A silicate disk in the heart of the Ant

Chesneau, O.; Lykou, Foteini; Balick, Bruce; Lagadec, E.; Matsuura, M.; Smith, Nathan; Spang, A.; Wolf, S.; Zijlstra, A. A.

doi:10.1051/0004-6361:20078268

Cited by 40 publications

(55 citation statements)

References 28 publications

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“…Livio & Soker 2001) made several authors suggest that M 2-9 contains a symbiotic star at its centre. Schmeja & Kimeswerner (2001) Movie is only available in electronic form at http://www.aanda.org several authors have pointed out that these colours can also be produced by dusty discs (Chesneau et al 2007;Cohen et al 2011;Lykou et al 2011). Figure 1 illustrates the morphology of M 2-9.…”

Section: Introductionmentioning

confidence: 99%

The evolution of M 2–9 from 2000 to 2010

Corradi

Balick

Santander-García

2011

A&A

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Context. Understanding the formation of collimated outflows is one of the most debated and controversial topics in the study of the late stages of stellar evolution. Aims. M 2-9 is an outstanding representative of extreme aspherical flows. It presents unique features such as a pair of high-velocity dusty polar blobs and a mirror-symmetric rotating pattern in the inner lobes. Their study provides important information on the nature of the poorly understood central source of M 2-9 and its nebula. Methods. Imaging monitoring at sub-arcsec resolution of the evolution of the nebula in the past decade is presented. Spectroscopic data provide complementary information. Results. We determine the proper motions of the dusty blobs, which infer a new distance estimate of 1.3 ± 0.2 kpc, a total nebular size of 0.8 pc, a speed of 147 km s −1 , and a kinematical age of 2500 yr. The corkscrew geometry of the inner rotating pattern is confirmed and quantified. Different recombination timescales for different ions explain the observed surface brightness distribution. According to the images taken after 1999, the pattern rotates with a period of 92 ± 4 years. On the other hand, the analysis of images taken between 1952 and 1977 measures a faster angular velocity. If the phenomenon were related to orbital motion, this would correspond to a modest orbital eccentricity (e = 0.10 ± 0.05), and a slightly shorter period (86 ± 5 years). New features have appeared after 2005 on the west side of the lobes and at the base of the pattern. Conclusions. The geometry and travelling times of the rotating pattern support our previous proposal that the phenomenon is produced by a collimated spray of high velocity particles (jet) from the central source, which excites the walls of the inner cavity of M 2-9, rather than by a ionizing photon beam. The speed of such a jet would be remarkable: between 11 000 and 16 000 km s −1 . The rotatingjet scenario may explain the formation and excitation of most of the features observed in the inner nebula, with no need for additional mechanisms, winds, or ionization sources. All properties point to a symbiotic-like interacting binary as the central source of M 2-9. The new distance determination implies system parameters that are consistent with this hypothesis.

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Section: Introductionmentioning

confidence: 99%

The evolution of M 2–9 from 2000 to 2010

Corradi

Balick

Santander-García

2011

A&A

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“…Discs can be formed during wind accretion preceding common envelope stage as well (Mastrodemos & Morris 1998), Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, ESO N: 079.D-146. 1 http://www.astro.washington.edu/users/balick/WFPC2/ index.html but have too low a mass to be the direct cause of the shaping of the older nebula (Chesneau et al 2007). The discs appear to be a remnant of the shaping process.…”

Section: Introductionmentioning

confidence: 99%

“…Observations of such small structures near evolved stars can only be performed with the use of high-angular resolution techniques like the infrared Very Large Telescope Interferometer (VLTI), i.e. planetary nebulae (Chesneau et al , 2007Lagadec et al 2006); VLTP star (Chesneau et al 2009); Mira stars (Tatebe et al 2006(Tatebe et al , 2007(Tatebe et al , 2008; carbon stars (Ohnaka & Boboltz 2008;Sacuto et al 2011;Deroo et al 2007b); OH/IR stars (Deroo et al 2007a,b;Chesneau et al 2005b); post-AGB stars (Deroo et al 2006;Matsuura et al 2006); proto-planetary nebulae (Murakawa et al 2008;Ohnaka et al 2006). Two of the best-studied examples of elongated and axisymmetric bipolar planetary nebulae are M2-9 and Menzel 3.…”

