Properties of Galactic B[e] Supergiants. V. 3 Pup–Constraining the Orbital Parameters and Modeling the Circumstellar Environments

Мирошниченко, А. С.; Danford, S.; Zharikov, S. V.; Клочкова, В. Г.; Ченцов, Е. Л.; Vanbeveren, D.; Zakhozhay, O. V.; Manset, N.; Погодин, М. А.; Omarov, Ch. Т.; Kuratova, A. K.; Khokhlov, S. A.

doi:10.3847/1538-4357/ab93d9

Cited by 13 publications

(10 citation statements)

References 34 publications

(55 reference statements)

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“…Preliminary parameters of the latter binary, which shows absorption lines from the cool component and emission lines from the hot one, found in [46] with eight spectra were refined by doubling the number of them. The orbital period of the brightest object with the B[e] phenomenon, 3 Pup, derived for the first time nearly 70 years ago [48] was confirmed in [21] with over 100 spectra taken at the 0.81 m TCO telescope. This large number of new observations allowed the determination of the RV amplitude for the first time and thus constrained the properties of the secondary component.…”

Section: Resultsmentioning

confidence: 79%

Recent Progress in Finding Binary Systems with the B[e] Phenomenon

et al. 2023

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This paper describes recent studies of the FS CMa-type objects, a group of stars showing the B[e] phenomenon defined in 2007. The objects exhibit strong emission-line spectra with both permitted and forbidden lines suggesting the presence of a B-type star as well as strong IR excesses due to radiation of circumstellar dust. These properties are hard to explain in the framework of the evolution of single stars with luminosities between ~300 and ~30,000 L⊙ typical of most B-type stars. We explore the hypothesis that the gaseous-and-dusty envelopes of FS CMa objects are due to either earlier or ongoing mass transfer between the binary system components. It is hard to detect the secondary components in these systems because of veiling and distortions by the circumstellar matter because of the relative faintness of the companions. Nevertheless, we detected regular radial velocity variations of the spectral lines in MWC 728, 3 Pup, and AS 386 and we found absorption lines typical of cool stars in the spectra of MWC 645, AS 174, and several other objects. The diversity of the secondary components in FS CMa objects is discussed in the context of non-conservative binary evolution.

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Section: Resultsmentioning

confidence: 79%

Recent Progress in Finding Binary Systems with the B[e] Phenomenon

et al. 2023

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“…MWC 645 is the first FS CMa group member with a seemingly ongoing mass transfer, while binaries found earlier most likely have finished the mass-transfer process (e.g., Miroshnichenko et al 2015;Khokhlov et al 2018;Miroshnichenko et al 2020). A closer study that includes higher signalto-noise, high-resolution spectroscopy at large telescopes and multicolor photometric monitoring would allow determination of more properties of the system, such as the orbital period and inclination, as well as those of its circumstellar envelope.…”

Section: Discussionmentioning

confidence: 99%

Toward Understanding the B[e] Phenomenon. IX. Nature and Binarity of MWC645

Nodyarov

Мирошниченко

Khokhlov

et al. 2022

ApJ

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We present the results of optical and near-IR spectroscopy and multicolor photometry of the emission-line star MWC 645, which exhibits the B[e] phenomenon. The presence of positionally variable absorption lines of a cool star detected for the first time indicates that the object is a binary system. Using a combination of the photometric and spectroscopic data as well as the Gaia EDR3 distance (D = 6.5 ± 0.9 kpc), we disentangled the components’ contributions and estimated their surface temperatures and luminosities (18, 000 ± 2000 K and 4250 ± 250 K, log L/L ⊙ = 4.0 ± 0.5 and 3.1 ± 0.3 for the hot and cool components, respectively). Quasi-cyclic short-period (months) and long-period (∼4 yr) photometric variations were detected in both optical and near-IR regions, and are most likely due to variable circumstellar extinction. Our analysis suggests that MWC 645 is a member of the FS CMa group. The object’s properties can be described by an evolutionary model of a close binary system that currently undergoes a nonconservative mass transfer between intermediate-mass stars (e.g., 7 M ⊙ + 2.8 M ⊙).

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“…For the stellar flux we took an ATLAS9 model atmosphere provided by F. Castelli 14 ([M/H] = 0.0, v turb = 2.0 km s −1 ) for T eff = 8500 K and log g = 2.0. We used the same disk-like model as in our previous studies of the emission-line objects IRAS 22150+6109 (Zakhozhay et al 2018) and 3 Pup (Miroshnichenko et al 2020). We note that one should consider it with caution, as there is no detailed information about the spatial distribution of the circumstellar dust in this system (e.g., IR and submillimetric images).…”

Section: Modeling Of the Spectral Energy Distributionmentioning

confidence: 99%

“…At the same time, only about a dozen binaries have been confirmed in the sample , which is mostly due to sparse observations and the complex nature of the objects. Although recent observing campaigns allowed us to prove binarity of some group members (e.g., Khokhlov et al 2018;Miroshnichenko et al 2020), binarity of some others still remains elusive (e.g., Khokhlov et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Toward Understanding the B[e] Phenomenon. VIII. Nature and Variability of IRAS 07080+0605

Khokhlov

Мирошниченко

Zharikov

et al. 2022

ApJ

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We report the results of spectroscopic and photometric observations of the emission-line object IRAS 07080+0605 carried out in 2004–2021. We found that the object is significantly underluminous for its spectroscopic properties (T eff = 8500 ± 500 K, log g = 2.0 ± 0.5), if a strong visual attenuation by a factor of ∼43 found through the spectral energy distribution modeling is not taken into account. Visual brightness variations with a stable period of 190 days but a variable amplitude of ∼0.2 mag were found in the ASAS SN data and attributed to variable circumstellar extinction in the dusty disk. We also found that the observed behavior of IRAS 07080+0605 is similar to that of the protoplanetary nebula Red Rectangle. The dusty disk of IRAS 07080+0605 shows the presence of carbonaceous particles (∼10%–20% of the total dust content) and polycyclic aromatic hydrocarbon emission bands. However, IRAS 07080+0605 shows no obvious signs of the refractory element depletion, which is common in post–asymptotic giant branch (AGB) dusty binaries, or of a visual nebula. Absorption-line positions vary with an amplitude of ∼25 km s−1, suggesting the presence of a secondary component. Spectroscopic monitoring on a timescale from days to months is needed to search for regular variations. We conclude that IRAS 07080+0605 is most likely a binary system with an A-type component on its way toward the post-AGB evolutionary stage, as binarity is capable of explaining most of the observed features.

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Properties of Galactic B[e] Supergiants. V. 3 Pup–Constraining the Orbital Parameters and Modeling the Circumstellar Environments

Abstract: with details of the nature of the infringement. We will investigate the claim and if justified, we will take the appropriate steps.

Cited by 13 publications

References 34 publications

Recent Progress in Finding Binary Systems with the B[e] Phenomenon

Recent Progress in Finding Binary Systems with the B[e] Phenomenon

Toward Understanding the B[e] Phenomenon. IX. Nature and Binarity of MWC645

Toward Understanding the B[e] Phenomenon. VIII. Nature and Variability of IRAS 07080+0605

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