On the population of galactic Luminous Blue Variables

Clark, J. S.; Larionov, V. M.; Arkharov, A. A.

doi:10.1051/0004-6361:20042563

Cited by 137 publications

(179 citation statements)

References 41 publications

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“…8). Based on the classification scheme presented by Clark et al (2011) for LBVs, the strong presence of He i 2.058 μm indicates that both of these stars are quite hot.…”

Section: Discussionmentioning

confidence: 99%

Probing the ejecta of evolved massive stars in transition

Oksala

Kraus

Cidale

et al. 2013

A&A

139

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Massive evolved stars in transition phases, such as luminous blue variables (LBVs), B[e] supergiants (B[e]SGs), and yellow hypergiants (YHGs), are not well understood, and yet crucial steps in determining accurate stellar and galactic evolution models. The circumstellar environments of these stars reveal their mass-loss history, identifying clues to both their individual evolutionary status and the connection between objects of different phases. Here we present a survey of 25 such evolved massive stars (16 B[e]SGs, 6 LBVs, 2 YHGs, and 1 Peculiar Oe star), observed in the K-band with the Spectrograph for INtegral Field Observation in the Near-Infrared (SINFONI; R = 4500) on the ESO VLT UT4 8 m telescope. The sample can be split into two categories based on spectral morphology: one group includes all of the B[e]SGs, the Peculiar Oe star, and two of the LBVs, while the other includes the YHGs and the rest of the LBVs. The difference in LBV spectral appearance is due to some objects being in a quiescent phase and some objects being in an active or outburst phase. CO emission features are found in 13 of our targets, with first time detections for MWC 137, LHA 120-S 35, and LHA 115-S 65. From model fits to the CO band heads, the emitting regions appear to be detached from the stellar surface. Each star with 12 CO features also shows 13 CO emission, signaling an evolved nature. Based on the level of 13 C enrichment, we conclude that many of the B[e]SGs are likely in a pre-Red Supergiant phase of their evolution. There appears to be a lower luminosity limit of log L/L = 5.0 below which CO is not detected. The lack of CO features in several high luminosity B[e]SGs and variability in others suggests that they may in fact be LBV candidates, strengthening the connection between these two very similar transition phases.

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“…8). Based on the classification scheme presented by Clark et al (2011) for LBVs, the strong presence of He i 2.058 μm indicates that both of these stars are quite hot.…”

Section: Discussionmentioning

confidence: 99%

Probing the ejecta of evolved massive stars in transition

Oksala

Kraus

Cidale

et al. 2013

A&A

139

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“…Moreover, their HIPPARCOS data do not show any periodic variations and thus do not influence the results of the analysis of the periodic components. There are also a few unconfirmed LBV candidates according to Clark et al (2005) within our sample but we cannot exclude them from this analysis without further evidence of their true status.…”

Section: Special Casesmentioning

confidence: 99%

A systematic study of variability among OB-stars based on HIPPARCOS photometry

Lefèvre

Марченко²,

Moffat

et al. 2009

A&A

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Context. Variability is a key factor for understanding the nature of the most massive stars, the OB stars. Such stars lie closest to the unstable upper limit of star formation. Aims. In terms of statistics, the data from the HIPPARCOS satellite are unique because of time coverage and uniformity. They are ideal to study variability in this large, uniform sample of OB stars. Methods. We used statistical techniques to determine an independant threshold of variability corresponding to our sample of OB stars, and then applied an automatic algorithm to search for periods in the data of stars that are located above this threshold. We separated the sample stars into 4 main categories of variability: 3 intrinsic and 1 extrinsic. The intrinsic categories are: OB main sequence stars (∼2/3 of the sample), OBe stars (∼10%) and OB Supergiant stars (∼1/4).The extrinsic category refers to eclipsing binaries. Results. We classified about 30% of the whole sample as variable, although the fraction depends on magnitude level due to instrumental limitations. OBe stars tend to be much more variable (≈80%) than the average sample star, while OBMS stars are below average and OBSG stars are average. Types of variables include α Cyg, β Cep, slowly pulsating stars and other types from the general catalog of variable stars. As for eclipsing binaries, there are relatively more contact than detached systems among the OBMS and OBe stars, and about equal numbers among OBSG stars.

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“…The selection of RSGs is described into the text. WR stars are from van der Hucht (2001); Messineo et al (2009Messineo et al ( , 2011, LBVs are from Clark et al (2005); Messineo et al (2011);Gvaramadze et al (2010); Mauerhan et al (2010Mauerhan et al ( , 2011. The continuous line near the bottom left corner is the locus of dwarf stars (Koornneef 1983), two dashed lines mark the traces of an O9 (lower) and an M5 (upper) star with increasing interstellar extinction.…”

Section: Sample Selectionmentioning

confidence: 99%

“…We considered a list of 42 confirmed or candidate LBVs in the Milky Way (Clark et al 2005;Messineo et al 2011;Gvaramadze et al 2010;Mauerhan et al 2010;Messineo et al 2009). We found 18 counterparts in the GLIMPSE catalog and 25 in the MSX catalog.…”

Section: Luminous Blue Variablesmentioning

confidence: 99%

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Near- and mid-infrared colors of evolved stars in the Galactic plane. TheQ1 andQ2 parameters

Messineo

Menten

Churchwell

et al. 2011

A&A

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Context. Mass-loss from evolved stars chemically enriches the interstellar medium (ISM). Stellar winds from massive stars and their explosions as supernovae shape the ISM and trigger star formation. Studying evolved stars is fundamental for understanding galaxy formation and evolution at any redshift. Aims. We aim to establish a photometric classification scheme for Galactic mass-losing evolved stars (e.g., WR, RSG, and AGB stars) with the goal of identifying new ones, and subsequently to use these samples as tracers of Galactic structure. Methods. We searched for counterparts of known Galactic WR, LBV, RSG, and O-rich AGB stars in the 2MASS, GLIMPSE, and MSX catalogs, and we analyzed their properties with near-and mid-infrared color-color diagrams. Results. We used the Q1 parameter, which is a measure of the deviation from the interstellar reddening vector in the J − H versus H−K s diagram, and we defined a new parameter, Q2, which is a measure of the deviation from the interstellar reddening vector in the Conclusions. The GLIMPSE catalog is a powerful tool for photometric classification of Galactic mass-losing evolved stars. Our new criteria will yield many new RSGs and WRs.

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On the population of galactic Luminous Blue Variables

Cited by 137 publications

References 41 publications

Probing the ejecta of evolved massive stars in transition

Probing the ejecta of evolved massive stars in transition

A systematic study of variability among OB-stars based on HIPPARCOS photometry

Near- and mid-infrared colors of evolved stars in the Galactic plane. TheQ1 andQ2 parameters

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