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Related Experiment Video

Updated: Jul 15, 2025

Emission Spectroscopic Boundary Layer Investigation during Ablative Material Testing in Plasmatron
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Circumstellar material ejected violently by a massive star immediately before its death.

Jujia Zhang1, Han Lin2, Xiaofeng Wang3

  • 1Yunnan Observatories (YNAO), Chinese Academy of Sciences, Kunming 650216, China; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, China; International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, China.

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Type II supernovae are common, but their progenitors remain mysterious. SN 2023ixf

Keywords:
Circumstellar materialCore-collapse supernovaMass lossSupernova: SN 2023ixf

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Area of Science:

  • Astronomy and Astrophysics
  • Stellar Evolution
  • Supernova Remnants

Background:

  • Type II supernovae are the most frequent stellar explosions.
  • The evolution of their massive, hydrogen-rich progenitors before core-collapse is not well understood.
  • SN 2023ixf in Messier 101 offers a unique chance to study these events.

Purpose of the Study:

  • To investigate the final evolutionary stages of massive stars leading to Type II supernovae.
  • To constrain the properties of circumstellar material around SN 2023ixf using early-time observations.
  • To identify the progenitor type of SN 2023ixf.

Main Methods:

  • Analysis of high-cadence flash spectra of SN 2023ixf within 1-5 days post-explosion.
  • Monitoring the rapid fading of narrow emission lines.
  • Studying the luminosity and profile of early Hα emission.

Main Results:

  • Estimated progenitor mass-loss rate of approximately 6x10^-4 M☉/year in the final 2-3 years before explosion.
  • Detected circumstellar material moving at ~55 km/s, forming a compact shell within 7x10^14 cm.
  • Pre-explosion observations suggest a possible yellow hypergiant progenitor.

Conclusions:

  • SN 2023ixf's progenitor experienced significant mass loss shortly before exploding.
  • The progenitor likely evolved from a red supergiant to a short-lived yellow hypergiant.
  • These findings provide crucial insights into the final evolution of massive stars.