The<i>η</i>Carinae spectrum of SS73 11 (=Ve 2-27)

Landaberry, S. J. C.; Pereira, C. B.; Araújo, F. X. de

doi:10.1051/0004-6361:20010947

Cited by 17 publications

(25 citation statements)

References 23 publications

(20 reference statements)

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“…In addition, the characteristic size of the CS dust in most symbiotic stars -except those with a Mira star -is reported to be of the order of 1 AU by Leedjärv (2006), while the uniform disc diameter of Hen 3-1191 is ≈30 AU per kpc of distance. Furthermore, Hen 3-1191 does not show evidence of the presence of a late-type companion (absence of TiO lines according to Landaberry et al 2001) Feast et al (1977). On the contrary, le Bertre et al (1989) measured little variability (<0.1 mag over the near-IR).…”

Section: The Symbiotic Star Hypothesismentioning

confidence: 90%

Resolving the B[e] star Hen 3-1191 at 10 $\mathsf{\mu}$m with VLTI/MIDI

Lachaume

Preibisch

Driebe

et al. 2007

A&A

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We report spatially resolved, spectrally dispersed N-band observations of the B[e] star Hen 3-1191 with the MIDI instrument of the Very Large Telescope Interferometer. The object is resolved with a 40 m baseline and has an equivalent uniform disc diameter ranging from 24 mas at 8 µm to 36 mas at 13 µm. The MIDI spectrum and visibilities show a curvature which can arise from a weak silicate feature in which the object appears ≈15% larger than in the continuum, but this could result from a change in the object's geometry within the band. We then model Hen's 3-1191 spectral energy distribution (.4−60 µm) and N-band visibilities. Because of the unknown nature of the object, we use a wide variety of models for objects with IR excesses. We find the observations to be consistent with a disc featuring an unusually high mass accretion and a large central gap almost void of matter, an excretion disc, and a binary made of two IR sources. We are unable to find a circumstellar shell model consistent with the data. We review the different hypotheses concerning the physical nature of the star and conclude that it is neither a Be supergiant nor a symbiotic star. However, we could not discriminate between the scenario of a young stellar object featuring an unusually strong FU Orionis-like outburst of mass accretion (4−250×10 −4 M /yr) and that of a protoplanetary nebula with an equatorial mass excretion rate > ∼ 4 × 10 −5 M /yr. In both cases, taking the additional presence of an envelope or wind into account would result in lower mass flows.

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Section: The Symbiotic Star Hypothesismentioning

confidence: 90%

Resolving the B[e] star Hen 3-1191 at 10 $\mathsf{\mu}$m with VLTI/MIDI

Lachaume

Preibisch

Driebe

et al. 2007

A&A

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“…In 1999, this value is almost constant for Hδ, Hγ, and Hβ, ∼35 km s −1 . However in 1 In order to identify the lines, we used the line lists provided by Moore (1945), Thackeray (1967), and Landaberry et al (2001). We also looked up two sites on the web: NIST Atomic Spectra Database Lines Form (URL physics.nist.gov/cgi-bin/AtData/lines_form) and The Atomic Line List v2.04 (URL http://www.pa.uky.edu/~peter/ atomic) 2007, this value is quite different for each line, 95 km s −1 (Hδ), 60 km s −1 (Hγ) and 50 km s −1 (Hβ).…”

Section: -Hydrogenmentioning

confidence: 99%

The galactic unclassified B[e] star HD 50138

Fernandes

Kraus²,

Chesneau

et al. 2009

A&A

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Context. The observed spectral variation of HD 50138 has led different authors to classify it in a very wide range of spectral types and luminosity classes (from B5 to A0 and III to Ia) and at different evolutionary stages as either HAeBe star or classical Be. Aims. Based on new high-resolution optical spectroscopic data from 1999 and 2007 associated to a photometric analysis, the aim of this work is to provide a deep spectroscopic description and a new set of parameters for this unclassified southern B[e] star and its interstellar extinction. Methods. From our high-resolution optical spectroscopic data separated by 8 years, we perform a detailed spectral description, presenting the variations seen and discussing their possible origin. We derive the interstellar extinction to HD 50138 by taking the influences of the circumstellar matter in the form of dust and an ionized disk into account. Based on photometric data from the literature and the new Hipparcos distance, we obtain a revised set of parameters for HD 50138. Results. Because of the spectral changes, we tentatively suggest that a new shell phase could have taken place prior to our observations in 2007. We find a color excess value of E(B − V) = 0.08 mag, and from the photometric analysis, we suggest that HD 50138 is a B6-7 III-V star. A discussion of the different evolutionary scenarios is also provided.

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“…The line identification was carried out using the line lists provided by Moore (1945), Garcia-Lario et al (1998), Landaberry et al (2001) and Fernandes et al (2001). We also looked up two sites on the web: NIST Atomic Spectra Database Lines Form (URL physics.nist.gov/cgi/AtData/lines) and The Atomic Line List v2.04 (URL www.pa.uky.edu/peter/atomic/).…”

Section: Description Of the Spectrummentioning

confidence: 99%