Winds in central stars of planetary nebulae

Cerruti-Sola, M.; Perinotto, M.

doi:10.1086/163062

Cited by 98 publications

(66 citation statements)

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“…that a similar mechanism, i.e., self-shocking winds, might be producing the point-like X-ray emission from many, perhaps most, CSPNe. This is further supported by the fact that during the high-luminosity phase of post-AGB evolution, where a majority of our detections are made, stellar winds are strongest and subsequently fade after the temperature of the central star has peaked (Cerruti-Sola & Perinotto 1985). Further evidence for self-shocking winds comes from UV spectroscopy where CSPNe with variable P Cygni profiles are observed with high ionization potential ions (e.g., O vi) despite low effective temperatures, which is interpreted as Auger ionization from X-ray emission due to shocks in their stellar winds (Guerrero & De Marco 2013).…”

Section: Tracing the Origin Of X-ray Emitting Cspnesupporting

confidence: 70%

“…Source of supplementary CSPNe properties and adopted X-ray spectral model are discussed in Section 3. a Binary notation scheme: "c"-close binary, "w"-wide binary, "y"-binary with unknown period, "o"-an optical pair; additionally, we indicate suspected binarity by placing the binary indicator within parentheses. b Stellar wind notation is from Cerruti-Sola & Perinotto (1985): "y"-P Cygni profiles were detected, "n"-no P Cygni profiles were detected and the stellar photosphere is detected, ":"-the observation is not sensitive to the photosphere, "-"-no UV satellite observations are present. c Adopted model: 1-N H determined from c Hβ (fixed-N H model); 2-N H determined from spectral fit (free-N H model).…”

Section: Hot Pg1159-type Cspnementioning

confidence: 99%

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THE CHANDRA PLANETARY NEBULA SURVEY (ChanPlaNS). III. X-RAY EMISSION FROM THE CENTRAL STARS OF PLANETARY NEBULAE

Montez

Kastner

Balick

et al. 2015

ApJ

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We present X-ray spectral analysis of 20 point-like X-ray sources detected in Chandra Planetary Nebula Survey observations of 59 planetary nebulae (PNe) in the solar neighborhood. Most of these 20 detections are associated with luminous central stars within relatively young, compact nebulae. The vast majority of these point-like X-rayemitting sources at PN cores display relatively "hard" ( 0.5 keV) X-ray emission components that are unlikely to be due to photospheric emission from the hot central stars (CSPN). Instead, we demonstrate that these sources are well modeled by optically thin thermal plasmas. From the plasma properties, we identify two classes of CSPN X-ray emission: (1) high-temperature plasmas with X-ray luminosities, L X , that appear uncorrelated with the CSPN bolometric luminosity, L bol and (2) lower-temperature plasmas with L X /L bol ∼ 10 −7 . We suggest these two classes correspond to the physical processes of magnetically active binary companions and self-shocking stellar winds, respectively. In many cases this conclusion is supported by corroborative multiwavelength evidence for the wind and binary properties of the PN central stars. By thus honing in on the origins of X-ray emission from PN central stars, we enhance the ability of CSPN X-ray sources to constrain models of PN shaping that invoke wind interactions and binarity.

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Section: Tracing the Origin Of X-ray Emitting Cspnesupporting

confidence: 70%

Section: Hot Pg1159-type Cspnementioning

confidence: 99%

THE CHANDRA PLANETARY NEBULA SURVEY (ChanPlaNS). III. X-RAY EMISSION FROM THE CENTRAL STARS OF PLANETARY NEBULAE

Montez

Kastner

Balick

et al. 2015

ApJ

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“…Near the time when the hot stellar core is exposed, the slow AGB wind, with terminal velocities 5-30 km s −1 (Eder et al 1988), is superseded by a fast stellar wind with terminal velocities 1,000-4,000 km s −1 (Cerruti-Sola & Perinotto 1985;Guerrero et al 2010). This fast stellar wind sweeps up the slower AGB wind to form a PN (Kwok 1983).…”

Section: Introductionmentioning

confidence: 99%

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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“…If the mass loss from the central star is driven by radiation pressure on resonance lines (Pauldrach et al 1988), then the terminal velocities are expected to be proportional to the escape velocities (Abbott 1978), which increase as the central stars evolve to higher temperatures at constant luminosities. It is estimated that approximately half of the PN central stars surveyed show evidence of fast winds (Cerruti-Sola and Perinotto 1985), suggesting that this is a common property. Figure 7 shows a schematic diagram of a PN system.…”

Section: Dynamical Energy Input From the Central Starmentioning

confidence: 99%

Planetary nebulae: A modern view

Kwok

1994

PASP

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ABSTRACT. Our current understanding of the origin and evolution of planetary nebulae is reviewed. We now recognize that a planetary nebula represents a dynamical system in which evolution is tightly coupled to the evolution of the central star. Not only is the ionization structure of the nebula controlled by the radiative output from the central star, the dynamics and morphology of the nebula are heavily influenced by the mechanical energy output from the central star. Since the time scale of evolution of the central star is strongly dependent on its mass, the extent of the radiative and mechanical interactions between the star and the nebula not only vary with time, but also vary with stellar mass. The physical properties of planetary nebulae are discussed in this context.

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Winds in central stars of planetary nebulae

Cited by 98 publications

References 0 publications

THE CHANDRA PLANETARY NEBULA SURVEY (ChanPlaNS). III. X-RAY EMISSION FROM THE CENTRAL STARS OF PLANETARY NEBULAE

THE CHANDRA PLANETARY NEBULA SURVEY (ChanPlaNS). III. X-RAY EMISSION FROM THE CENTRAL STARS OF PLANETARY NEBULAE

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

Planetary nebulae: A modern view

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