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Title:
SALT HRS Discovery of the Binary Nucleus of the Etched Hourglass Nebula MyCn 18
Authors:
Miszalski, Brent; Manick, Rajeev; Mikolajewska, Joanna; Van Winckel, Hans; Ilkiewicz, Krystian
Affiliation:
AA(South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa; Southern African Large Telescope Foundation, PO Box 9, Observatory 7935, South Africa 0000-0003-2561-6306), AB(Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D bus 2401, B-3001 Leuven, Belgium), AC(Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, PL-00716 Warsaw, Poland), AD(Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D bus 2401, B-3001 Leuven, Belgium), AE(Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, PL-00716 Warsaw, Poland)
Publication:
Publications of the Astronomical Society of Australia, Volume 35, id.e027 11 pp. (PASA Homepage)
Publication Date:
06/2018
Origin:
CUP
Astronomy Keywords:
binaries: spectroscopic, planetary nebulae: general, planetary nebulae: individual: MyCn 18, stars: AGB and post-AGB, techniques: radial velocites
Abstract Copyright:
2018: Astronomical Society of Australia
DOI:
10.1017/pasa.2018.23
Bibliographic Code:
2018PASA...35...27M

Abstract

The shaping of various morphological features of planetary nebulae is increasingly linked to the role of binary central stars. Identifying a binary within a planetary nebula offers a powerful tool with which to directly investigate the formation mechanisms behind these features. The Etched Hourglass Nebula, MyCn 18, is the archetype for several binary-linked morphological features, yet it has no identified binary nucleus. It has the fastest jets seen in a planetary nebula of 630 km s-1, a central star position offset from the nebula centre, and a bipolar nebula with a very narrow waist. Here we report on the Southern African Large Telescope High Resolution Spectrograph detection of radial velocity variability in the nucleus of MyCn 18 with an orbital period of 18.15 ± 0.04 d and a semi-amplitude of 11.0 ± 0.3 km s-1. Adopting an orbital inclination of 38 ± 5° and a primary mass of 0.6 ± 0.1 M&sun; yields a secondary mass of 0.19 ± 0.05 M&sun; corresponding to an M5V companion. The detached nature of the binary rules out a classical nova as the origin of the jets and the offset central star as hypothesised in the literature. Furthermore, scenarios that produce the offset central star during the AGB and that form narrow waist bipolar nebulae result in orbital separations 80-800 times larger than observed in MyCn 18. The inner hourglass and jets may have formed from part of the common envelope ejecta that remained bound to the binary system in a circumbinary disk, whereas the offset central star position may best be explained by proper motion. Detailed simulations of MyCn 18 are encouraged that are compatible with the binary nucleus to further investigate its complex formation history.
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