A Carbon-rich Hot Bubble in the Planetary Nebula NGC 5189

Toalá, J. A.; Montez, Rodolfo; Karovska, M.

doi:10.3847/1538-4357/ab498e

Cited by 7 publications

(7 citation statements)

References 48 publications

(52 reference statements)

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“…Predictions for the extended WRPNe NGC 5189 and NGC 6905 (not shown here) are also consistent with the presence of mixing layers. In particular, NGC 5189 is the most extended PNe with a hot bubble that seems to have been powered by a born-again event, which produced the C overabundance of the X-ray-emitting material (Toalá et al 2019a).…”

Section: Mixing Layer In Other Wrpnementioning

confidence: 99%

“…Most of the hot bubbles detected through X-ray observations correspond to PNe harbouring H-deficient CSPN, in particular those classified as [Wolf-Rayet] ([WR]) type (Kastner et al 2012;Freeman et al 2014;Toalá et al 2019a). Although the reason is not completely clear, one might suggest that is the result of the powerful winds from [WR]-type CSPNe interacting with the slow AGB material producing higher degree of turbulent structures (Gesicki et al 2006;Medina et al 2006).…”

Section: Introductionmentioning

confidence: 99%

“…References: (1)Kaler (1976), (2)Feibelman (1999), (3) García-Rojas et al (2012), (4)Toalá et al (2019a), (5)Feibelman (1997), (6)Keller, Bianchi, & Maciel (…”

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confidence: 99%

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Planetary nebulae with Wolf-Rayet-type central stars -- IV. NGC 1501 and its mixing layer

Rubio¹,

Toalá²,

Todt³

et al. 2022

Preprint

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Theory predicts that the temperature of the X-ray-emitting gas (∼10 6 K) detected from planetary nebulae (PNe) is a consequence of mixing or thermal conduction when in contact with the ionized outer rim (∼10 4 K). Gas at intermediate temperatures (∼10 5 K) can be used to study the physics of the production of X-ray-emitting gas, via C , N and O ions. Here we model the stellar atmosphere of the CSPN of NGC 1501 to demonstrate that even this hot H-deficient [WO4]-type star cannot produce these emission lines by photoionization. We use the detection of the C lines to assess the physical properties of the mixing region in this PNe in comparison with its X-ray-emitting gas, rendering NGC 1501 only the second PNe with such characterization. We extend our predictions to the hottest [WO1] and cooler [WC5] spectral types and demonstrate that most energetic photons are absorbed in the dense winds of [WR] CSPN and highly ionized species can be used to study the physics behind the production of hot bubbles in PNe. We found that the UV observations of NGC 2452, NGC 6751 and NGC 6905 are consistent with the presence mixing layers and hot bubbles, providing excellent candidates for future X-ray observations.

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Section: Mixing Layer In Other Wrpnementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Planetary nebulae with Wolf-Rayet-type central stars -- IV. NGC 1501 and its mixing layer

Rubio¹,

Toalá²,

Todt³

et al. 2022

Preprint

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show abstract

“…Only one more PN has been found to exhibit diffuse X-ray emission since the WORKPLANS I. This is the case of NGC 5189, a PN around a [WO1] CSPN whose extended X-ray emission has been discovered by XMM-Newton [23]. The spatial distribution and spectral properties of the X-ray emission, particularly its high carbon abundances, are consistent with a born-again scenario where a CSPN becomes carbon-rich through a very late thermal pulse (VLTP) event and then develops a fast, carbon-rich wind that generates X-ray emission.…”

Section: New Discoveries Of X-ray Pnementioning

confidence: 99%

X-ray Observations of Planetary Nebulae since WORKPLANS I and Beyond

Guerrero

2020

Galaxies

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Planetary nebulae (PNe) were expected to be filled with hot pressurized gas driving their expansion. ROSAT hinted at the presence of diffuse X-ray emission from these hot bubbles and detected the first sources of hard X-ray emission from their central stars, but it was not until the advent of Chandra and XMM-Newton that we became able to study in detail their occurrence and physical properties. Here I review the progress in the X-ray observations of PNe since the first WORKshop for PLAnetary Nebulae observationS (WORKPLANS) and present the perspective for future X-ray missions with particular emphasis on eROSITA.

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“…Most of the hot bubbles detected through X-ray observations correspond to PNe harbouring H-deficient CSPN, in particular those classified as (Wolf-Rayet [WR]) type (Kastner et al 2012 ;Freeman et al 2014 ;Toal á, Montez & Karovska 2019a ). Although the reason is not completely clear, one might suggest that is the result of the powerful winds from [WR]-type CSPNe interacting with the slow AGB material producing higher degree of turbulent structures (Gesicki et al 2006 ;Medina et al 2006 ).…”

Section: Introductionmentioning

confidence: 99%

Planetary nebulae with Wolf–Rayet-type central stars – IV. NGC 1501 and its mixing layer

Rubio

Toalá²,

Todt

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Theory predicts that the temperature of the X-ray-emitting gas (∼106 K) detected from planetary nebulae (PNe) is a consequence of mixing or thermal conduction when in contact with the ionized outer rim (∼104 K). Gas at intermediate temperatures (∼105 K) can be used to study the physics of the production of X-ray-emitting gas, via C iv, N v and O vi ions. Here we model the stellar atmosphere of the CSPN of NGC 1501 to demonstrate that even this hot H-deficient [WO4]-type star cannot produce these emission lines by photoionization. We use the detection of the C iv lines to assess the physical properties of the mixing region in this PNe in comparison with its X-ray-emitting gas, rendering NGC 1501 only the second PNe with such characterization. We extend our predictions to the hottest [WO1] and cooler [WC5] spectral types and demonstrate that most energetic photons are absorbed in the dense winds of [WR] CSPN and highly ionized species can be used to study the physics behind the production of hot bubbles in PNe. We found that the UV observations of NGC 2452, NGC 6751 and NGC 6905 are consistent with the presence mixing layers and hot bubbles, providing excellent candidates for future X-ray observations.

show abstract

A Carbon-rich Hot Bubble in the Planetary Nebula NGC 5189

Cited by 7 publications

References 48 publications

Planetary nebulae with Wolf-Rayet-type central stars -- IV. NGC 1501 and its mixing layer

Planetary nebulae with Wolf-Rayet-type central stars -- IV. NGC 1501 and its mixing layer

X-ray Observations of Planetary Nebulae since WORKPLANS I and Beyond

Planetary nebulae with Wolf–Rayet-type central stars – IV. NGC 1501 and its mixing layer

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