TY - JOUR
T1 - Common Envelope Shaping of Planetary Nebulae. IV. From Proto-planetary to Planetary Nebula
AU - García-Segura, Guillermo
AU - Taam, Ronald E
AU - Ricker, Paul M
N1 - Funding Information:
We thank our referee, Orsola De Marco, for a careful reading of the manuscript and for her suggestions, which improved considerably the article. We thank Michael L. Norman and the Laboratory for Computational Astrophysics for the use of ZEUS-3D. The compu- tations were performed at the Instituto de Astronomía-UNAM at Ensenada. GG-S. is partially supported by CONACyT grant 178253. Partial support for this work has been provided by NSF through grants AST-0200876 and AST-0703950.
Publisher Copyright:
© 2022 The Author(s).
PY - 2022/12/1
Y1 - 2022/12/1
N2 - We present 2D hydrodynamical simulations of the transition of a protoplanetary nebula (PPN) to a planetary nebula for central stars in binary systems that have undergone a common-envelope event. After 1000 yr of magnetically driven dynamics (PPN phase), a line-driven stellar wind is introduced into the computational domain and the expansion of the nebula is simulated for another 10 000 yr, including the effects of stellar photoionization. In this study we consider central stars with main sequence (final) masses of 1 (0.569) and 2.5 (0.677) M⊙, together with a 0.6-M⊙ main-sequence companion. Extremely bipolar, narrow-waisted PPNe result in bipolar planetary nebulae, while the rest of the shapes mainly evolve into elliptical planetary nebulae. The initial magnetic field's effects on the collimated structures, such as jets, tend to disappear in most of the cases, leaving behind the remnants of those features in only a few cases. Equatorial zones fragmented mainly by photoionization (1-M⊙progenitors), result in 'necklace' structures made of cometary clumps aligned with the radiation field. On the other hand, fragmentation by photoionization and shocked wind (2.5-M⊙progenitors) give rise to the formation of multiple clumps in the latitudinal direction, which remain within the lobes, close to the center, which are immersed and surrounded by hot shocked gas, not necessarily aligned with the radiation field. These results reveal that the fragmentation process has a dependence on the stellar-mass progenitor. This fragmentation is made possible by the distribution of gas in the previous post-common-envelope PPN as sculpted by the action of the jets.
AB - We present 2D hydrodynamical simulations of the transition of a protoplanetary nebula (PPN) to a planetary nebula for central stars in binary systems that have undergone a common-envelope event. After 1000 yr of magnetically driven dynamics (PPN phase), a line-driven stellar wind is introduced into the computational domain and the expansion of the nebula is simulated for another 10 000 yr, including the effects of stellar photoionization. In this study we consider central stars with main sequence (final) masses of 1 (0.569) and 2.5 (0.677) M⊙, together with a 0.6-M⊙ main-sequence companion. Extremely bipolar, narrow-waisted PPNe result in bipolar planetary nebulae, while the rest of the shapes mainly evolve into elliptical planetary nebulae. The initial magnetic field's effects on the collimated structures, such as jets, tend to disappear in most of the cases, leaving behind the remnants of those features in only a few cases. Equatorial zones fragmented mainly by photoionization (1-M⊙progenitors), result in 'necklace' structures made of cometary clumps aligned with the radiation field. On the other hand, fragmentation by photoionization and shocked wind (2.5-M⊙progenitors) give rise to the formation of multiple clumps in the latitudinal direction, which remain within the lobes, close to the center, which are immersed and surrounded by hot shocked gas, not necessarily aligned with the radiation field. These results reveal that the fragmentation process has a dependence on the stellar-mass progenitor. This fragmentation is made possible by the distribution of gas in the previous post-common-envelope PPN as sculpted by the action of the jets.
KW - Stars: Evolution
KW - ISM: individual (Hubble 5, NGC 6302, NGC 2440)
KW - ISM: planetary nebulae
KW - Stars: binaries
KW - Stars: AGB and post-AGB
KW - Stars: Rotation
KW - stars: evolution
KW - stars: AGB and post-AGB
KW - stars: rotation
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U2 - 10.1093/mnras/stac2824
DO - 10.1093/mnras/stac2824
M3 - Article
SN - 0035-8711
VL - 517
SP - 3822
EP - 3831
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
M1 - stac2824
ER -