A New Look at the Evolution of Wolf‐Rayet Central Stars of Planetary Nebulae

2002 ◽  
Vol 114 (796) ◽  
pp. 602-611 ◽  
Author(s):  
Orsola De Marco ◽  
Noam Soker
Keyword(s):  
Planetary Nebulae ◽  
Central Stars ◽  
New Look

scholarly journals Planetary Nebula Evolution Traced by Distance-Independent Parameters

1993 ◽  
Vol 155 ◽  
pp. 480-480
Author(s):  
C.Y. Zhang ◽  
S. Kwok
Keyword(s):  
Physical Properties ◽  
Mass Distribution ◽  
Planetary Nebula ◽  
Strong Support ◽  
Planetary Nebulae ◽  
Central Star ◽  
Evolution Model ◽  
The Core ◽  
Independent Parameters ◽  
Central Stars

Making use of the results from recent infrared and radio surveys of planetary nebulae, we have selected 431 nebulae to form a sample where a number of distance-independent parameters (e.g., Tb, Td, I60μm and IRE) can be constructed. In addition, we also made use of other distance-independent parameters ne and T∗ where recent measurements are available. We have investigated the relationships among these parameters in the context of a coupled evolution model of the nebula and the central star. We find that most of the observed data in fact lie within the area covered by the model tracks, therefore lending strong support to the correctness of the model. Most interestingly, we find that the evolutionary tracks for nebulae with central stars of different core masses can be separated in a Tb-T∗ plane. This implies that the core masses and ages of the central stars can be determined completely independent of distance assumptions. The core masses and ages have been obtained for 302 central stars with previously determined central-star temperatures. We find that the mass distribution of the central stars strongly peaks at 0.6 M⊙, with 66% of the sample having masses <0.64 MM⊙. The luminosities of the central stars are then derived from their positions in the HR diagram according to their core masses and central star temperatures. If this method of mass (and luminosity) determination turns out to be accurate, we can bypass the extremely unreliable estimates for distances, and will be able to derive other physical properties of planetary nebulae.

scholarly journals The long-period binary central stars of the planetary nebulae NGC 1514 and LoTr 5

2017 ◽  
Vol 600 ◽  
pp. L9 ◽  
Author(s):  
D. Jones ◽  
H. Van Winckel ◽  
A. Aller ◽  
K. Exter ◽  
O. De Marco
Keyword(s):  
Planetary Nebulae ◽  
Long Period ◽  
Central Stars

scholarly journals Analysis of chemical abundances in planetary nebulae with [WC] central stars

2013 ◽  
Vol 558 ◽  
pp. A122 ◽  
Author(s):  
Jorge García-Rojas ◽  
Miriam Peña ◽  
Christophe Morisset ◽  
Gloria Delgado-Inglada ◽  
Adal Mesa-Delgado ◽  
...  
Keyword(s):  
Planetary Nebulae ◽  
Chemical Abundances ◽  
Central Stars

scholarly journals Imaging the elusive H-poor gas in planetary nebulae with large abundance discrepancy factors

2016 ◽  
Vol 12 (S323) ◽  
pp. 65-69 ◽  
Author(s):  
Jorge García-Rojas ◽  
Romano L. M. Corradi ◽  
Henri M. J. Boffin ◽  
Hektor Monteiro ◽  
David Jones ◽  
...  
Keyword(s):  
Planetary Nebulae ◽  
Tunable Filter ◽  
Close Binary ◽  
Chemical Abundances ◽  
Dual Nature ◽  
Gas Phases ◽  
Binary Evolution ◽  
The Universe ◽  
Central Stars

AbstractThe discrepancy between abundances computed using optical recombination lines (ORLs) and collisionally excited lines (CELs) is a major, unresolved problem with significant implications for the determination of chemical abundances throughout the Universe. In planetary nebulae (PNe), the most common explanation for the discrepancy is that two different gas phases coexist: a hot component with standard metallicity, and a much colder plasma enhanced in heavy elements. This dual nature is not predicted by mass loss theories, and direct observational support for it is still weak. In this work, we present our recent findings that demonstrate that the largest abundance discrepancies are associated with close binary central stars. OSIRIS-GTC tunable filter imaging of the faint O ii ORLs and MUSE-VLT deep 2D spectrophotometry confirm that O ii ORL emission is more centrally concentrated than that of [Oiii] CELs and, therefore, that the abundance discrepancy may be closely linked to binary evolution.

scholarly journals BINARY CENTRAL STARS OF PLANETARY NEBULAE DISCOVERED THROUGH PHOTOMETRIC VARIABILITY. IV. THE CENTRAL STARS OF HaTr 4 AND Hf 2-2

2016 ◽  
Vol 152 (2) ◽  
pp. 34 ◽  
Author(s):  
Todd C. Hillwig ◽  
Howard E. Bond ◽  
David J. Frew ◽  
S. C. Schaub ◽  
Eva H. L. Bodman
Keyword(s):  
Planetary Nebulae ◽  
Photometric Variability ◽  
Central Stars
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