X‐Ray Imaging of Planetary Nebulae with Wolf‐Rayet–type Central Stars: Detection of the Hot Bubble in NGC 40

2005 ◽  
Vol 635 (1) ◽  
pp. 381-385 ◽  
Author(s):  
Rodolfo Montez, Jr. ◽  
Joel H. Kastner ◽  
Orsola De Marco ◽  
Noam Soker
Keyword(s):  
Planetary Nebulae ◽  
X Ray ◽  
X Ray Imaging ◽  
Central Stars

scholarly journals X-ray emission from Planetary Nebulae

1997 ◽  
Vol 180 ◽  
pp. 214-215 ◽  
Author(s):  
Gail M. Conway ◽  
You-Hua Chu
Keyword(s):  
Planetary Nebulae ◽  
Point Sources ◽  
Stellar Winds ◽  
X Rays ◽  
Will Emit ◽  
X Ray ◽  
Extended Sources ◽  
Central Stars

X-ray emission from planetary nebulae (PNe) may originate from two sources: central stars which are 100,000–200,000 K will emit soft X-rays, and shocked fast stellar winds reaching 106–107 K will emit harder X-rays. The former are point sources, while the shocked winds are expected to be extended sources emitting continuously out to the inner wall of the visible nebular shell (Weaver et al. 1977; Wrigge & Wendker 1996).

scholarly journals The role of heat conduction to the formation of [WC]-type planetary nebulae

2011 ◽  
Vol 7 (S283) ◽  
pp. 494-495
Author(s):  
Christer Sandin ◽  
Matthias Steffen ◽  
Ralf Jacob ◽  
Detlef Schönberner ◽  
Ute Rühling ◽  
...  
Keyword(s):  
Heat Conduction ◽  
Chemical Composition ◽  
Physical Properties ◽  
Planetary Nebulae ◽  
Time Dependent ◽  
Diffuse Emission ◽  
Hydrodynamic Models ◽  
X Ray ◽  
Central Stars

AbstractX-ray observations of young Planetary Nebulæ (PNe) have revealed diffuse emission in extended regions around both H-rich and H-deficient central stars. In order to also reproduce physical properties of H-deficient objects, we have, at first, extended our time-dependent radiation-hydrodynamic models with heat conduction for such conditions. Here we present some of the important physical concepts, which determine how and when a hot wind-blown bubble forms. In this study we have had to consider the, largely unknown, evolution of the CSPN, the slow (AGB) wind, the fast hot-CSPN wind, and the chemical composition. The main conclusion of our work is that heat conduction is needed to explain X-ray properties of wind-blown bubbles also in H-deficient objects.

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

Galaxies ◽  
2020 ◽  
Vol 8 (1) ◽  
pp. 24
Author(s):  
Martín A. Guerrero
Keyword(s):  
Physical Properties ◽  
Planetary Nebulae ◽  
X Ray ◽  
Central Stars

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.

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

2015 ◽  
Vol 800 (1) ◽  
pp. 8 ◽  
Author(s):  
R. Montez Jr. ◽  
J. H. Kastner ◽  
B. Balick ◽  
E. Behar ◽  
E. Blackman ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Planetary Nebulae ◽  
X Ray ◽  
Central Stars

scholarly journals X-RAY EMISSION FROM THE BINARY CENTRAL STARS OF THE PLANETARY NEBULAE HFG 1, DS 1, AND LOTR 5

2010 ◽  
Vol 721 (2) ◽  
pp. 1820-1828 ◽  
Author(s):  
Rodolfo Montez ◽  
Orsola De Marco ◽  
Joel H. Kastner ◽  
You-Hua Chu
Keyword(s):  
Planetary Nebulae ◽  
X Ray ◽  
Central Stars

scholarly journals X-ray Shaping of Planetary Nebulae

Galaxies ◽  
2018 ◽  
Vol 6 (3) ◽  
pp. 98
Author(s):  
Martín Guerrero
Keyword(s):  
Stellar Wind ◽  
Essential Role ◽  
Planetary Nebulae ◽  
Asymptotic Giant Branch ◽  
Stellar Winds ◽  
Physical Processes ◽  
X Ray ◽  
Hot Gas ◽  
Energy And Momentum ◽  
Central Stars

The stellar winds of the central stars of planetary nebulae play an essential role in the shaping of planetary nebulae. In the interacting stellar winds model, the fast stellar wind injects energy and momentum, which are transferred to the nebular envelope through an X-ray-emitting hot bubble. Together with other physical processes, such as the ionization of the nebular envelope, the asymmetrical mass-loss in the asymptotic giant branch (AGB), and the action of collimated outflows and magnetic fields, the pressurized hot gas determines the expansion and evolution of planetary nebulae. Chandra and XMM-Newton have provided us with detailed information of this hot gas. Here in this talk I will review our current understanding of the effects of the fast stellar wind in the shaping and evolution of planetary nebulae and give some hints of the promising future of this research.

scholarly journals X-ray, EUV and infrared coronal-line radiation from Planetary Nebulae

1997 ◽  
Vol 180 ◽  
pp. 293-293
Author(s):  
S. A. Zhekov ◽  
M. Perinotto
Keyword(s):  
Thermal Conduction ◽  
Extreme Ultraviolet ◽  
Planetary Nebulae ◽  
Stellar Winds ◽  
Gas Temperature ◽  
Coronal Line ◽  
Temperature Plasma ◽  
Line Radiation ◽  
X Ray ◽  
Central Stars

The interacting stellar winds (ISW) theory (Kwok, S., Purton, C. R., Fitzgerald, P. M., 1978, ApJL, 219, L125) is nowadays widely accepted in the physics of Planetary Nebulae (PNe). It received much support from the observed fast winds in the central stars of PNe (CSPN), recognized to be a quite common phenomenon (e.g., Perinotto, M., 1993, in IAU Symp. No. 155, Planetary Nebulae, eds. R. Weinberger and A. Acker, Kluwer, Dordrecht, 57). Thus, the existance of a hot bubble in the PNe structure is a cornerstone of the ISW model. The high velocities (600–3500 km s–1) of the CSPN winds, are, according to the ISW model, directly responsible for an high gas temperature in the hot bubble, which is then expected to be the source of an extended X-ray and extreme ultraviolet (EUV) radiation. The PNe should also emit infrared coronal lines (IRCL) of highly ionized species since the high temperature plasma of the hot bubble is in contact with the much colder outer shell (optical PN) and the thermal conduction will produce a region of intermediate temperatures (5 × 105–106 K). A model considering the structure of the hot bubble in PNe with taking into account the thermal conductivity effects was present by Zhekov and Perinotto (1996, A&A, 309, 648).

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