Section: Introductionmentioning

confidence: 99%

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A disc inside the bipolar planetary nebula M2-9

Lykou

Chesneau

Zijlstra

et al. 2011

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Aims. Bipolarity in proto-planetary and planetary nebulae is associated with events occurring in or around their cores. Past infrared observations have revealed the presence of dusty structures around the cores, many in the form of discs. Characterising those dusty discs provides invaluable constraints on the physical processes that govern the final mass expulsion of intermediate mass stars. We focus this study on the famous M2-9 bipolar nebula, where the moving lighthouse beam pattern indicates the presence of a wide binary. The compact and dense dusty core in the centre of the nebula can be studied by means of optical interferometry. Methods. M2-9 was observed with VLTI/MIDI at 39-47 m baselines with the UT2-UT3 and UT3-UT4 baseline configurations. These observations are interpreted using a dust radiative transfer Monte Carlo code. Results. A disc-like structure is detected perpendicular to the lobes, and a good fit is found with a stratified disc model composed of amorphous silicates. The disc is compact, 25 × 35 mas at 8 μm and 37 × 46 mas at 13 μm. For the adopted distance of 1.2 kpc, the inner rim of the disc is ∼15 AU. The mass represents a few percent of the mass found in the lobes. The compactness of the disc puts strong constraints on the binary content of the system, given an estimated orbital period 90-120 yr. We derive masses of the binary components between 0.6-1.0 M for a white dwarf and 0.6-1.4 M for an evolved star. We present different scenarios on the geometric structure of the disc accounting for the interactions of the binary system, which includes an accretion disc as well.

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“…The outer nebulae show a large variety of morphological characteristics, including tori, bipolar flows, and ellipsoidal shapes (e.g., Ramos-Larios et al 2008), with typical sizes of 10 4 -10 5 AU. But embedded in these nebulae a central dust disk has sometimes been discovered with sizes of order 10 2 AU, which can be resolved with the VLT interferometer (e.g., Chesneau et al 2007). The disks appear well aligned with the outer nebulae but are of too low mass to have directly affected their formation.…”

Section: Introductionmentioning

confidence: 99%

Disk evaporation in a planetary nebula

Gęsicki

Zijlstra

Szyszka

et al. 2010

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Aims. Binary interactions are believed to be important contributors to the structures seen in planetary nebulae (PN), and the sole cause of the newly discovered compact dust disks. The evolution of these disks is not clear, nor are the binary parameters required for their creation. Methods. Using HST imaging and VLT spectroscopy, both long-slit and integral field, we study the Galactic bulge planetary nebula M 2-29 for which a 3-year eclipse event of the central star has been attributed to a dust disk. Results. The central PN cavity of M 2-29 is being filled with a decreasingly, slow wind. An inner high density core is detected, of radius smaller than 250 AU, interpreted as a rotating gas/dust disk with a bipolar disk wind. The evaporating disk is argued to be the source of the slow wind. The central star is the source of a very fast wind (∼10 3 km s −1 ). An outer, partial ring is seen in the equatorial plane, expanding at 12 km s −1 . The azimuthal asymmetry is attributed to mass-loss modulation by an eccentric binary. A crucial point in disk evolution is represented by M 2-29 where ionization causes the gas to be lost, leaving a low-mass dust disk behind.

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A silicate disk in the heart of the Ant

Cited by 40 publications

References 28 publications

The evolution of M 2–9 from 2000 to 2010

The evolution of M 2–9 from 2000 to 2010

A disc inside the bipolar planetary nebula M2-9

Disk evaporation in a planetary nebula

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