Editing Appendix/Ramblings/OriginOfPlanetaryNebulae (section)

==Twentieth Century==
* [http://adsabs.harvard.edu/abs/2000ApJ...538..837S D. Sugimoto &amp; M. Y. Fujimoto (2000, ApJ, Vol. 538, pp. 837 - 853)], ''Why Stars Become Red Giants.'' <-- Good list of references in the article.

* [http://adsabs.harvard.edu/abs/1991ApJ...372..592B R. Bhaskar &amp; A. Nigam (1991, ApJ, Vol. 372, pp. 592 - 596)], ''Qualitative Explanations for Red Giant Formation.'' <-- &sect;3.3 lists ''Existing Explanations''
** [http://adsabs.harvard.edu/abs/1981ASSL...88..179E Eggleton &amp; Faulkner (1981, Proceedings &hellip; p. 179 - 182)], ''Why Do Stars Become Red Giants?''
** [http://adsabs.harvard.edu/abs/1984PhR...105..329I Iben &amp; Renzini (1984, Physics Reports, Vol. 105, Issue 6, pp. 329 - 406)], ''Single Star Evolution I.  Massive Stars and Early Evolution of Low and Intermediate Mass Stars.''
** [http://adsabs.harvard.edu/abs/1985ApJ...296..554Y A. Yahil &amp; L. van den Horn (1985, ApJ, Vol. 296, pp. 554 - 564)], ''Why do Giants Puff Up?''
** [http://adsabs.harvard.edu/abs/1988ApJ...329..803A J. H. Applegate (1988, ApJ, Vol. 329, pp. 803 - 807)], ''Why Stars Become Red Giants.''
** [http://adsabs.harvard.edu/abs/1989MNRAS.236..505W A. P. Whitworth (1989, MNRAS, Vol. 236, pp. 505 - 544)], ''Why Red Giants are Giant.''


* [http://adsabs.harvard.edu/abs/1975ApJ...200..324H R. H&auml;rm &amp; M. Schwarzschild (1975, ApJ, Vol. 200, pp. 324 - 329)], ''Transition from a Red Giant to a Blue Nucleus after Ejection of a Planetary Nebula.''
* [http://adsabs.harvard.edu/abs/1970ApJ...161..657K D. A. Keeley (1970, ApJ, Vol. 161, pp. 657 - 667)], ''Dynamical Models of Long-Period Variable Stars.''
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(p. 663) "The parameters of the model close to dynamical instability were <math>~M = 1.3 M_\odot</math> &hellip; and core mass-fraction <math>~=0.20</math>.  This model is the same as model 2.5 in Paper I = [http://adsabs.harvard.edu/abs/1970ApJ...161..643K D. A. Keeley (1970, ApJ, Vol. 161, p. 643)] &hellip; This model was calculated to test the possibility that an extreme red giant could eject its envelope and form a planetary nebula.  [http://adsabs.harvard.edu/abs/1966PASP...78..232A G. O. Abell &amp; P. Goldreich (1966, PASP, Vol. 78, P. 232)] presented arguments in favor of this hypothesis.  The problem was subsequently pursued by [http://adsabs.harvard.edu/abs/1968AcA....18..511P B. Paczynski (1968, Acta Astr., Vol. 18, p. 511)], [http://adsabs.harvard.edu/abs/1968IAUS...34..396P B. Paczynski &amp; J. Zi&oacute;lkowski (1968a)] and [http://adsabs.harvard.edu/abs/1968AcA....18..255P (1968b)] and the writer."
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Quote from Abell &amp; Goldreich (1966): 
* (p. 239) <font color="darkgreen">"We are therefore virtually forced to the conclusion that planetary nebulae are ejected more or less suddenly, although apparently not catastrophically, from stars of extremely large radii."</font>
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* [http://adsabs.harvard.edu/abs/1968IAUS...34..396P B. Paczynski &amp; J. Zi&oacute;lkowski (1968a, Proceedings from IAU Symposium no. 34: ''Planetary Nebulae'', ed. D. E. Osterbrock and Charles R. O'Dell, p. 396)], ''Dynamical Instability of the Envelopes of Red Supergiants and the Origin of Planetary Nebulae.''
