The Astrophysical Journal (Jan 2024)

Early-time Observations of SN 2023wrk: A Luminous Type Ia Supernova with Significant Unburned Carbon in the Outer Ejecta

  • Jialian Liu,
  • Xiaofeng Wang,
  • Cristina Andrade,
  • Pierre-Alexandre Duverne,
  • Jujia Zhang,
  • Liping Li,
  • Zhenyu Wang,
  • Felipe Navarete,
  • Andrea Reguitti,
  • Stefan Schuldt,
  • Yongzhi Cai,
  • Alexei V. Filippenko,
  • Yi Yang,
  • Thomas G. Brink,
  • WeiKang Zheng,
  • Ali Esamdin,
  • Abdusamatjan Iskandar,
  • Chunhai Bai,
  • Jinzhong Liu,
  • Xin Li,
  • Maokai Hu,
  • Gaici Li,
  • Wenxiong Li,
  • Xiaoran Ma,
  • Shengyu Yan,
  • Jun Mo,
  • Christophe Adami,
  • Dalya Akl,
  • Sarah Antier,
  • Eric Broens,
  • Jean-Grégoire Ducoin,
  • Eslam Elhosseiny,
  • Thomas M. Esposito,
  • Michael Freeberg,
  • Priyadarshini Gokuldass,
  • Patrice Hello,
  • Sergey Karpov,
  • Isabel Márquez,
  • Martin Mašek,
  • Oleksandra Pyshna,
  • Yodgor Rajabov,
  • Denis Saint-Gelais,
  • Marc Serrau,
  • Oleksii Sokoliuk,
  • Ali Takey,
  • Manasanun Tanasan,
  • Damien Turpin

DOI
https://doi.org/10.3847/1538-4357/ad6600
Journal volume & issue
Vol. 973, no. 2
p. 117

Abstract

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We present extensive photometric and spectroscopic observations of the nearby Type Ia supernova (SN) 2023wrk at a distance of about 40 Mpc. The earliest detection of this SN can be traced back to a few hours after the explosion. Within the first few days, the light curve shows a bump feature, while the B − V color is blue and remains nearly constant. The overall spectral evolution is similar to that of an SN 1991T/SN 1999aa-like SN Ia, while the C ii λ 6580 absorption line appears to be unusually strong in the first spectrum taken at t ≈ −15.4 days after the maximum light. This carbon feature disappears quickly in subsequent evolution but it reappears at around the time of peak brightness. The complex evolution of the carbon line and the possible detection of Ni iii absorption around 4700 Å and 5300 Å in the earliest spectra indicate macroscopic mixing of fuel and ash. The strong carbon lines are likely related to the collision of SN ejecta with unbound carbon, consistent with the predictions of pulsational delayed-detonation or carbon-rich circumstellar-matter interaction models. Among those carbon-rich SNe Ia with strong C ii λ 6580 absorption at very early times, the line-strength ratio of C ii to Si ii and the B − V color evolution are found to exhibit large diversity, which may be attributed to different properties of unbound carbon and outward-mixing ^56 Ni.

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