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

Ruiz, N.; Guerrero, M. A.; Chu, You‐Hua; Gruendl, R. A.

doi:10.1088/0004-6256/142/3/91

Cited by 19 publications

(20 citation statements)

References 39 publications

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“…The same model can give a limb-brightened or flat surface brightness profile depending on the FWHM of the Gaussian profile of the PSF. Indeed, observations of the same object with XMM-Newton and Chandra can give different radial surface brightness profiles, such as is the case with NGC 3242 (see Ruiz et al 2011,Kastner et al 2012. This is because the PSF of the EPIC XMM-Newton X-ray detectors is not able to resolve structures with the same level of detail as the back-illuminated ACIS-S CCD3 of the Chandra telescope.…”

Section: Discussionmentioning

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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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: Discussionmentioning

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 in this context, it may be worth pointing out that the presence of a system of concentric rings, whose brightness is higher in the mid-IR than in the optical, located in an extended halo around the source, has been recently reported by Phillips et al (2009). Furthermore, from the analysis of its HST images, Ruiz et al (2011) modelled its Hα brightness spatial distribution as a thin shell with a constant density embedded within an outer shell, characterized by a radial density profile much shallower than the classical profile for a free-expanding wind at a constant massloss rate (r −2 ). This is in agreement with our dust modelling for NGC 3242, whose density profile is less steep than that of the other PNe.…”

Section: Physical Properties Of the Source Samplementioning

confidence: 84%

Planckintermediate results. XVIII. The millimetre and sub-millimetre emission from planetary nebulae

Arnaud¹,

Atrio-Barandela²,

Aumont³

et al. 2014

A&A

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Late stages of stellar evolution are characterized by copious mass-loss events whose signature is the formation of circumstellar envelopes (CSE). Planck multi-frequency measurements have provided relevant information on a sample of Galactic planetary nebulae (PNe) in the important and relatively unexplored observational band between 30 and 857 GHz. Planck enables the assembly of comprehensive PNe spectral energy distributions (SEDs) from radio to far-IR frequencies. Modelling the derived SEDs provides us with information on physical properties of CSEs and the mass content of both main components: ionized gas, traced by the free-free emission at cm-mm waves; and thermal dust, traced by the millimetre and far-IR emission. In particular, the amount of ionized gas and dust has been derived here. Such quantities have also been estimated for the very young PN CRL 618, where the strong variability observed in its radio and millimetre emission has previously prevented constructing its SED. A morphological study of the Helix Nebula was also performed. Planck maps reveal, for the first time, the spatial distribution of the dust inside the envelope, allowing us to identify different components, the most interesting of which is a very extended component (up to 1 pc) that may be related to a region where the slow expanding envelope is interacting with the surrounding interstellar medium.

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“…In an XMM observation ( Figure 4, upper left), NGC 3242 (the Ghost of Jupiter nebula) is well detected and appears as a marginally extended, asymmetric X-ray source (Ruiz et al 2011). However, as in the cases of NGC 2392 (Guerrero et al 2005) and 7009 (Guerrero et al 2002), the diameter of the inner nebula of NGC 3242 is similar to the width of the XMM/EPIC (pn and MOS) point spread functions, rendering its XMM X-ray morphology difficult to interpret and (in particular) the potential contribution from an X-ray-luminous CSPN impossible to ascertain.…”

Section: Bd+30mentioning

confidence: 99%

THECHANDRAX-RAY SURVEY OF PLANETARY NEBULAE (CHANPLANS): PROBING BINARITY, MAGNETIC FIELDS, AND WIND COLLISIONS

Kastner

Montez

Balick

et al. 2012

The Astronomical Journal

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We present an overview of the initial results from the Chandra Planetary Nebula Survey (ChanPlaNS), the first systematic (volume-limited) Chandra X-Ray Observatory survey of planetary nebulae (PNe) in the solar neighborhood. The first phase of ChanPlaNS targeted 21 mostly high-excitation PNe within ∼1.5 kpc of Earth, yielding four detections of diffuse X-ray emission and nine detections of X-ray-luminous point sources at the central stars (CSPNe) of these objects. Combining these results with those obtained from Chandra archival data for all (14) other PNe within ∼1.5 kpc that have been observed to date, we find an overall X-ray detection rate of ∼70% for the 35 sample objects. Roughly 50% of the PNe observed by Chandra harbor X-ray-luminous CSPNe, while soft, diffuse X-ray emission tracing shocks-in most cases, "hot bubbles"-formed by energetic wind collisions is detected in ∼30%; five objects display both diffuse and point-like emission components. The presence (or absence) of X-ray sources appears correlated with PN density structure, in that molecule-poor, elliptical nebulae are more likely to display X-ray emission (either point-like or diffuse) than molecule-rich, bipolar, or Ring-like nebulae. All but one of the point-like CSPNe X-ray sources display X-ray spectra that are harder than expected from hot (∼100 kK) central stars emitting as simple blackbodies; the lone apparent exception is the central star of the Dumbbell nebula, NGC 6853. These hard X-ray excesses may suggest a high frequency of binary companions to CSPNe. Other potential explanations include self-shocking winds or PN mass fallback. Most PNe detected as diffuse X-ray sources are elliptical nebulae that display a nested shell/halo structure and bright ansae; the diffuse X-ray emission regions are confined within inner, sharp-rimmed shells. All sample PNe that display diffuse X-ray emission have inner shell dynamical ages 5 × 10 3 yr, placing firm constraints on the timescale for strong shocks due to wind interactions in PNe. The high-energy emission arising in such wind shocks may contribute to the high excitation states of certain archetypical "hot bubble" nebulae (e.g., NGC 2392, 3242, 6826, and 7009).

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

Cited by 19 publications

References 39 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

Planckintermediate results. XVIII. The millimetre and sub-millimetre emission from planetary nebulae

THECHANDRAX-RAY SURVEY OF PLANETARY NEBULAE (CHANPLANS): PROBING BINARITY, MAGNETIC FIELDS, AND WIND COLLISIONS

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