A long life of excess: The interacting transient SN 2017hcc

Moran, S.; Fraser, M.; Kotak, R.; Pastorello, A.; Benetti, S.; Brennan, S.; Gutiérrez, C. P.; Kankare, E.; Kuncarayakti, H.; Mattila, S.; Reynolds, T.; Anderson, J. P.; Brown, P. J.; Campana, S.; Chambers, K.; Chen, T.-W.; Valle, M. Della; Dennefeld, M.; Elias‐Rosa, N.; Galbany, L.; Galindo-Guil, F. J.; Gromadzki, M.; Hiramatsu, D.; Inserra, C.; Leloudas, G.; Müller-Bravo, T. E.; Nicholl, M.; Reguitti, A.; Shahbandeh, Melissa; Smartt, S. J.; Tartaglia, L.; Young, D. R.

doi:10.1051/0004-6361/202244565

Cited by 6 publications

(1 citation statement)

References 82 publications

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“…The alternative is that increased CSM interaction is producing extra blue flux. This is often seen in Type IIn SNe with strong interaction where a forest of Fe emission lines emerge and creates a blue pseudocontinuum (Smith et al 2009;Moran et al 2023). For other Type II SNe, though, weaker CSM interaction can manifest as an overall shift to bluer emission (Dessart et al 2023), although this generally happens much later in the evolution.…”

Section: Color Evolutionmentioning

confidence: 99%

SN 2022jox: An Extraordinarily Ordinary Type II SN with Flash Spectroscopy

Andrews,

Pearson,

Hosseinzadeh

et al. 2024

ApJ

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We present high-cadence optical and ultraviolet (UV) observations of the Type II supernova (SN), SN 2022jox which exhibits early spectroscopic high-ionization flash features of H i, He ii, C iv, and N iv that disappear within the first few days after explosion. SN 2022jox was discovered by the Distance Less Than 40 Mpc survey ∼0.75 day after explosion with follow-up spectra and UV photometry obtained within minutes of discovery. The SN reached a peak brightness of M V ∼ −17.3 mag, and has an estimated 56Ni mass of 0.04 M ⊙, typical values for normal Type II SNe. The modeling of the early light curve and the strong flash signatures present in the optical spectra indicate interaction with circumstellar material (CSM) created from a progenitor with a mass-loss rate of M ̇ ∼ 10 − 3 – 10 − 2 M ⊙ y r − 1 . There may also be some indication of late-time CSM interaction in the form of an emission line blueward of Hα seen in spectra around 200 days. The mass-loss rate of SN 2022jox is much higher than the values typically associated with quiescent mass loss from red supergiants, the known progenitors of Type II SNe, but is comparable to inferred values from similar core-collapse SNe with flash features, suggesting an eruptive event or a superwind in the progenitor in the months or years before explosion.

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Section: Color Evolutionmentioning

confidence: 99%

SN 2022jox: An Extraordinarily Ordinary Type II SN with Flash Spectroscopy

Andrews,

Pearson,

Hosseinzadeh

et al. 2024

ApJ

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Environmental dependence of Type IIn supernova properties

Moriya¹,

Galbany²,

Jimenez-Palau³

et al. 2023

A&A

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Type IIn supernovae occur when stellar explosions are surrounded by dense hydrogen-rich circumstellar matter. The dense circumstellar matter is likely formed by extreme mass loss from their progenitors shortly before they explode. The nature of Type IIn supernova progenitors and the mass-loss mechanism forming the dense circumstellar matter are still unknown. In this work, we investigate whether Type IIn supernova properties and their local environments are correlated. We use Type IIn supernovae with well-observed light curves and host-galaxy integral field spectroscopic data so that we can estimate both supernova and environmental properties. We find that Type IIn supernovae with a higher peak luminosity tend to occur in environments with lower metallicity and/or younger stellar populations. The circumstellar matter density around Type IIn supernovae is not significantly correlated with metallicity, so the mass-loss mechanism forming the dense circumstellar matter around Type IIn supernovae might be insensitive to metallicity.

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Interacting supernovae from wide massive binary systems

Ercolino,

Jin,

Langer

et al. 2024

A&A

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The features in the light curves and spectra of many I and II supernovae (SNe) can be understood by assuming an interaction of the SN ejecta with circumstellar matter (CSM) surrounding the progenitor star. This suggests that many massive stars may undergo various degrees of envelope stripping shortly before exploding, and may therefore produce a considerable diversity in their pre-explosion CSM properties. We explore a generic set of about 100 detailed massive binary evolution models in order to characterize the amount of envelope stripping and the expected CSM configurations. Our binary models were computed with the MESA stellar evolution code, considering an initial primary star mass of 12.6mso and secondaries with initial masses of between $ and $ and focus on initial orbital periods above $ We compute these models up to the time of iron core collapse in the primary. Our models exhibit varying degrees of stripping due to mass transfer, resulting in SN progenitor models ranging from fully stripped helium stars to stars that have not been stripped at all. We find that Roche lobe overflow often leads to incomplete stripping of the mass donor, resulting in a large variety of pre-SN envelope masses. In many of our models, the red supergiant (RSG) donor stars undergo core collapse during Roche lobe overflow, with mass transfer and therefore system mass-loss rates of up to $0.01 at that time. The corresponding CSM densities are similar to those inferred for IIn SNe, such as 1998S . In other cases, the mass transfer becomes unstable, leading to a common-envelope phase at such late time that the mass donor explodes before the common envelope is fully ejected or the system has merged. We argue that this may cause significant pre-SN variability, as witnessed for example in 2020tlf . Other models suggest a common-envelope ejection just centuries before core collapse, which may lead to the strongest interactions, as observed in superluminous IIn SNe, such as 1994W and 2006gy Wide massive binaries exhibit properties that may not only explain the diverse envelope stripping inferred in Type Ib, IIb, IIL, and IIP SNe, but also offer a natural framework to understand a broad range of hydrogen-rich interacting SNe. On the other hand, the flash features observed in many IIP SNe, such as 2013fs may indicate that RSG atmospheres are more extended than currently assumed; this could enhance the parameter space for wide binary interaction.

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A long life of excess: The interacting transient SN 2017hcc

Cited by 6 publications

References 82 publications

SN 2022jox: An Extraordinarily Ordinary Type II SN with Flash Spectroscopy

SN 2022jox: An Extraordinarily Ordinary Type II SN with Flash Spectroscopy

Environmental dependence of Type IIn supernova properties

Interacting supernovae from wide massive binary systems

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