Simulating Hydrogen-poor Interaction-powered Supernovae with CHIPS

Takei, Yuki; Tsuna, Daichi; Ko, Takatoshi; Shigeyama, Toshikazu

doi:10.3847/1538-4357/ad0da4

Cited by 3 publications

(1 citation statement)

References 126 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For Type Ibn/Icn SNe from helium (He)/Wolf-Rayet (W-R) stars, light-curve modeling of these SNe in general suggests a CSM mass of ∼0.01-1 M e (Dessart et al 2022;Maeda & Moriya 2022;Wu & Fuller 2022b;Takei et al 2024). For these stripped progenitors we expect a broad range of masses in their outer helium layers (∼0.1-2 M e for solar metallicity; e.g., Yoon 2017).…”

Section: ~´-mentioning

confidence: 99%

Bright Supernova Precursors by Outbursts from Massive Stars with Compact Object Companions

Tsuna,

Matsumoto,

et al. 2024

ApJ

Self Cite

View full text Add to dashboard Cite

A fraction of core-collapse supernovae (SNe) with signs of interaction with a dense circumstellar matter are preceded by bright precursor emission. While the precursors are likely caused by a mass ejection before core collapse, their mechanism to power energetic bursts—sometimes reaching 1048–1049 erg, which is larger than the binding energies of red supergiant envelopes—is still under debate. Remarkably, such a huge energy deposition should result in an almost complete envelope ejection and hence a strong sign of interaction, but the observed SNe with precursors show in fact typical properties among the interacting SNe. More generally, the observed luminosity of 1040−1042 erg s−1 is shown to be challenging for a single SN progenitor. To resolve these tensions, we propose a scenario where the progenitor is in a binary system with a compact object (CO) and an outburst from the star leads to a super-Eddington accretion onto the CO. We show that for sufficiently short separations outbursts with moderate initial kinetic energies of 1046–1047 erg can be energized by the accreting CO so that their radiative output can be consistent with the observed precursors. We discuss the implications of our model in relation to CO binaries detectable with Gaia and gravitational-wave detectors.

show abstract

Section: ~´-mentioning

confidence: 99%

Bright Supernova Precursors by Outbursts from Massive Stars with Compact Object Companions

Tsuna,

Matsumoto,

et al. 2024

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey

Toshikage,

Tanaka,

Yasuda

et al. 2024

ApJ

View full text Add to dashboard Cite

Recent high-cadence transient surveys have discovered rapid transients whose light-curve timescales are shorter than those of typical supernovae (SNe). In this paper, we present a systematic search for rapid transients at medium-high redshifts among 3381 SNe candidates obtained from the Hyper Suprime-Cam Subaru Strategic Program transient survey. We developed a machine learning classifier to classify the SN candidates into four types (Type Ia, Ibc, II SNe and rapid transients) based on the features derived from the light curves. By applying this classifier to the 3381 SN candidates and by further applying the quality cut, we selected 14 rapid transient samples. They are located at a wide range of redshifts (0.34 ≤ z ≤ 1.85) and show a wide range of the peak absolute magnitude (−17 ≥ M ≥ −22). The event rate of the rapid transients is estimated to be ∼6 × 103 events yr−1 Gpc−3 at z ∼ 0.74, which corresponds to about 2% of the event rate of normal core-collapse SNe at a similar redshift. Based on the luminosity and color evolution, we selected two candidates of Type Ibn SNe at z ∼ 0.75. The event rate of Type Ibn SN candidates is more than 1% of Type Ib SN rate at the same redshift, suggesting that this fraction of massive stars at this redshift range eruptively ejects their He-rich envelope just before the explosions. Also, two objects at z = 1.37 and 1.85 show high luminosities comparable to superluminous SNe. Their event rate is about 10%–25% of superluminous SNe at z ∼ 2.

show abstract

The X-Ray Luminous Type Ibn SN 2022ablq: Estimates of Preexplosion Mass Loss and Constraints on Precursor Emission

Pellegrino,

Modjaz,

Takei

et al. 2024

ApJ

View full text Add to dashboard Cite

Type Ibn supernovae (SNe Ibn) are rare stellar explosions powered primarily by interaction between the SN ejecta and H-poor, He-rich material lost by their progenitor stars. Multiwavelength observations, particularly in the X-rays, of SNe Ibn constrain their poorly understood progenitor channels and mass-loss mechanisms. Here we present Swift X-ray, ultraviolet, and ground-based optical observations of the Type Ibn SN 2022ablq, only the second SN Ibn with X-ray detections to date. While similar to the prototypical Type Ibn SN 2006jc in the optical, SN 2022ablq is roughly an order of magnitude more luminous in the X-rays, reaching unabsorbed luminosities L X ∼ 4 × 1040 erg s−1 between 0.2–10 keV. From these X-ray observations we infer time-varying mass-loss rates between 0.05 and 0.5 M ⊙ yr−1 peaking 0.5–2 yr before explosion. This complex mass-loss history and circumstellar environment disfavor steady-state winds as the primary progenitor mass-loss mechanism. We also search for precursor emission from alternative mass-loss mechanisms, such as eruptive outbursts, in forced photometry during the 2 yr before explosion. We find no statistically significant detections brighter than M ≈ −14—too shallow to rule out precursor events similar to those observed for other SNe Ibn. Finally, numerical models of the explosion of an ∼15 M ⊙ helium star that undergoes an eruptive outburst ≈1.8 yr before explosion are consistent with the observed bolometric light curve. We conclude that our observations disfavor a Wolf–Rayet star progenitor losing He-rich material via stellar winds and instead favor lower-mass progenitor models, including Roche-lobe overflow in helium stars with compact binary companions or stars that undergo eruptive outbursts during late-stage nucleosynthesis stages.

show abstract

Simulating Hydrogen-poor Interaction-powered Supernovae with CHIPS

Cited by 3 publications

References 126 publications

Bright Supernova Precursors by Outbursts from Massive Stars with Compact Object Companions

Bright Supernova Precursors by Outbursts from Massive Stars with Compact Object Companions

A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey

The X-Ray Luminous Type Ibn SN 2022ablq: Estimates of Preexplosion Mass Loss and Constraints on Precursor Emission

Contact Info

Product

Resources

About