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(p. 398) "We propose the following scheme for the late phases of stellar evolution.  After the exhaustion of helium [sic] in the core the star evolves into the region of red supergiants and moves up on the H-R diagram very close to the Hayashi border &hellip;  The mass of the helium and carbon core and the luminosity due to the helium and hydrogen-shell sources increase.  A star with total mass smaller than about 4 <math>~M_\odot</math> will terminate this type of evolution with an outflow of hydrogen-rich matter as a result of the dynamical instability of the extended envelope.  We suggest that planetary nebulae are formed in this way"
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* [http://adsabs.harvard.edu/abs/1968AcA....18..255P B. Paczynski &amp; J. Zi&oacute;lkowski (1968b)], ''Mira Variables.''
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(p. 265) "We suggest that a planetary nebula is formed in this way.  This process seems to be impossible for a star with larger mass.  In the latter case the mass of the core in which all the nuclear energy sources are exhausted will finally exceed the Chandrasekhar limit for degenerate configurations.  The dynamical instability of the core, followed by a supernova explosion may be expected &hellip;"
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* [http://adsabs.harvard.edu/abs/1972ApJ...176..395S R. L. Smith &amp; W. K. Rose (1972, ApJ, Vol. 176, pp. 395 - )], ''Relaxation Oscillations in the Envelopes of Luminous Red Giants.''
* [http://adsabs.harvard.edu/abs/1974ApJ...192..447K G. S. Kutter &amp; W. M. Sparks (1974, ApJ, Vol. 192, pp. 447 - 456)], ''Studies of Hydrodynamic Events in Stellar Evolution.  III. Ejection of Planetary Nebulae.''

* [https://ui.adsabs.harvard.edu/abs/1974ARA%26A..12..215I/abstract I. Iben, Jr. (1974, ARAA, Vol. 12, pp. 215-256)], ''Post Main Sequence Evolution of Single Stars.''
* [http://adsabs.harvard.edu/abs/2018Sci...362..201D K. De et al. (12 October 2018, Science, Vol. 362, No. 6411, pp. 201 - 206)], ''A Hot and Fast Ultra-stripped Supernova that likely formed a Compact Neutron Star Binary.''
* [http://adsabs.harvard.edu/abs/1994ApJS...92..125V E. Vassiliadis (1994, Astrophysical Journal Supplements Series, Vol. 92, pp. 125 - 144)], ''Post-Asymptotic Giant Branch Evolution of Low- to Intermediate-Mass Stars.''
* [http://adsabs.harvard.edu/abs/1995A%26A...299..755B T. Bl&ouml;cker (1995b, Astronomy &amp; Astrophysics, Vol. 299, pp. 755 - 769)], ''Stellar Evolution of Low- and Intermediate-Mass Stars.  II.  Post-AGB Evolution.''
* [http://adsabs.harvard.edu/abs/1995A%26A...297..727B T. Bl&ouml;cker (1995a, Astronomy &amp; Astrophysics, Vol. 297, pp. 727 - 738)], ''Stellar Evolution of Low- and Intermediate-Mass Stars.  I.  Mass Loss on the AGB and Its Consequences for Stellar Evolution.''
**(p. 727)  "Thus high mass losses must take place during the AGB evolution in order to remove the whole envelope before the core mass reaches the Chandrasekhar limit."
**(p. 728) "The physical mechanism of mass loss is not well understood up to now, and different approaches are discussed (cf. Lafon &amp; Berruyer 1991)"
* [http://adsabs.harvard.edu/abs/1991A%26ARv...2..249L J.-P. J. Lafon &amp; N. Berruyer (1991, Astronomy and Astrophysics Review, Vol. 2, April 1991, pp. 249 - 289)], ''Mass Loss Mechanisms in Evolved Stars''
* [http://adsabs.harvard.edu/abs/2008ASPC..401..166E B. R. Espey &amp; C. Crowley (2008)], Proceedings of the Conference on RS Ophiuchi (2006) and the Recurrent Nova Phenomenon, ASP Conference Series, Vol. 401, held 12 - 14 June, 2007 at Keele University, Keele, UK.  ''Mass-Loss from Red Giants''. (p. 166)
* Sequence of highly cited papers by Detlev Sch&ouml;nberner:
** [http://adsabs.harvard.edu/abs/1983ApJ...272..708S D. Sch&ouml;nberner (1983, ApJ, Vol. 272, pp. 708 - 714)], ''Late Stages of Stellar Evolution. II. -  Mass Loss and the Transition of Asymptotic Giant Branch Stars into Hot Remnants.''
