Accretion Disks in Pre–Planetary Nebulae

Reyes-Ruiz, M.; López, J. A.

doi:10.1086/307827

Cited by 49 publications

(62 citation statements)

References 30 publications

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“…Because low-mass companions do not release enough orbital energy to eject the envelope, as the orbital separation is reduced, the differential gravitational force due to the proto-WD tidally shreds the companion. The disrupted companion then forms a disk inside the CE that subsequently accretes onto the proto-WD (22). For more detail on the onset and dynamics of the CE phase for post-MS giants and low-mass companions (i.e., low, mass-ratio binaries), see refs.…”

Section: Common Envelope Evolutionmentioning

confidence: 99%

“…If the field generated in the envelope cannot diffuse to the WD surface, an alternative possibility is amplification in an accretion disk that forms when the companion is tidally disrupted inside the common envelope (22). As shown below, this scenario is attractive because it provides a natural mechanism for transporting the field to the proto-WD surface.…”

Section: Amplification Of Magnetic Fieldsmentioning

confidence: 99%

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Formation of high-field magnetic white dwarfs from common envelopes

Nordhaus

Wellons

Spiegel

et al. 2011

Proc. Natl. Acad. Sci. U.S.A.

114

116

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The origin of highly magnetized white dwarfs has remained a mystery since their initial discovery. Recent observations indicate that the formation of high-field magnetic white dwarfs is intimately related to strong binary interactions during post-main-sequence phases of stellar evolution. If a low-mass companion, such as a planet, brown dwarf, or low-mass star, is engulfed by a post-mainsequence giant, gravitational torques in the envelope of the giant lead to a reduction of the companion's orbit. Sufficiently low-mass companions in-spiral until they are shredded by the strong gravitational tides near the white dwarf core. Subsequent formation of a super-Eddington accretion disk from the disrupted companion inside a common envelope can dramatically amplify magnetic fields via a dynamo. Here, we show that these disk-generated fields are sufficiently strong to explain the observed range of magnetic field strengths for isolated, high-field magnetic white dwarfs. A higher-mass binary analogue may also contribute to the origin of magnetar fields.magnetohydrodynamics | compact objects

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Section: Common Envelope Evolutionmentioning

confidence: 99%

Section: Amplification Of Magnetic Fieldsmentioning

confidence: 99%

Formation of high-field magnetic white dwarfs from common envelopes

Nordhaus

Wellons

Spiegel

et al. 2011

Proc. Natl. Acad. Sci. U.S.A.

114

116

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show abstract

“…If the companion is of low mass ( brown dwarf or planet), it enters the AGB star and spirals in toward the core, where it is gravitationally shredded to form a disk that may blow jets through the envelope (Soker 1996;Reyes-Ruiz & López 1999;Nordhaus & Blackman 2006). A very low mass secondary has insufficient energy to eject much of the AGB envelope during the spiral-in process, so it does not naturally lead to the formation of a massive torus.…”

Section: Primary Accretion Disksmentioning

confidence: 99%

“…Four different types of scenario have been proposed for the formation of the jets: a magnetic wind from single stars (García-Segura et al 2005); an accretion disk around a binary companion, fed by the mass loss of the primary ( Morris 1987;Soker & Rappaport 2000); a magnetic ( possibly explosive) wind from the primary, spun up by a companion (e.g., Nordhaus & Blackman 2006;Matt et al 2006); and an accretion disk around the core of the primary, formed by the overflow or breakup of a binary companion during or after a common envelope phase (Soker & Livio 1994;Soker 1996;Reyes-Ruiz & López 1999;Nordhaus & Blackman 2006). In all these cases the region of jet launching is too small to be resolved by current observations.…”

Section: Introductionmentioning

confidence: 99%

Jets and Tori in Proto–Planetary Nebulae

Huggins¹

2007

ApJ

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We investigate the time sequence for the appearance of jets and molecular tori in the transition of stars from the asymptotic giant branch to the planetary nebula phase. Jets and tori are prominent features of this evolution, but their origins are uncertain. Using optical and millimeter line kinematics, we determine the ejection history in a sample of well-observed cases. We find that jets and tori develop nearly simultaneously. We also find evidence that jets typically appear slightly later than tori, with a lag time of a few hundred years. These characteristics provide strong evidence that jets and tori are physically related, and they set new constraints on theories of jet formation. The ejection of a discrete torus followed by jets on a short timescale favors the class of models in which a companion interacts with the central star. Models with long timescales, or with jets followed by a torus, are ruled out. Subject headingg s: circumstellar matter -planetary nebulae: general -stars: AGB and post-AGBstars: mass loss

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“…The dusty component of the outflows may imply that these, after emanating from the central regions of K 3-35, have entrained material from these inner regions, thus revealing additional interaction between the fast outflows and the dust cocoon. In these regards, K 3-35 is a notorious case study for models where high-velocity jets and disks are the basic ingredient in the shaping of the most axisymmetric PNe (Morris 1987;Soker 1996;Reyes-Ruiz & López 1999;Sahai & Trauger 1998;Soker & Rappaport 2000;Nordhaus & Blackman 2006;Huggins 2007).…”

Section: Discussionmentioning

confidence: 99%

Near- and mid-IR morphology of the water maser emitting planetary nebula K 3-35

Blanco

Guerrero

Miranda

et al. 2014

A&A

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The shaping process of planetary nebulae (PNe) takes place during the short transition from the asymptotic giant branch (AGB) phase to the white dwarf stage. The young PN K 3-35 represents a unique case where a small-sized water maser ring has been linked to the launch of collimated outflows that shape the nebula. The contrasting optical and radio continuum morphologies of K 3-35 indicate that they disclose different structural components that are apparently unconnected. To bridge the gap between optical and radio continuum observations, we present here new broadband and narrowband near-and mid-IR images of K 3-35. These images, and their comparison with optical and radio continuum images, are revealing. The radio continuum and mid-IR images are dominated by a compact source at the core of K 3-35 whose emission gives evidence of very dense ionized material embedded within a dust cocoon. The emission from the core, obscured at optical wavelengths, is faintly detected in the K s band. We suggest that the dust may shield the water molecules at the inner ring from the central star ionizing radiation. The precessing collimated outflows, very prominent in radio continuum, are also detected in mid-IR, very particularly in the [S iv] image. The mid-IR emission from these outflows consist mostly of ionized material, although the broadband filter at 11.85 μm seems to imply that a small amount of dust may be carried out by the outflow. The interactions of these outflows with the nebular shell result in shocks that excite the emission of H 2 as well as low-excitation lines from ionized species, such as [N ii] at the tips of the outflows.

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Accretion Disks in Pre–Planetary Nebulae

Cited by 49 publications

References 30 publications

Formation of high-field magnetic white dwarfs from common envelopes

Formation of high-field magnetic white dwarfs from common envelopes

Jets and Tori in Proto–Planetary Nebulae

Near- and mid-IR morphology of the water maser emitting planetary nebula K 3-35

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