Two’s company, three’s a crowd: SALT reveals the likely triple nature of the nucleus of the extreme abundance discrepancy factor planetary nebula Sp 3

Miszalski, B.; Manick, R.; Rauch, T.; Iłkiewicz, Krystian; Winckel, H. Van; Mikołajewska, Joanna

doi:10.1017/pasa.2019.36

Cited by 6 publications

(2 citation statements)

References 88 publications

(179 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The case of an AGB star that engulfs a tight binary system of two MSSs or of a white dwarf with a MSS is relevant to the formation of planetary nebulae, and in particular to planetary nebulae with 'messy' morphologies, i.e, that lack any kind of symmetry. 'Messy' planetary nebulae most like result from triple star interaction (e.g., Bear & Soker 2017;Danehkar et al 2018;Jones et al 2019;Miszalski et al 2019;Schreier et al 2019;Rechy-García et al 2020;Henney et al 2021). The spinning-up of the AGB envelope to have a rotation that is inclined to the triple star orbital angular momentum that I studied here adds to the 'messy' mass loss morphology.…”

Section: Discussion and Summarymentioning

confidence: 85%

Spin-orbit misalignment from triple-star common envelope evolution

Soker

2021

Preprint

View full text Add to dashboard Cite

I study a triple star common envelope evolution (CEE) of a tight binary system that is spiralingin inside a giant envelope and launches jets that spin-up the envelope with an angular momentum component perpendicular to the orbital angular momentum of the triple star system. This occurs when the orbital plane of the tight binary system and that of the triple star system are inclined to each other, so the jets are not along the triple star orbital angular momentum. The merger of the tight binary stars also tilts the envelope spin direction. If the giant is a red supergiant (RSG) star that later collapses to form a black hole (BH) the BH final spin is misaligned with the orbital angular momentum. Therefore, CEE of neutron star (NS) or BH tight binaries with each other or with one main sequence star (MSS) inside the envelope of an RSG, where the jets power a common envelope jets supernova (CEJSN) event, might end with a NS/BH-NS/BH close binary system with spin-orbit misalignment. Such binaries can later merge to be gravitational waves sources. I list five triple star scenarios that might lead to spin-orbit misalignments of NS/BH-NS/BH binary systems, two of which predict that the two spins be parallel to each other. In the case of a tight binary system of two MSSs inside an asymptotic giant branch star the outcome is an additional non-spherical component to the mass loss with the formation of a 'messy' planetary nebula.

show abstract

Section: Discussion and Summarymentioning

confidence: 85%

Spin-orbit misalignment from triple-star common envelope evolution

Soker

2021

Preprint

View full text Add to dashboard Cite

show abstract

“…Many observations and theoretical studies over the years, and more so in the last decade, attribute major roles to jets in shaping planetary nebulae (PNe; e.g., Morris 1987;Soker 1990;Sahai & Trauger 1998;Boffin et al 2012;Miszalski et al 2013;Tocknell et al 2014;Huang et al 2016;Sahai et al 2016;Rechy-García et al 2017;García-Segura et al 2016;Dopita et al 2018;Fang et al 2018;Kameswara Rao et al 2018;Lagadec 2018;Ali & Dopita 2019;Derlopa et al 2019;Jones et al 2019;Miszalski et al 2019;Orosz et al 2019;Scibelli et al 2019;Guerrero et al 2020;Monreal-Ibero & Walsh 2020;Rechy-García et al 2020;Soker 2020;Tafoya et al 2020;Zou et al 2020, for a small fraction of many more papers). Observations show a link between the presence of a binary central star and shaping by jets (e.g., Boffin et al 2012;Miszalski et al 2013Miszalski et al , 2018.…”

Section: Introductionmentioning

confidence: 99%

Shaping `Ears' in planetary nebulae by early jets

Akashi,

Soker

2020

Preprint

View full text Add to dashboard Cite

We conduct three dimensional hydrodynamical numerical simulations of planetary nebula (PN) shaping and show that jets that precede the ejection of the main PN shell can form the morphological feature of ears. Ears are two opposite protrusions from the main nebula that are smaller than the main nebula and with a cross section that decreases monotonically from the base of an ear at the shell to its far end. Only a very small fraction of PNe has ears. The short-lived jets, about a year in the present simulations, interact with the regular AGB wind to form the ears, while the later blown dense wind forms the main PN dense shell. Namely, the jets are older than the main PN shell. We also find that for the jets to inflate ears they cannot be too energetic, cannot be too wide, and cannot be too slow. A flow structure where short-lived jets precede the main phase of nebula ejection by a few years or less can result from a system that enters a common envelope evolution. The companion accretes mass through an accretion disk and launches jets just before it enters the envelope of the giant progenitor star of the PN. Shortly after that the companion enters the envelope and spirals-in to eject the envelope that forms the main PN shell.

show abstract

The ionised and molecular mass of post-common-envelope planetary nebulae

Santander-García

Jones

Alcolea

et al. 2022

A&A

View full text Add to dashboard Cite

Context. Most planetary nebulae (PNe) show beautiful, axisymmetric morphologies despite their progenitor stars being essentially spherical. Close binarity is widely invoked to help eject an axisymmetric nebula, after a brief phase of engulfment of the secondary within the envelope of the asymptotic giant branch (AGB) star, known as the common envelope (CE). The evolution of the AGB would thus be interrupted abruptly, with its still quite massive envelope being rapidly ejected to form the PN, which a priori would be more massive than the PN coming from a single version of the same star. Aims. We aim to test this hypothesis by investigating the ionised and molecular masses of a sample consisting of 21 post-CE PNe, roughly one-fifth of the known total population of these objects, and to compare them to a large sample of ‘regular’ (i.e. not known to arise from close-binary systems) PNe. Methods. We gathered data on the ionised and molecular content of our sample from the literature, and carried out molecular observations of several previously unobserved objects. We derived the ionised and molecular masses of the sample by means of a systematic approach, using tabulated, dereddened Hβ fluxes to find the ionised mass, and 12CO J = 2–1 and J = 3–2 observations to estimate the molecular mass. Results. There is a general lack of molecular content in post-CE PNe. Our observations only reveal molecule-rich gas around NGC 6778, which is distributed into a low-mass, expanding equatorial ring lying beyond the ionised broken ring previously observed in this nebula. The only two other objects showing molecular content (from the literature) are NGC 2346 and NGC 7293. Once we derive the ionised and molecular masses, we find that post-CE PNe arising from single-degenerate (SD) systems are just as massive, on average, as members of the ‘regular’ PNe sample, whereas post-CE PNe arising from double-degenerate systems are considerably more massive, and show substantially higher linear momentum and kinetic energy than SD systems and ‘regular’ PNe. Reconstruction of the CE of four objects, for which a wealth of data on the nebulae and complete orbital parameters are available, further suggests that the mass of SD nebulae actually amounts to a very small fraction of the envelope of their progenitor stars. This leads to the uncomfortable questions of where the rest of the envelope is and why we cannot detect it in the stars’ vicinity, raising serious doubts about our understanding of these intriguing objects.

show abstract

Two’s company, three’s a crowd: SALT reveals the likely triple nature of the nucleus of the extreme abundance discrepancy factor planetary nebula Sp 3

Cited by 6 publications

References 88 publications

Spin-orbit misalignment from triple-star common envelope evolution

Spin-orbit misalignment from triple-star common envelope evolution

Shaping `Ears' in planetary nebulae by early jets

The ionised and molecular mass of post-common-envelope planetary nebulae

Contact Info

Product

Resources

About