Light-curve Model for Luminous Red Novae and Inferences about the Ejecta of Stellar Mergers

Matsumoto, Tatsuya; Metzger, Brian D.

doi:10.3847/1538-4357/ac6269

Cited by 22 publications

(16 citation statements)

References 117 publications

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“…The enormous difference between the inferred parameters for these three objects can be explained by a different fate of the system: while the large ejected mass of AT 2021blu can only result from the coalescence of massive stars, two different scenarios can be invoked to explain the low ejected mass of AT 2021afy: the massive primary merged with a very low-mass companion, or the system survived as a binary system. However, as remarked by Matsumoto & Metzger (2022), the ejected mass and the radius strongly depend on the adopted velocity, and the presence of an extra heating source (such as shock interaction with circumbinary material) may severely affect the above estimates. 25 If we account for the error in the luminosity at the second peak, L pk2 = 2.1(±0.6) × 10 41 erg s −1 , the upper limit to the total energy radiated by AT 2021afy in this phase ranges from 0.65 to 1.15 × 10 48 erg.…”

Section: The Merger Scenariomentioning

confidence: 96%

“…Matsumoto & Metzger ( 2022) recently presented accurate one-dimensional models of LRN light curves which improve on previous studies based on Popov (1993) approximations. The models of Matsumoto & Metzger (2022) assume that the shortlasting initial blue peak is due to thermal energy release from the low-mass, fast outer ejecta dominated by radiation pressure, while the second long-duration red peak emission is powered by hydrogen recombination. This study offers a grid of lightcurve models showing two luminosity peaks, remarkably similar to those observed for LRNe.…”

Section: The Merger Scenariomentioning

confidence: 99%

“…This study offers a grid of lightcurve models showing two luminosity peaks, remarkably similar to those observed for LRNe. Following Matsumoto & Metzger (2022), we can estimate the LRN parameters during the first peak. In particular, the ejected mass (M ej ) is inferred from…”

Section: The Merger Scenariomentioning

confidence: 99%

“…After the early peak, the light curve reaches a minimum before rising again to the second broad maximum, which is mostly powered by hydrogen recombination. We still follow Matsumoto & Metzger (2022) to describe the recombination phase. The mass of the recombining hydrogen shell (M rec ) is obtained through the relation (equivalent to Eq.…”

Section: The Merger Scenariomentioning

confidence: 99%

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Forbidden hugs in pandemic times

Pastorello

Valerin

Fraser

et al. 2023

A&A

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We present photometric and spectroscopic data on three extragalactic luminous red novae (LRNe): AT 2018bwo, AT 2021afy, and AT 2021blu. AT 2018bwo was discovered in NGC 45 (at about 6.8 Mpc) a few weeks after the outburst onset. During the monitoring period, the transient reached a peak luminosity of 1040 erg s−1. AT 2021afy, hosted by UGC 10043 (∼49.2 Mpc), showed a double-peaked light curve, with the two peaks reaching a similar luminosity of 2.1(±0.6)×1041 erg s−1. Finally, for AT 2021blu in UGC 5829 (∼8.6 Mpc), the pre-outburst phase was well-monitored by several photometric surveys, and the object showed a slow luminosity rise before the outburst. The light curve of AT 2021blu was sampled with an unprecedented cadence until the object disappeared behind the Sun, and it was then recovered at late phases. The light curve of LRN AT 2021blu shows a double peak, with a prominent early maximum reaching a luminosity of 6.5 × 1040 erg s−1, which is half of that of AT 2021afy. The spectra of AT 2021afy and AT 2021blu display the expected evolution for LRNe: a blue continuum dominated by prominent Balmer lines in emission during the first peak, and a redder continuum consistent with that of a K-type star with narrow absorption metal lines during the second, broad maximum. The spectra of AT 2018bwo are markedly different, with a very red continuum dominated by broad molecular features in absorption. As these spectra closely resemble those of LRNe after the second peak, AT 2018bwo was probably discovered at the very late evolutionary stages. This would explain its fast evolution and the spectral properties compatible with that of an M-type star. From the analysis of deep frames of the LRN sites years before the outburst, and considerations of the light curves, the quiescent progenitor systems of the three LRNe were likely massive, with primaries ranging from about 13 M⊙ for AT 2018bwo, to 14−1+4 M⊙ for AT 2021blu, and over 40 M⊙ for AT 2021afy.

