Transition from a Red Giant to a Blue Nucleus after Ejection of a Planetary Nebula

1975 ◽  
Vol 200 ◽  
pp. 324 ◽  
Author(s):  
R. Harm ◽  
M. Schwarzschild
Keyword(s):  
Planetary Nebula ◽  
Red Giant

scholarly journals A Speculation into the Origin of Neutral Globules in Planetary Nebulae: Could the Helix’s Comets Really be Comets?

1995 ◽  
Vol 12 (2) ◽  
pp. 170-173
Author(s):  
Grant Gussie
Keyword(s):  
Solar System ◽  
Planetary Nebula ◽  
Planetary Nebulae ◽  
Central Star ◽  
Oort Cloud ◽  
Asymptotic Giant Branch ◽  
Neutral Gas ◽  
Red Giant ◽  
The Masses

AbstractA novel explanation for the origin of the cometary globules within NGC 7293 (the ‘Helix’ planetary nebula) is examined, namely that these globules originate as massive cometary bodies at large astrocentric radii. The masses of such hypothetical cometary bodies would have to be several orders of magnitude larger than those of any such bodies observed in our solar system in order to supply the observed mass of neutral gas. It is, however, shown that comets at ‘outer Oort cloud’ distances are likely to survive past the red giant and asymptotic giant branch evolutionary phases of the central star, allowing them to survive until the formation of the planetary nebula. Some observational tests of this hypothesis are proposed.

scholarly journals Lower Limit for NPN's Masses

1989 ◽  
Vol 131 ◽  
pp. 454-454
Author(s):  
Amos Harpaz
Keyword(s):  
Mass Loss ◽  
Lower Limit ◽  
Planetary Nebula ◽  
Mass Range ◽  
Lower Mass ◽  
Single Star ◽  
Star Evolution ◽  
Low Mass ◽  
Red Giant

The lowest mass observed for a nucleus of a planetary nebula (NPN) is about 0.55 M⊙ (Weidemann and Koester, 1983, Schonberner, 1983). Hence, Lower mass WD's should have been produced without going through the phase of a visible PN ejection. Recently, Harpaz et al. (1987), have shown that very low mass WD's (up to 0.45 M⊙) can be formed by a single star evolution from red giant branch (RGB) stars, due to mass loss along the RGB. It turns out that WD's in mass range of 0.46–0.55 M⊙ formed by a single star evolution should be formed from the AGB, without an observable PN.

scholarly journals The post-common-envelope binary central star of the planetary nebula PN G283.7−05.1

2020 ◽  
Vol 642 ◽  
pp. A108 ◽  
Author(s):  
D. Jones ◽  
H. M. J. Boffin ◽  
J. Hibbert ◽  
T. Steinmetz ◽  
R. Wesson ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Main Sequence ◽  
Planetary Nebulae ◽  
Central Star ◽  
Radial Velocity Curve ◽  
Common Envelope ◽  
Low Mass ◽  
Red Giant ◽  
Model Temperature ◽  
Temperature Surface

We present the discovery and characterisation of the post-common-envelope central star system in the planetary nebula PN G283.7−05.1. Deep images taken as part of the POPIPlaN survey indicate that the nebula may possess a bipolar morphology similar to other post-common-envelope planetary nebulae. Simultaneous light and radial velocity curve modelling reveals that the newly discovered binary system comprises a highly irradiated M-type main-sequence star in a 5.9-hour orbit with a hot pre-white dwarf. The nebular progenitor is found to have a particularly low mass of around 0.4 M⊙, making PN G283.7−05.1 one of only a handful of candidate planetary nebulae that is the product of a common-envelope event while still on the red giant branch. In addition to its low mass, the model temperature, surface gravity, and luminosity are all found to be consistent with the observed stellar and nebular spectra through comparison with model atmospheres and photoionisation modelling. However, the high temperature (Teff ∼ 95 kK) and high luminosity of the central star of the nebula are not consistent with post-RGB evolutionary tracks.

scholarly journals From AGB to PN in External Galaxies

1995 ◽  
Vol 10 ◽  
pp. 490-492
Author(s):  
Cesare Chiosi
Keyword(s):  
Chemical Composition ◽  
Planetary Nebula ◽  
Elliptical Galaxies ◽  
Asymptotic Giant Branch ◽  
Star Formation History ◽  
Horizontal Branch ◽  
Chemical Enrichment ◽  
Formation History ◽  
External Galaxies ◽  
Red Giant

AbstractWe present new results from spectro-photometric models for elliptical galaxies in which detailed descriptions of the star formation history and chemical enrichment are taken into account. In particular, we focus on the important role played stars of different chemical composition evolving along the red giant branch (RGB), horizontal branch (HB), asymptotic giant branch (AGB), and finally planetary nebula (PN) stages in relation to the sources of UV flux in elliptical galaxies. A few important applications of these new galaxy models are briefly outlined.

