A 12.4-day periodicity in a close binary system after a supernova

Chen, Ping; Gal-Yam, Avishay; Sollerman, Jesper; Schulze, Steve; Post, Richard S.; Liu, Chang; Ofek, Eran O.; Das, Kaustav K.; Fremling, Christoffer; Horesh, Assaf; Katz, Boaz; Kushnir, Doron; Kasliwal, Mansi M.; Kulkarni, Shri R.; Liu, Dezi; Liu, Xiangkun; Miller, Adam A.; Rose, Kovi; Waxman, Eli; Yang, Sheng; Yao, Yuhan; Zackay, Barak; Bellm, Eric C.; Dekany, Richard; Drake, Andrew J.; Fang, Yuan; Fynbo, Johan P. U.; Groom, Steven L.; Helou, George; Irani, Ido; Jegou du Laz, Theophile; Liu, Xiaowei; Mazzali, Paolo A.; Neill, James D.; Qin, Yu-Jing; Riddle, Reed L.; Sharon, Amir; Strotjohann, Nora L.; Wold, Avery; Yan, Lin

doi:10.1038/s41586-023-06787-x

Cited by 14 publications

(6 citation statements)

References 167 publications

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“…The effect of companions on SN lightcurves has already been discussed in the literature (e.g., Gao et al 2020;Soker 2020;Hirai & Podsiadlowski 2022;Wen et al 2023) and has been observed in SN 2022jli (Moore et al 2023;Chen et al 2024), identified as a normal Type Ic SN. In this Letter, we propose a magnetar-star binary engine model to explain bumpy SLSNe.…”

Section: Summary and Discussionmentioning

confidence: 80%

Bumpy Superluminous Supernovae Powered by a Magnetar–Star Binary Engine

Zhu,

Liu,

et al. 2024

ApJL

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Wolf–Rayet stars in close binary systems can be tidally spun up by their companions, potentially leaving behind fast-spinning, highly magnetized neutron stars, known as “magnetars,” after core collapse. These newborn magnetars can transfer rotational energy into heating and accelerating the ejecta, producing hydrogen-poor superluminous supernovae (SLSNe). In this Letter, we propose that the magnetar wind of the newborn magnetar could significantly evaporate its companion star, typically a main-sequence or helium star, if the binary system is not disrupted by the abrupt mass loss and supernova (SN) kick. The subsequent heating and acceleration of the evaporated star material along with the SN ejecta by the magnetar wind can produce a postpeak bump in the SLSN lightcurve. Our model can reproduce the primary peaks and postpeak bumps of four example observed multiband SLSN lightcurves, revealing that the mass of the evaporated material could be ∼0.4–0.6 M ⊙ if the material is hydrogen-rich. We propose that the magnetar could induce strongly enhanced evaporation from its companion star near the pericenter if the orbit of the post-SN binary is highly eccentric, ultimately generating multiple postpeak bumps in the SLSN lightcurves. This “magnetar–star binary engine” model may offer a possible explanation for the evolution of polarization, along with the origin and velocity broadening of late-time hydrogen or helium broad spectral features observed in some bumpy SLSNe. The diversity in the lightcurves and spectra of SLSNe may be attributed to the wide variety of companion stars and post-SN binary systems.

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Section: Summary and Discussionmentioning

confidence: 80%

Bumpy Superluminous Supernovae Powered by a Magnetar–Star Binary Engine

Zhu,

Liu,

et al. 2024

ApJL

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“…The SN was discovered (Srivastav et al 2024;Tonry et al 2024) in NGC 3621 on MJD 60411.14 (UT 2024) by the ATLAS survey group with a discovery magnitude of 18.915 (orange-ATLAS). The fast rise in SN magnitudes was confirmed in further monitoring (Chen et al 2024a;Kumar et al 2024). The early spectra taken within a few hours suggest a Type II SN with flash features and the redshift z s = 0.002435 (Hoogendam et al 2024;Zhai et al 2024 (2024b).…”

Section: Introductionmentioning

confidence: 71%

Early-phase Simultaneous Multiband Observations of the Type II Supernova SN 2024ggi with Mephisto