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Section: The Merger Scenariomentioning

confidence: 96%

Section: The Merger Scenariomentioning

confidence: 99%

Section: The Merger Scenariomentioning

confidence: 99%

Section: The Merger Scenariomentioning

confidence: 99%

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Forbidden hugs in pandemic times

Pastorello

Valerin

Fraser

et al. 2023

A&A

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“…CE evolution (CEE) is vital in the formation of short-orbital-period binaries of one or two compact objects (Livio & Soker 1988;Taam & Sandquist 2000;Ivanova et al 2013). These systems cover a broad range of progenitor masses and types, such as merging black hole-black hole, black holeneutron star, and neutron star-neutron star binaries (e.g., Broekgaarden et al 2021;Olejak et al 2021;Shao & Li 2021;Gallegos-Garcia et al 2023;Iorio et al 2023), Type Ibn/Icn supernovae from merging Wolf-Rayet stars/black holes (Metzger 2022), Type IIb supernovae (Soker 2017), luminous red novae (e.g., Cai et al 2022;Matsumoto & Metzger 2022), Type Ia supernovae progenitors (e.g., Kashi & Soker 2011;Wang 2018), binary pulsars (e.g., Chen & Liu 2013;Liu et al 2018), X-ray binaries (e.g., Podsiadlowski & Rappaport 2000;Tauris et al 2000), double white dwarfs (WDs; e.g., Li et al 2023), cataclysmic variables (e.g., Webbink 1984), and planetary nebulae with binary nuclei (e.g., Livio & Soker 1988). For a comprehensive review, we refer the reader to Ivanova et al (2013), Röpke & De Marco (2023), or Tauris & van den Heuvel (2023).…”

Section: Introductionmentioning

confidence: 99%

The Common Envelope Evolution Outcome. II. Short-orbital-period Hot Subdwarf B Binaries Reveal a Clear Picture

Ge,

Tout,

Webbink

et al. 2024

ApJ

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Common envelope evolution (CEE) is vital for forming short-orbital-period compact binaries. It covers many objects, such as double compact merging binaries, Type Ia supernovae progenitors, binary pulsars, and X-ray binaries. Knowledge of the common envelope (CE) ejection efficiency still needs to be improved, though progress has been made recently. Short-orbital-period hot subdwarf B star (sdB) plus white dwarf (WD) binaries are the most straightforward samples with which to constrain CEE physics. We apply the known orbital period–WD mass relation to constrain the sdB progenitors of seven sdB+WD binaries with a known inclination angle. The average CE efficiency parameter is 0.32. This is consistent with previous studies. However, the CE efficiency need not be constant, but a function of the initial mass ratio, based on well-constrained sdB progenitor mass and evolutionary stage. Our results can be used as physical inputs for binary population synthesis simulations of related objects. A similar method can also be applied to study other short-orbital-period WD binaries.

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Simulations of common-envelope evolution in binary stellar systems: physical models and numerical techniques

Roepke

Marco

2023

Living Rev Comput Astrophys

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When the primary star in a close binary system evolves into a giant and engulfs its companion, its core and the companion temporarily orbit each other inside a common envelope. Drag forces transfer orbital energy and angular momentum to the envelope material. Depending on the efficiency of this process, the envelope may be ejected leaving behind a tight remnant binary system of two stellar cores, or the cores merge retaining part of the envelope material. The exact outcome of common-envelope evolution is critical for in the formation of X-ray binaries, supernova progenitors, the progenitors of compact-object mergers that emit detectable gravitational waves, and many other objects of fundamental astrophysical relevance. The wide ranges of spatial and temporal timescales that characterize common-envelope interactions and the lack of spatial symmetries present a substantial challenge to generating consistent models. Therefore, these critical phases are one of the largest sources for uncertainty in classical treatments of binary stellar evolution. Three-dimensional hydrodynamic simulations of at least part of the common-envelope interaction are the key to gain predictive power in modeling common-envelope evolution. We review the development of theoretical concepts and numerical approaches for such three-dimensional hydrodynamic simulations. The inherent multi-physics, multi-scale challenges have resulted in a wide variety of approximations and numerical techniques to be exercised on the problem. We summarize the simulations published to date and their main results. Given the recent rapid progress, a sound understanding of the physics of common-envelope interactions is within reach and thus there is hope that one of the remaining fundamental problems of stellar astrophysics may be solved before long.

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Light-curve Model for Luminous Red Novae and Inferences about the Ejecta of Stellar Mergers

Cited by 22 publications

References 117 publications

Forbidden hugs in pandemic times

Forbidden hugs in pandemic times

The Common Envelope Evolution Outcome. II. Short-orbital-period Hot Subdwarf B Binaries Reveal a Clear Picture

Simulations of common-envelope evolution in binary stellar systems: physical models and numerical techniques

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