scholarly journals Fast Winds in Planetary Nebulae

1983 ◽  
Vol 103 ◽  
pp. 305-316 ◽  
Author(s):  
F. D. Kahn
Keyword(s):  
Planetary Nebula ◽  
Planetary Nebulae ◽  
Central Star ◽  
Taylor Instability ◽  
Considerable Time ◽  
Left Behind ◽  
Hot Gas ◽  
Fast Wind ◽  
Rayleigh Taylor Instability ◽  
Red Giant

A planetary nebula consists mainly of gas ejected slowly by a red giant. Its dynamics is dominated by the hot central star which is left behind later. In particular a fast wind from this star forms a bubble of hot gas which fills the inner part of the nebula and pushes the envelope into a shell. This shell remains only partly ionized for a considerable time. Its non-ionized part is subject to a Rayleigh-Taylor instability, and is expected to break up into fragments which remain behind in the HII part of the nebula.

scholarly journals The cooling-down central star of the planetary nebula SwSt 1: a late thermal pulse in a massive post-AGB star?

2020 ◽  
Vol 498 (1) ◽  
pp. 1205-1220
Author(s):  
Marcin Hajduk ◽  
Helge Todt ◽  
Wolf-Rainer Hamann ◽  
Karolina Borek ◽  
Peter A M van Hoof ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Central Star ◽  
Line Flux ◽  
Stellar Spectrum ◽  
Thermal Pulse ◽  
Ultraviolet Spectra ◽  
Stellar Temperature ◽  
Released Energy ◽  
Red Giant ◽  
Born Again

ABSTRACT SwSt 1 (PN G001.5-06.7) is a bright and compact planetary nebula containing a late [WC]-type central star. Previous studies suggested that the nebular and stellar lines are slowly changing with time. We studied new and archival optical and ultraviolet spectra of the object. The [O iii] 4959 and 5007 Å to H β line flux ratios decreased between about 1976 and 1997/2015. The stellar spectrum also shows changes between these epochs. We modelled the stellar and nebular spectra observed at different epochs. The analyses indicate a drop of the stellar temperature from about 42 kK to 40.5 kK between 1976 and 1993. We do not detect significant changes between 1993 and 2015. The observations show that the star performed a loop in the H–R diagram. This is possible when a shell source is activated during its post-AGB evolution. We infer that a late thermal pulse (LTP) experienced by a massive post-AGB star can explain the evolution of the central star. Such a star does not expand significantly as the result of the LTP and does not became a born-again red giant. However, the released energy can remove the tiny H envelope of the star.

scholarly journals Molecular Radio Line Observations of Mass Loss From Red Giants

1989 ◽  
Vol 106 ◽  
pp. 321-338
Author(s):  
H. Olofsson
Keyword(s):  
Mass Loss ◽  
Planetary Nebula ◽  
Loss Rate ◽  
Mass Loss Rate ◽  
Central Star ◽  
Circumstellar Envelope ◽  
Red Giants ◽  
Radio Line ◽  
Red Giant ◽  
Evolution With Time

AbstractThe number of molecules detected at radio wavelengths in envelopes around red giants stands presently at 36. Among these OH and CO have proven to be the most useful for the study of the physical characteristics of a circumstellar envelope. The mass loss rate of the central star can be relatively accurately estimated and it appears possible to trace its evolution with time. Also fascinating objects in transition from the red giant phase to the planetary nebula phase are becoming observationally accessible.

scholarly journals The planetary nebula luminosity function

2012 ◽  
Vol 8 (S289) ◽  
pp. 247-254
Author(s):  
Robin Ciardullo
Keyword(s):  
Planetary Nebula ◽  
Surface Brightness ◽  
Luminosity Function ◽  
Zero Point ◽  
Theoretical Explanation ◽  
Number Of Factors ◽  
Surface Brightness Fluctuations ◽  
Type Ia ◽  
Red Giant ◽  
Supernovae Type Ia

AbstractAlthough the method has no theoretical explanation, the [Oiii]λ5007Å planetary nebula luminosity function (PNLF) is an extremely valuable tool for obtaining accurate (< 10%) extragalactic distances out to ~ 18 Mpc. Because the PNLF works in large galaxies of all Hubble types, it is one of the best tools we have for cross-checking the results of other methods and identifying systematic offsets between the Population I and Population II distance ladders. We review the PNLF's calibration and show that the method's Cepheid-derived zero point is virtually identical to that inferred from measurements of the tip of the red giant branch. We then compare the PNLF to the surface brightness fluctuations method and demonstrate that the latter's calibration yields a distance scale that is ~ 15% larger than that of the PNLF. We argue that this offset is likely due to a number of factors, including the effects of reddening on both of the techniques. We conclude by discussing the use of the PNLF for supernovae Type Ia calibration and considering the outstanding problems associated with the method.

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