The Peculiar Nebula M2-9

Allen, D. A.; Swings, J. P.

doi:10.1086/151520

Cited by 43 publications

(55 citation statements)

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“…Spectrophotometry of the core has shown an intrinsic amount of (high-excitation) iron emission lines ([Fe ii] and Fe iii], Allen & Swings 1972) This gives an electron temperature for the core ∼10 000 K and an electron density of 10 7 cm −3 (similar to Mz3, Smith 2003). As it is mentioned in that work, at such high core densities collisional de-excitation prevails and weak forbidden nitrogen lines in the core are not a surprise.…”

Section: The Mass Of the Components And An Accretion Discmentioning

confidence: 99%

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A disc inside the bipolar planetary nebula M2-9

Lykou

Chesneau

Zijlstra

et al. 2011

A&A

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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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Section: The Mass Of the Components And An Accretion Discmentioning

confidence: 99%

“…The lighthouse effect was witnessed by knots in the nebula known as early as 1952 (Allen & Swings 1972), was monitored from 1989 to 2007, revealing a period of ∼100 years. This feature can be created by orbital motion and is the best evidence that the core engulfs a binary system.…”

Section: Introductionmentioning

confidence: 99%

A disc inside the bipolar planetary nebula M2-9

Lykou

Chesneau

Zijlstra

et al. 2011

A&A

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“…In the 1970s, several authors (Geisel 1970;Ciatti et al 1974;Allen & Swings 1972, 1976 noticed that a peculiar group of Be stars showed forbidden emission lines together with a strong infrared excess. Members of this group were later referred as "B[e] stars" (see e.g.…”

Section: Introductionmentioning

confidence: 99%

First detections of FS Canis Majoris stars in clusters

Fuente

Najarro

Trombley

et al. 2015

A&A

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Context. FS CMa stars are low-luminosity objects showing the B[e] phenomenon whose evolutionary state remains a puzzle. These stars are surrounded by compact disks of warm dust of unknown origin. Hitherto, membership of FS CMa stars to coeval populations has never been confirmed. Aims. The discovery of low-luminosity line emitters in the young massive clusters Mercer 20 and Mercer 70 prompts us to investigate the nature of such objects. We intend to confirm membership to coeval populations in order to characterize these emission-line stars through the cluster properties.

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“…The evolutionary stage of MWC 922 is still unclear, and both pre and post-main sequence evolutionary status have been suggested (Tuthill & Lloyd 2007). The central object is mainly known for its infrared properties (Allen & Swings 1976). Allen & Swings (1976) give also a brief description of the optical properties of MWC 922 in their paper on B[e] stars with infrared excess.…”

Section: Introductionmentioning

confidence: 99%

“…The central object is mainly known for its infrared properties (Allen & Swings 1976). Allen & Swings (1976) give also a brief description of the optical properties of MWC 922 in their paper on B[e] stars with infrared excess. Whereas Fe II lines are mentioned absent in that paper, Rudy et al (1992) published the IR spectrum of MWC 922 and noted unusually strong Fe II and [Fe II] lines.…”

Section: Introductionmentioning

confidence: 99%

Search for DIBs in Emission: MWC 922 - The Red Square Nebula

et al. 2013

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Abstract. This work focusses on MWC 922, the central object in the Red Square Nebula. We obtained low and medium resolution spectra of both, the central object and the surrounding nebula, using the DIS and TSpec spectrograph. The spectra show the whole spectral range between ∼3 500Åup to ∼25 000Å. The central object shows a plethora of emission lines, including many Fe II and forbidden Fe [II] lines. Here, we present the inventory of the emission lines of the central object, MWC 922. Future work will comprise the identification of the nebula emission lines by using newly obtained X-Shooter spectra. That way we want to gain further insight into the physical and chemical conditions in this environment. A comparison of the Red Square to the Red Rectangle Nebula is anticipated and will guide our search for DIBs in emission.

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The Peculiar Nebula M2-9

Cited by 43 publications

References 0 publications

A disc inside the bipolar planetary nebula M2-9

A disc inside the bipolar planetary nebula M2-9

First detections of FS Canis Majoris stars in clusters

Search for DIBs in Emission: MWC 922 - The Red Square Nebula

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