Jets and Tori in Proto–Planetary Nebulae

Huggins, P. J.

doi:10.1086/518415

Cited by 79 publications

(113 citation statements)

References 48 publications

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“…Note that K 3−35, the other PN showing maser emission at 1720 MHz, has also been inferred to host a magnetized disk (Miranda et al 2001;Gómez et al 2009). These equatorial ejections could be created, for instance, by binary interactions (Nordhaus & Blackman 2006;Huggins 2007). Magnetized equatorial structures traced by maser emission have also been found in post-AGB stars (Bains et al 2003(Bains et al , 2004, with similar values for the derived magnetic field as the ones found in PNe (Gómez et al 2009, and this paper).…”

Section: The Origin Of Oh Maser Emissionsupporting

confidence: 83%

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Qiao

Walsh

Gómez

et al. 2016

ApJ

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We report on OH maser emission toward G336.644−0.695 (IRAS 16333−4807), which is a H 2 O maser-emitting Planetary Nebula (PN). We have detected 1612, 1667, and 1720 MHz OH masers at two epochs using the Australia Telescope Compact Array, hereby confirming it as the seventh known case of an OH-maser-emitting PN. This is only the second known PN showing 1720 MHz OH masers after K 3−35 and the only evolved stellar object with 1720 MHz OH masers as the strongest transition. This PN is one of a group of very young PNe. The 1612 MHz and 1667 MHz masers are at a similar velocity to the 22 GHz H 2 O masers, whereas the 1720 MHz masers show a variable spectrum, with several components spread over a higher velocity range (up to 36 km s −1 ). We also detect Zeeman splitting in the 1720 MHz transition at two epochs (with field strengths of ∼2 to ∼10 mG), which suggests the OH emission at 1720 MHz is formed in a magnetized environment. These 1720 MHz OH masers may trace short-lived equatorial ejections during the formation of the PN.

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Section: The Origin Of Oh Maser Emissionsupporting

confidence: 83%

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Qiao

Walsh

Gómez

et al. 2016

ApJ

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“…which the flow radial velocity v rad increases linearly with the distance r from the origin (v rad ∝ r). This behavior is fairly common in protoplanetary nebulae (Corradi 2004;Huggins 2007) and eruptive stars (Weis et al 1999). It is believed to indicate that the outflow is dictated by self-similar expansion, confirming the ballistic character of the knot trajectory and the explosive dynamics of its ejection (Dennis et al 2008).…”

Section: Spectroscopymentioning

confidence: 65%

Discovery of a Giant, Highly Collimated Jet From Sanduleak's Star in the Large Magellanic Cloud

Angeloni¹,

Mille²,

Bland-Hawthorn³

et al. 2011

ApJ

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Highly collimated gas ejections are among the most dramatic structures in the universe, observed to emerge from very different astrophysical systems-from active galactic nuclei down to young brown dwarf stars. Even with the huge span in spatial scales, there is convincing evidence that the physics at the origin of the phenomenon, namely, the acceleration and collimation mechanisms, is the same in all classes of jets. Here we report on the discovery of a giant, highly collimated jet from Sanduleak's star in the Large Magellanic Cloud (LMC). With a physical extent of 14 pc at the distance of the LMC, it represents the largest stellar jet ever discovered, and the first resolved stellar jet beyond the Milky Way. The kinematics and extreme chemical composition of the ejecta from Sanduleak's star bear strong resemblance with the low-velocity remnants of SN1987A and with the outer filaments of the most famous supernova progenitor candidate, η Carinae. Moreover, the precise knowledge of the jets distance implies that it will be possible to derive accurate estimates of most of its physical properties. Sanduleak's bipolar outflow will thus become a crucial test bed for future theoretical modeling of astrophysical jets.

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“…The formation of the dense waists seen in PNe likely occurs during the early PPN or late-AGB phase. Waists and lobes are perhaps formed nearly simultaneously, as suggested by Huggins (2007) from a study of a small sample, with waists forming a bit earlier (the expansion timescales are ∼ few × 100 to 1000 yr). We need to focus our attention on the PPN and very late-AGB phases if we are to succesfully resolve fundamental issues in the formation of aspherical PNe.…”

Section: Introductionmentioning

confidence: 85%

Understanding the immediate progenitors of planetary nebulae

Sahai¹,

Morris²,

Contreras³

et al. 2011

Proc. IAU

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Abstract. Pre-Planetary Nebulae (PPNe) are believed to represent a relatively short, intermediate evolutionary phase in the evolution of AGB stars to Planetary Nebulae (PNe). Our unbiased, high-resolution imaging surveys with HST of young PNe and PPNe show very strong morphological similarities between these classes, enabling us to extend our morphological scheme for PPN classification to young PNe, preserving virtually all of the primary and secondary descriptors, and adding a few new ones. These morphological surveys show that the primary shaping of PNe begins during the PPNe and/or late-AGB phase, and the key to understanding the shaping process lies in the study of these PNe progenitors. Here we present results from two recent studies of PNe progenitors: (i) Hα emission with very broad wings and P-Cygni profiles as probes of the region where the fast post-AGB outflows that do the shaping are most likely launched from, and (ii) equatorial waists with large-sized dust grains and large masses.

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Jets and Tori in Proto–Planetary Nebulae

Cited by 79 publications

References 48 publications

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Discovery of a Giant, Highly Collimated Jet From Sanduleak's Star in the Large Magellanic Cloud

Understanding the immediate progenitors of planetary nebulae

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