* [http://adsabs.harvard.edu/abs/1981Ap.....17...92P L. S. Pilyugin &amp; G. S. Khromov (1981, Astrophysics, Vol. 17, no. 1, pp. 92 - 99)], ''The Origin of Planetary Nebulae.''
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(p. 98) "Of the three mechanisms considered earlier for the separation of the planetary nebula, preference must clearly be given to the ejection of a massive shell at a single time; for it is free of many of the difficulties inherent in the hypothesis of gradual accumulation of matter in the neighborhood of the star that is the precursor of the planetary nebula and its central star."
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* [http://adsabs.harvard.edu/abs/1986ApJ...308..706M I. Mazzitelli &amp; F. Dantona (1986, ApJ, Vol. 308, pp. 706 - 720)], ''Evolution from the Main Sequence to the White Dwarf Stage for a 3 Solar Mass Star.''
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(&sect; VI, p. 711) "&hellip; we summarize the major concepts which are currently accepted for the evolution through the PN stage." 
* i) "[http://adsabs.harvard.edu/abs/1981ASSL...88..431R Renzini (1981)] first considered that the very existence of PNs implies that, at a given time, the mass loss rate from asymptotic giant branch (AGB) stars must become much larger than the normal 'wind' rate (Reimers 1975).  This 'superwind' must be at least several times <math>~10^{-5} M_\odot~\mathrm{yr}^{-1}</math>.  
* ii) "The precise phase during the AGB evolution at which the super wind sets in is also a fundamental parameter for the following evolution, as the helium shell burning is more or less efficient at different stages. [http://adsabs.harvard.edu/abs/1984ApJ...277..333I Iben (1984)] followed numerically a number of cases, showing, for instance, how the complete loss of the hydrogen layer may be achieved if, after the PN ejection, there is the possibility of igniting a final helium shell flash."
* iii) "It is not clear at all whether PN ejection is a hydrodynamical event or not.  The few existing hydrodynamic computations (e.g., [http://adsabs.harvard.edu/abs/1974ApJ...192..447K Kutter and Sparks 1974]) do not consider the resulting behavior of the hydrostatic remnant, whose further evolution to the blue is crucial for the appearance of the PN.  many of the non hydrodynamical computations &#8212; starting from a fundamental paper by [http://adsabs.harvard.edu/abs/1975ApJ...200..324H H&auml;rm and Schwarzschild (1975)] and end with [http://adsabs.harvard.edu/abs/1984ApJ...277..333I Iben (1984)] &#8212; simulate the dynamics ejection by 'scaling' the models before ejection to smaller masses.  It is not proven that this procedure is physically meaningful."
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* [http://adsabs.harvard.edu/abs/1981ASSL...88..431R A. Renzini (1981, in Physical Processes in Red Giants; Proceedings of the Second Workshop, Erice, Italy, pp. 431 - 446)], ''Red Giants as Precursors of Planetary Nebulae.''
* [http://adsabs.harvard.edu/abs/1984ApJ...277..333I I. Iben, Jr. (1984, ApJ, Vol. 277, pp. 333 - 354)], ''On the Frequency of Planetary Nebula Nuclei Powered by Helium Burning and on the Frequency of White Dwarfs with Hydrogen-Deficient Atmospheres.''
* [https://ui.adsabs.harvard.edu/abs/1989IAUS..131..541H/abstract I. Hachisu &amp; M. Kato (1989)], in Planetary Nebulae.  Proceedings of the 131st. Symposium of the International Astronomical Union, held in Mexico City, Mexico, October 5 - 9, 1987.  Editor, Silvia Torres-Peimbert; Publisher, Kluwer Academic Publishers, Dordrecht, The Netherlands, Boston, MA, 1988:  ''Common Envelope Evolutions of Binary System and Formation of Planetary Nebulae''