Active Luminous Blue Variables in the Large Magellanic Cloud

Walborn, N. R.; Gamen, R.; Morrell, N.; Barbá, R. H.; Lajús, E. Fernández; Angeloni, R.

doi:10.3847/1538-3881/aa6195

Cited by 24 publications

(44 citation statements)

References 47 publications

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“…The F-type stellar classifications prior to 1990 may be observations of HD 269929 and the O-star classification in the early 1980s may also belong to observations of another star. However, the documented spectroscopic variations in Walborn et al (2017) and the massive nebula (this work) both support an LBV classification. Given the star's relatively low luminosity for an LBV, small spectroscopic variabilities would be expected following the amplitude-luminosity relation of S Doradus variables (Wolf 1989 is used since smaller aperture contain many outliers due to background subtraction issues.…”

Section: The Lbv Status Of Rmc 143 and Its Circumstellar Nebulasupporting

confidence: 63%

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A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA

Agliozzo

Mehner

Phillips

et al. 2019

A&A

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The luminous blue variable (LBV) RMC 143 is located in the outskirts of the 30 Doradus complex, a region rich with interstellar material and hot luminous stars. We report the 3σ sub-millimetre detection of its circumstellar nebula with ALMA. The observed morphology in the sub-millimetre is different than previously observed with HST and ATCA in the optical and centimetre wavelength regimes. The spectral energy distribution (SED) of RMC 143 suggests that two emission mechanisms contribute to the sub-mm emission: optically thin bremsstrahlung and dust. Both the extinction map and the SED are consistent with a dusty massive nebula with a dust mass of 0.055 ± 0.018 M ⊙ (assuming κ 850 = 1.7 cm 2 g −1 ). To date, RMC 143 has the most dusty LBV nebula observed in the Magellanic Clouds. We have also re-examined the LBV classification of RMC 143 based on VLT/X-shooter spectra obtained in 2015/16 and a review of the publication record. The radiative transfer code CMFGEN is used to derive its fundamental stellar parameters. We find an effective temperature of ∼ 8500 K, luminosity of log(L/L ⊙ ) = 5.32, and a relatively high mass-loss rate of 1.0 × 10 −5 M ⊙ yr −1 . The luminosity is much lower than previously thought, which implies that the current stellar mass of ∼ 8 M ⊙ is comparable to its nebular mass of ∼ 5.5 M ⊙ (from an assumed gas-to-dust ratio of 100), suggesting that the star has lost a large fraction of its initial mass in past LBV eruptions or binary interactions. While the star may have been hotter in the past, it is currently not hot enough to ionize its circumstellar nebula. We propose that the nebula is ionized externally by the hot stars in the 30 Doradus star-forming region.

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Section: The Lbv Status Of Rmc 143 and Its Circumstellar Nebulasupporting

confidence: 63%

“…5. Walborn et al (2017) report spectroscopic changes between the spectral types A and late-B in the time span from 1998 to 2016. 6.…”

Section: The Lbv Status Of Rmc 143 and Its Circumstellar Nebulamentioning

confidence: 99%

A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA

Agliozzo

Mehner

Phillips

et al. 2019

A&A

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“…In both objects, an indicative v FWH M ∼ 700 km s −1 is estimated for Hα. We also note that none of these objects show the [Ca II] doublet emission which usually characterizes other types of gap transients, including the intermediate-luminosity red transients (ILRTs, Botticella et al 2009;Kasliwal et al 2011) and S Dor-type LBV outbursts (e.g., Walborn et al 2017, and references therein).…”

Section: Spectroscopic Evolution Of Individual Objectsmentioning

confidence: 85%

Luminous red novae: Stellar mergers or giant eruptions?

Pastorello

Mason

Taubenberger

et al. 2019

A&A

104

125

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We present extensive datasets for a class of intermediate-luminosity optical transients known as "luminous red novae" (LRNe). They show doublepeaked light curves, with an initial rapid luminosity rise to a blue peak (at −13 to −15 mag), which is followed by a longer-duration red peak that sometimes is attenuated, resembling a plateau. The progenitors of three of them (NGC4490-2011OT1, M101-2015OT1, and SNhunt248), likely relatively massive blue to yellow stars, were also observed in a pre-eruptive stage when their luminosity was slowly increasing. Early spectra obtained during the first peak show a blue continuum with superposed prominent narrow Balmer lines, with P Cygni profiles. Lines of Fe II are also clearly observed, mostly in emission. During the second peak, the spectral continuum becomes much redder, Hα is barely detected, and a forest of narrow metal lines is observed in absorption. Very late-time spectra (∼6 months after blue peak) show an extremely red spectral continuum, peaking in the infrared (IR) domain. Hα is detected in pure emission at such late phases, along with broad absorption bands due to molecular overtones (such as TiO, VO). We discuss a few alternative scenarios for LRNe. Although major instabilities of single massive stars cannot be definitely ruled out, we favour a common envelope ejection in a close binary system, with possibly a final coalescence of the two stars. The similarity between LRNe and the outburst observed a few months before the explosion of the Type IIn SN 2011ht is also discussed.

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“…8 9 of 24 HD 5980 [39] convincingly shows a hotter spectrum in the minimum of brightness. Other LBV stars showing WN-like spectrum in quiescent "hot" phase usually stop at colder spectral types such as WN11 (for example AG Car [40] and WS 1 [41,42]) or Ofpe/WN9 (for example R 127 [43] and HD 269582 [44]).…”

Section: Spectroscopy and Determination Of Physical Parametersmentioning

confidence: 99%

The History Goes On: Century Long Study of Romano’s Star

et al. 2019

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GR 290 (M 33 V0532 = Romano’s Star) is a unique variable star in the M33 galaxy, which simultaneously displays variability typical for luminous blue variable (LBV) stars and physical parameters typical for nitrogen-rich Wolf-Rayet (WR) stars (WN). As of now, GR 290 is the first object which is confidently classified as a post-LBV star. In this paper, we outline the main results achieved from extensive photometric and spectroscopic observations of the star: the structure and chemical composition of its wind and its evolution over time, the systematic increase of the bolometric luminosity during the light maxima, the circumstellar environment. These results show that the current state of Romano’s Star constitutes a fundamental link in the evolutionary path of very massive stars.

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Active Luminous Blue Variables in the Large Magellanic Cloud

Cited by 24 publications

References 47 publications

A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA

A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA

Luminous red novae: Stellar mergers or giant eruptions?

The History Goes On: Century Long Study of Romano’s Star

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