Chen,

Kumar,

et al. 2024

ApJL

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We present early-phase good-cadence (hour-to-day) simultaneous multiband (ugi and vrz bands) imaging of the nearby supernova SN 2024ggi, which exploded in the nearby galaxy NGC 3621. A quick follow-up was conducted within less than a day after the explosion and continued for ∼23 days. The uvg band light curves display a rapid rise (∼1.4 mag day−1) to maximum in ∼4 days and absolute magnitude M g ∼ −17.75 mag. The postpeak decay rate in redder bands is ∼0.01 mag day−1. Different colors (e.g., u − g and v − r) of SN 2024ggi are slightly redder than SN 2023ixf. A significant rise (∼12.5 kK) in blackbody temperature (optical) was noticed within ∼2 days after the explosion, which successively decreased, indicating shock break out inside a dense circumstellar medium surrounding the progenitor. Using semianalytical modeling, the ejecta mass and progenitor radius were estimated as 1.2 M ☉ and ∼550 R ☉. The archival deep images (g, r, i, and z bands) from the Dark Energy Camera Legacy Survey were examined, and a possible progenitor was detected in each band (∼22–22.5 mag) and had a mass range of 14–17 M ☉.

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“…If the hydrogen-rich layers in the ejecta are thin enough, the second peak caused by the delayed energy injection could be observed as a hydrogenpoor event. The delayed energy injection may be caused by a fallback accretion disk toward the central compact remnant (e.g., Moriya et al 2019;Chen et al 2024). Depending on the initial angular momentum, the formation of the accretion disk that can provide the central energy injection could be delayed.…”

Section: Origin Of Sn 2023aewmentioning

confidence: 99%

“…Even though we now have hundreds of well-observed SESNe, there are still several open questions regarding their nature, when it comes to both their progenitor stars and their powering mechanism. Binarity seems to be a key component for stripping their envelopes, with arguments supported by relatively low ejecta masses, large relative rates (Smith 2011), and direct evidence of a binary system after the SESN 2022jli (Chen et al 2024). These deduced ejecta masses often come from comparisons with simple analytical models (e.g., Arnett 1982;Barbarino et al 2021;Yang & Sollerman 2023), which match reasonably well with the observed light curves assuming powering by radioactive 56 Ni.…”

Section: Introductionmentioning

confidence: 99%

Dramatic Rebrightening of the Type-changing Stripped-envelope Supernova SN 2023aew

Sharma,

Sollerman,

Kulkarni

et al. 2024

ApJ

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Multipeaked supernovae with precursors, dramatic light-curve rebrightenings, and spectral transformation are rare, but are being discovered in increasing numbers by modern night-sky transient surveys like the Zwicky Transient Facility. Here, we present the observations and analysis of SN 2023aew, which showed a dramatic increase in brightness following an initial luminous (−17.4 mag) and long (∼100 days) unusual first peak (possibly precursor). SN 2023aew was classified as a Type IIb supernova during the first peak but changed its type to resemble a stripped-envelope supernova (SESN) after the marked rebrightening. We present comparisons of SN 2023aew’s spectral evolution with SESN subtypes and argue that it is similar to SNe Ibc during its main peak. P-Cygni Balmer lines are present during the first peak, but vanish during the second peak’s photospheric phase, before Hα resurfaces again during the nebular phase. The nebular lines ([O i], [Ca ii], Mg i], Hα) exhibit a double-peaked structure that hints toward a clumpy or nonspherical ejecta. We analyze the second peak in the light curve of SN 2023aew and find it to be broader than that of normal SESNe as well as requiring a very high 56Ni mass to power the peak luminosity. We discuss the possible origins of SN 2023aew including an eruption scenario where a part of the envelope is ejected during the first peak and also powers the second peak of the light curve through interaction of the SN with the circumstellar medium.

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A 12.4-day periodicity in a close binary system after a supernova

Cited by 14 publications

References 167 publications

Bumpy Superluminous Supernovae Powered by a Magnetar–Star Binary Engine

Bumpy Superluminous Supernovae Powered by a Magnetar–Star Binary Engine

Early-phase Simultaneous Multiband Observations of the Type II Supernova SN 2024ggi with Mephisto

Dramatic Rebrightening of the Type-changing Stripped-envelope Supernova SN 2023aew

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