Intermediate Luminosity Red Transients by Black Holes Born from Erupting Massive Stars

Tsuna, Daichi; Ishii, Ayako; Kuriyama, Naoto; Kashiyama, Kazumi; Shigeyama, Toshikazu

doi:10.48550/arxiv.2005.06103

Cited by 3 publications

(3 citation statements)

References 36 publications

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“…Such a fallback scenario has been proposed as a possible driver of activity from AT 2018cow (Margutti et al 2019). Additional power and/or diversity of properties can arise if ejected shells intract with a dense circumstellar medium (e.g., Tsuna et al 2020).…”

Section: Modelmentioning

confidence: 99%

Mass ejection in failed supernovae: equation of state and neutrino loss dependence

Ivanov,

Fernández

2021

Preprint

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A failed core-collapse supernova from a non-rotating progenitor can eject mass due to a weakening of gravity associated to neutrino emission by the protoneutron star. This mechanism yields observable transients and sets an upper limit to the mass of the black hole (BH) remnant. Previous global simulations of this mechanism have included neutrino losses parametrically, however, with direct implications for the ejecta mass and energy.Here we evolve the inner supernova core with a spherically-symmetric, general-relativistic neutrino radiationhydrodynamic code until BH formation. We then use the result in a Newtonian code that follows the response of the outer layers of the star to the change in gravity and resolves the surface pressure scale height. We find that the dense-matter equation of state (EOS) can introduce a factor ∼ 2 variation in gravitational mass lost to neutrinos, with a stiff EOS matching previous parametric results, and a soft EOS yielding lower ejecta masses and energies by a factor of several. This difference is caused primarily by the longer time to BH formation in stiffer EOSs. With a soft EOS, our red and yellow supergiant progenitors fail to unbind mass if hydrogen recombination energy is not included. Using a linear ramp in time for mass-energy lost to neutrinos (with suitable parameters) yields a stellar response within ∼ 10% of that obtained using the detailed history of neutrino losses. Our results imply quantitative but not qualitative modifications to previous predictions for shock breakout, plateau emission, and final BH masses from these events.

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Section: Modelmentioning

confidence: 99%

Mass ejection in failed supernovae: equation of state and neutrino loss dependence

Ivanov,

Fernández

2021

Preprint

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“…As Pursiainen et al (2018) suggest, this wide variety in the peak luminosity may indicate that observed FBOTs are actually composed of multiple populations. For example, such an extremely less energetic explosion may be realized in a failed supernova with small mass ejection (Nadezhin 1980;Lovegrove & Woosley 2013;Kashiyama & Quataert 2015;Fernández et al 2018;Tsuna et al 2020). Some FBOTs are highly luminous and short-lived.…”

Section: Fbotsmentioning

confidence: 99%

A systematic study on the rise time-peak luminosity relation for bright optical transients powered by wind shock breakout

Suzuki,

Moriya,

Takiwaki

2020

Preprint

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A number of astrophyical transients originating from stellar explosions are powered by the collision of the ejected material with the circumstellar medium, which efficiently produces thermal radiation via shock dissipation. We investigate how such interaction-powered transients are distributed in the peak bolometric luminosity vs the rise time phase space. Taking the advantage of less time-consuming one-dimensional simulations with spherical symmetry, we calculated more than 500 models with different circumstellar mass and radius, ejecta mass and energy, and chemical compositions. The peak bolometric luminosity, the total radiated energy, and the rise time of the interaction-powered emission are measured for each simulated light curve. We consider how these characteristic quantities are determined as a function of the model parameters and discuss possible implications for the observed populations of (potential) interaction-powered transients, such as type IIn supernovae and fast blue optical transients.

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“…Broken lines (Solid lines) correspond to the CSM erupted by the first injection (second injection). Grey line represents the relation ρ ∝ v −1.5 which we adopt as a fiducial slope in case of the eruptive mass lossTsuna et al 2020).…”

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confidence: 99%

Comparison between the first and second mass eruptions from progenitors of Type IIn supernovae

Kuriyama

Shigeyama

2021

A&A

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Context. Some massive stars experience episodic and intense mass loss phases with fluctuations in the luminosity. Ejected material forms circumstellar matter around the star, and the subsequent core collapse results in a Type IIn supernova that is characterized by interaction between supernova ejecta and circumstellar matter. The energy source that triggers these mass eruptions and dynamics of the outflow have not been clearly explained. Moreover, the mass eruption itself can alter the density structure of the envelope and affect the dynamics of the subsequent mass eruption if these events are repeated. A large amount of observational evidence suggests multiple mass eruptions prior to core collapse. Aims. We investigate the density structure of the envelope altered by the first mass eruption and the nature of the subsequent second mass eruption event in comparison with the first event. Methods. We deposited extra energy at the bottom of the hydrogen envelope of 15 M⊙ stars twice and calculated the time evolution by radiation hydrodynamical simulation code. We did not deal with the origin of the energy source, but focused on the dynamics of repeated mass eruptions from a single massive star. Results. There are significant differences between the first and second mass eruptions in terms of the luminosity, color, and amount of produced circumstellar matter. The second eruption leads to a redder burst event in which the associated brightening phase lasts longer than the first. The amount of ejected matter is different even with the same deposited energy in the first and second event, but the difference depends on the density structure of the star. Conclusions. Upcoming high cadence and deep transient surveys will provide us a lot of pre-supernova activities, and some of which might show multi-peaked light curves. These should be interpreted taking the effect of density structure altered by the preceding outburst events into consideration.

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Intermediate Luminosity Red Transients by Black Holes Born from Erupting Massive Stars

Cited by 3 publications

References 36 publications

Mass ejection in failed supernovae: equation of state and neutrino loss dependence

Mass ejection in failed supernovae: equation of state and neutrino loss dependence

A systematic study on the rise time-peak luminosity relation for bright optical transients powered by wind shock breakout

Comparison between the first and second mass eruptions from progenitors of Type IIn supernovae

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