Evolution of red Nova V4332 Sagittarii remnant

Barsukova, E. A.; Goranskij, V. P.; Valeev, A. F.; Zharova, A. V.

doi:10.1134/s1990341314010076

Cited by 20 publications

(30 citation statements)

References 32 publications

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“…The conditions in the latter case differ from those in the ejected material. We aso note that direct observations show the existence of a significant amount of dust shrouding/obscuring post CE/merger objects (Kamiński et al 2010;Kamiński & Tylenda 2011;Tylenda et al 2011;Barsukova et al 2014;Tylenda et al 2015). The radiation from the inner parts of the star applies radiation pressure on the dust, accelerating it above the sound speed of the gas, and the collisional coupling of the dust to the gas can eventually result in the ejection of the entire outer layer of the envelope.…”

Section: Dust-assisted Common-envelope Ejectionmentioning

confidence: 83%

“…In the dust-driven CE ejection the CE is not dynamically ejected as typically envisioned, but rather the dynamical phase introduces the conditions allowing for the long-term slow mass-loss phase. We point out that even during the dynamical phase of the inspiral, dust may form and thereby affect the appearance of the light curve ans spectra of the transient CEE event and the remnant post-CE binary, and should be accounted for (see also Kamiński et al 2010;Kamiński & Tylenda 2011;Tylenda et al 2011;Barsukova et al 2014;Tylenda et al 2015;Galaviz et al 2017, for observational evidence and theoretical discussion of the dust effects on the post-CE appearance) .…”

Section: Discussion and Summarymentioning

confidence: 99%

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Efficient common-envelope ejection through dust-driven winds

Glanz

Perets

2018

Monthly Notices of the Royal Astronomical Society: Letters

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Common-envelope evolution (CEE) is the short-lived phase in the life of an interacting binary-system during which two stars orbit inside a single shared envelope. Such evolution is thought to lead to the inspiral of the binary, the ejection of the extended envelope and the formation of a remnant short-period binary. However, detailed hydrodynamical models of CEE encounter major difficulties. They show that following the inspiral most of the envelope is not ejected; though it expands to larger separations, it remains bound to the binary. Here we propose that dust-driven winds can be produced following the CEE. These can evaporate the envelope following similar processes operating in the ejection of the envelopes of AGB stars. Pulsations in an AGB-star drives the expansion of its envelope, allowing the material to cool down to low temperatures thus enabling dust condensation. Radiation pressure on the dust accelerates it, and through its coupling to the gas it drives winds which eventually completely erode the envelope. We show that the inspiral phase in CE-binaries can effectively replace the role of stellar pulsation and drive the CE expansion to scales comparable with those of AGB stars, and give rise to efficient mass-loss through dust-driven winds.

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Section: Dust-assisted Common-envelope Ejectionmentioning

confidence: 83%

Section: Discussion and Summarymentioning

confidence: 99%

Efficient common-envelope ejection through dust-driven winds

Glanz

Perets

2018

Monthly Notices of the Royal Astronomical Society: Letters

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“…We note that RNe usually experience a metamorphosis from a bluer spectral type at the epoch of the light curve peak to an M-type at late phases, and all their spectra transition from being continuum-dominated to a configuration characterized by broad and strong molecular absorption features (see, e.g., V4332 Sgr, Martini et al 1999). Barsukova et al (2014) suggested that the spectrum of V4332 Sgr observed over a decade after the outburst, showing simultaneously a late M-type continuum, molecular bands and emission features of metals, was due the contribution of a third, red companion that was dynamically destroying the expanding envelope produced in the merging event.…”

Section: Detection Of Molecules and Dust Formationmentioning

confidence: 99%

Luminous red novae: Stellar mergers or giant eruptions?

Pastorello

Mason

Taubenberger

et al. 2019

A&A

108

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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“…This would also generate a cool dense shell, which is an ideal site for late dust formation, as likely observed in AT 2017jfs. Barsukova et al (2014) provided a somewhat different interpretation. The rapid coalescence generates a violent forward shock which leads the photospheric temperature to largely increase, producing the blue light curve peak.…”

Section: Evolution Of the Temperature And The Radiusmentioning

confidence: 99%

“…The spectra of the comparison objects are taken fromPastorello et al (2019),Blagorodnova et al (2017), andKankare et al (2015). The identification of the molecular bands is performed followingKirkpatrick et al (1991),Valenti et al (1998),Martini et al (1999), andBarsukova et al (2014).…”

mentioning

confidence: 99%

The evolution of luminous red nova AT 2017jfs in NGC 4470

Pastorello

Chen

Cai

et al. 2019

A&A

Self Cite

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We present the results of our photometric and spectroscopic follow-up of the intermediate-luminosity optical transient AT 2017jfs. At peak, the object reaches an absolute magnitude of Mg = −15.46 ± 0.15 mag and a bolometric luminosity of 5.5 × 1041 erg s−1. Its light curve has the double-peak shape typical of luminous red novae (LRNe), with a narrow first peak bright in the blue bands, while the second peak is longer-lasting and more luminous in the red and near-infrared (NIR) bands. During the first peak, the spectrum shows a blue continuum with narrow emission lines of H and Fe II. During the second peak, the spectrum becomes cooler, resembling that of a K-type star, and the emission lines are replaced by a forest of narrow lines in absorption. About 5 months later, while the optical light curves are characterized by a fast linear decline, the NIR ones show a moderate rebrightening, observed until the transient disappears in solar conjunction. At these late epochs, the spectrum becomes reminiscent of that of M-type stars, with prominent molecular absorption bands. The late-time properties suggest the formation of some dust in the expanding common envelope or an IR echo from foreground pre-existing dust. We propose that the object is a common-envelope transient, possibly the outcome of a merging event in a massive binary, similar to NGC 4490−2011OT1.

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Evolution of red Nova V4332 Sagittarii remnant

Cited by 20 publications

References 32 publications

Efficient common-envelope ejection through dust-driven winds

Efficient common-envelope ejection through dust-driven winds

Luminous red novae: Stellar mergers or giant eruptions?

The evolution of luminous red nova AT 2017jfs in NGC 4470

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