Common Envelope Shaping of Planetary Nebulae

Garcı́a-Segura, Guillermo; Ricker, P. M.; Taam, Ronald E.

doi:10.3847/1538-4357/aac08c

Cited by 74 publications

(73 citation statements)

References 56 publications

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“…Our results show that the time-averaged density is maximal at the orbital plane and minimal along the poles. Thus for example, the interactions of an ejected CE will be affected by this gas distribution, even more the subsequent PNe formation (García-Segura et al 2018). This suggests that the connection between PNe symmetry axis and binary star parameters Table 2.…”

Section: Discussionmentioning

confidence: 99%

AGB winds in interacting binary stars

Bermúdez-Bustamante

Garcı́a-Segura

Steffen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We perform numerical simulations to investigate the stellar wind from interacting binary stars. Our aim is to find analytical formulae describing the outflow structure. In each binary system the more massive star is in the asymptotic giant branch and its wind is driven by a combination of pulsations in the stellar surface layers and radiation pressure on dust, while the less massive star is in the main sequence. Time averages of density and outflow velocity of the stellar wind are calculated and plotted as profiles against distance from the centre of mass and colatitude angle. We find that mass is lost mainly through the outer Lagrangian point L 2 . The resultant outflow develops into a spiral at low distances from the binary. The outflowing spiral is quickly smoothed out by shocks and becomes an excretion disk at larger distances. This leads to the formation of an outflow structure with an equatorial density excess, which is greater in binaries with smaller orbital separation. The pole-to-equator density ratio reaches a maximum value of ∼ 10 5 at Roche-Lobe Overflow state. We also find that the gas stream leaving L 2 does not form a circumbinary ring for stellar mass ratios above 0.78, when radiation pressure on dust is taken into account. Analytical formulae are obtained by curve fitting the 2-dimensional, azimuthally averaged density and outflow velocity profiles. The formulae can be used in future studies to setup the initial outflow structure in hydrodynamic simulations of common-envelope evolution and formation of planetary nebulae.

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Section: Discussionmentioning

confidence: 99%

AGB winds in interacting binary stars

Bermúdez-Bustamante

Garcı́a-Segura

Steffen

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Looking at the problem from the side of the PN morphology and kinematics, the evidence is strong that in those cases where the central star of a PNe has gone through CE evolution, there is also a link to the spatio-kinematic evolution of the nebula (Hillwig et al 2016), and some understanding how this works (García-Segura et al 2018). This adds strength to the question whether the estimated low percentage of close-binary systems among PNe is wrong.…”

Section: Termination Of Red Giant Evolutionmentioning

confidence: 99%

HD 101584: circumstellar characteristics and evolutionary status

Olofsson

Khouri

Maercker

et al. 2019

A&A

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Context. There is growing evidence that red giant evolution is often affected by an interplay with a nearby companion, in some cases taking the form of a common-envelope evolution. Aims. We have performed a study of the characteristics of the circumstellar environment of the binary object HD 101584, that provides information on a likely evolutionary scenario. Methods. We have obtained and analyzed ALMA observations, complemented with observations using APEX, of a large number of molecular lines. An analysis of the spectral energy distribution has also been performed. Results. Emissions from 12 molecular species (not counting isotopologues) have been observed, and most of them mapped with angular resolutions in the range 0 . 1 to 0 . 6. Four circumstellar components are identified: i) a central compact source of size ≈ 0 . 15, ii) an expanding equatorial density enhancement (a flattened density distribution in the plane of the orbit) of size ≈ 3 , iii) a bipolar high-velocity outflow (≈ 150 km s −1 ), and iv) an hourglass structure. The outflow is directed almost along the line of sight. There is evidence of a second bipolar outflow. The mass of the circumstellar gas is ≈ 0.5 [D/1 kpc] 2 M , about half of it lies in the equatorial density enhancement. The dust mass is ≈ 0.01 [D/1 kpc] 2 M , and a substantial fraction of this is in the form of large-sized, up to 1 mm, grains. The estimated kinetic age of the outflow is ≈ 770 [D/1 kpc] yr. The kinetic energy and the scalar momentum of the accelerated gas are estimated to be 7×10 45 [D/1 kpc] 2 erg and 10 39 [D/1 kpc] 2 g cm s −1 , respectively. Conclusions. We provide good evidence that the binary system HD 101584 is in a post-common-envelope-evolution phase, that ended before a stellar merger. Isotope ratios combined with stellar mass estimates suggest that the primary star's evolution was terminated already on the first red giant branch (RGB). Most of the energy required to drive the outflowing gas was probably released when material fell towards the companion.

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“…Once the hot core of an AGB star is revealed, it may illuminate the layers of expelled material to form a spectacular planetary nebula (PN). Binary companions to the central stars of PNe (CSPNe) are widely believed to be responsible for bipolar (axisymmetric) structures in PNe (see, e.g., Balick & Frank 2002;Balick 2004;García-Segura et al 2018). Many dC stars were likely born within planetary nebulae.…”

Section: The Planetary Nebula Connectionmentioning

confidence: 99%

A Chandra Study: Are Dwarf Carbon Stars Spun Up and Rejuvenated by Mass Transfer?

Green

Montez

Mazzoni

et al. 2019

ApJ

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Carbon stars (with C/O> 1) were long assumed to all be giants, because only AGB stars dredge up significant carbon into their atmospheres. The case is nearly iron-clad now that the formerly mysterious dwarf carbon (dC) stars are actually far more common than C giants, and have accreted carbon-rich material from a former AGB companion, yielding a white dwarf and a dC star that has gained both significant mass and angular momentum. Some such dC systems have undergone a planetary nebula phase, and some may evolve to become CH, CEMP, or Ba giants. Recent studies indicate that most dCs are likely from older, metal-poor kinematic populations. Given the well-known anti-correlation of age and activity, dCs would not be expected to show significant X-ray emission related to coronal activity. However, accretion spin-up might be expected to rejuvenate magnetic dynamos in these post mass-transfer binary systems. We describe our Chandra pilot study of six dCs selected from the SDSS for Hα emission and/or a hot white dwarf companion, to test whether their X-ray emission strength and spectral properties are consistent with a rejuvenated dynamo. We detect all 6 dCs in the sample, which have X-ray luminosities ranging from logL x ∼ 28.5 -29.7, preliminary evidence that dCs may be active at a level consistent with stars that have short rotation periods of several days or less. More definitive results require a sample of typical dCs with deeper X-ray observations to better constrain their plasma temperatures.

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Common Envelope Shaping of Planetary Nebulae

Cited by 74 publications

References 56 publications

AGB winds in interacting binary stars

AGB winds in interacting binary stars

HD 101584: circumstellar characteristics and evolutionary status

A Chandra Study: Are Dwarf Carbon Stars Spun Up and Rejuvenated by Mass Transfer?

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