Analysis of the variability of the luminous emission line   star MWC 314

Muratorio, G.; Rossi, C.; Friedjung, M.

doi:10.1051/0004-6361:20078940

Cited by 13 publications

(30 citation statements)

References 12 publications

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“…As already described in Muratorio et al (2008), forbidden lines are narrower than permitted lines: a mean FWHM of 55 ± 8 km s −1 is found from a single Gaussian fitting. The RV curve reproduces the behavior of the permitted (and therefore of the absorption) lines though with quite a large scatter, likely the result of the small number of lines and their faintness (see Fig.…”

Section: Forbidden Emission Linessupporting

confidence: 64%

“…A detailed logbook of these observations and the data reduction procedures are described in Muratorio et al (2008).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…However, it does not show the typical brightness variations of the latter class. The profiles of the permitted emission lines show two peaks, which suggests their formation in a rotating disk, and which led us to consider MWC 314 as a B [e] supergiant rather than an LBV (Muratorio et al 2008). Marston & McCollum (2008) detected a very large bipolar nebula that emits in Hα and extends for ∼13.5 pc.…”

Section: Introductionmentioning

confidence: 99%

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Interpreting the spectral behavior of MWC 314

Frasca

Мирошниченко

Rossi

et al. 2015

A&A

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Context. MWC 314 is one of the most luminous stars in the Milky Way. Its fundamental parameters are similar to those of luminous blue variables (LBVs), although no large photometric variations have been recorded. Moreover, it shows no evidence of either a dust shell or a relevant spectral variability. Aims. The main purpose of this work is to clarify the origin of the radial velocity and line profile variations exhibited by absorption and emission lines. Methods. We analyzed the radial velocity (RV) variations displayed by the absorption lines from the star's atmosphere using highresolution optical spectra and fitting the RV curve with an eccentric orbit model. We also studied the RV and profile variations of some permitted and forbidden emission lines of metallic ions with a simple geometric model. The behavior of the Balmer and He i lines has also been investigated. Results. Fourier analysis applied to the RV of the absorption lines clearly shows a 60-day periodicity. A dense coverage of the RV curve allowed us to derive accurate orbital parameters. The RV of the Fe ii emission lines varies in the same way, but with a smaller amplitude. Additionally, the intensity ratio of the blue/red peaks of these emission lines correlates with the RV variations. The first three members of the Balmer series as well as [N ii] lines display a nearly constant RV and no profile variations in phase with the orbital motion instead. The He i λ5876 Å line shows a strongly variable profile with broad and blue-shifted absorption components that reach velocities of ≤−1000 km s −1 in some specific orbital phases. Conclusions. Our data and analysis provide strong evidence that the object is a binary system composed of a supergiant B[e] star and an undetected companion. The emission lines with a non-variable RV could originate in a circumbinary region. For the Fe ii emission lines, we propose a simple geometrical two-component model where a compact source of Fe ii emission, moving around the center of mass, is affected by a static extra absorption that originates from a larger area. Finally, the blue-shifted absorption in the He i λ5876 Å line could be the result of density enhancements in the primary star wind that is flowing towards the companion, and which is best observed when projected over the disk of the primary star.

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Section: Forbidden Emission Linessupporting

confidence: 64%

“…A detailed logbook of these observations and the data reduction procedures are described in Muratorio et al (2008).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Interpreting the spectral behavior of MWC 314

Frasca

Мирошниченко

Rossi

et al. 2015

A&A

Self Cite

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“…In addition, it appears to be one of the most luminous stars in the Galaxy (Miroshnichenko et al 1998). Permitted emission line profiles show two peaks, suggesting formation in a rotating disk and we considered it to belong rather to the B[e] class (Muratorio et al 2008). Rapid variations in the displacements of the absorption lines, previouly suggested by Wisniewski et al (2006), could indicate binarity (Muratorio et al 2008) with a period of ∼ 31 days.…”

Section: Introductionmentioning

confidence: 97%

“…Permitted emission line profiles show two peaks, suggesting formation in a rotating disk and we considered it to belong rather to the B[e] class (Muratorio et al 2008). Rapid variations in the displacements of the absorption lines, previouly suggested by Wisniewski et al (2006), could indicate binarity (Muratorio et al 2008) with a period of ∼ 31 days. In order to confirm the suggested periodicity, we obtained additional spectra at the Catania Observatory (OAC) during 2008 and 2009 in the range 4300-6850Å with resolution R 21 000.…”

Section: Introductionmentioning

confidence: 99%

The spectral variations of MWC 314

et al. 2010

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Long-term spectroscopic monitoring of LBVs and LBV candidates

et al. 2010

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Abstract. We present results of a long-term spectroscopic monitoring program (since mid 2009) of Luminous Blue Variables with the new HERMES echelle spectrograph on the 1.2m Mercator telescope at La Palma (Spain). We investigate high-resolution (R = 80,000) optical spectra of two LBVs, P Cyg and HD 168607, the LBV candidates MWC 930 and HD 168625, and the LBV binary MWC 314. In P Cyg we observe flux changes in the violet wings of the Balmer Hα, Hβ, and He i lines between May and Sep 2009. The changes around 200 to 300 km s −1 are caused by variable opacity at the base of the supersonic wind from the blue supergiant.We observe in MWC 314 broad double-peaked metal emission lines with invariable radial velocities over time. On the other hand, we measure in the photospheric S ii λ5647 absorption line, with lower excitation energy of ∼14 eV, an increase of the heliocentric radial velocity centroid from 37 km s

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Analysis of the variability of the luminous emission line star MWC 314

Cited by 13 publications

References 12 publications

Interpreting the spectral behavior of MWC 314

Interpreting the spectral behavior of MWC 314

The spectral variations of MWC 314

Long-term spectroscopic monitoring of LBVs and LBV candidates

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