipitous detection of the planetary nebula NGC 5315 by the Chandra X-ray Observatory. The Chandra imaging spectroscopy results indicate that the X-rays from this PN, which harbors a Wolf-Rayet (WR) central star, emanate from a T X ∼ 2.5 × 10 6 K plasma generated via the same windwind collisions that have cleared a compact (∼ 8000 AU radius) central cavity within the nebula. The inferred X-ray luminosity of NGC 5315 is ∼ 2.5 × 10 32 erg s −1 (0.3-2.0 keV), placing this object among the most luminous such "hot bubble" X-ray sources yet detected within PNe. With the X-ray detection of NGC 5315, objects with WR-type central stars now constitute a clear majority -2of known examples of diffuse X-ray sources among PNe; all such "hot bubble" PN X-ray sources display well-defined, quasi-continuous optical rims. We therefore assert that X-ray-luminous hot bubbles are characteristic of young PNe with large central star wind kinetic energies and closed bubble morphologies. However, the evidence at hand also suggests that processes such as wind and bubble temporal evolution, as well as heat conduction and/or mixing of hot bubble and nebular gas, ultimately govern the luminosity and temperature of superheated plasma within PNe.

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High-resolution X-ray Spectroscopy of BD +30°3639

Cited by 4 publications

References 13 publications

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

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

Non–Local Thermodynamic Equilibrium Model of NGC 6543’s Central Star and Its Relation to the Surrounding Planetary Nebula

SerendipitousChandraX-Ray Detection of a Hot Bubble within the Planetary Nebula NGC 5315

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