Production of Silicon on Mass-increasing White Dwarfs: Possible Origin of High-velocity Features in Type Ia Supernovae

Mariko Kato, Hideyuki Saio, Izumi Hachisu

Research output: Contribution to journalArticle

4 Citations (Scopus)

Abstract

Type Ia supernovae (SNe Ia) often show high-velocity absorption features (HVFs) in their early phase spectra; however, the origin of the HVFs is unknown. We show that a near-Chandrasekhar-mass white dwarf (WD) develops a silicon-rich layer on a carbon-oxygen (CO) core before it explodes as an SN Ia. We calculated the nuclear yields in successive helium shell flashes for 1.0 M , 1.2 M , and 1.35 M CO WDs accreting helium-rich matter with several mass-accretion rates, ranging from 1 ×10-7 M yr-1 to 7.5 ×10-7 M yr-1. For the 1.35 M WD with the accretion rate of 1.6 ×10-7 M yr-1, the surface layer developed as helium burning ash and consisted of 40% 24Mg, 33% 12C, 23% 28Si, and a few percent of 20Ne by weight. For a higher mass-accretion rate of 7.5 ×10-7 M yr-1, the surface layer consisted of 58% 12C, 31% 24Mg, and 0.43% 28Si. For the 1.2 M WDs, silicon is produced only for lower mass-accretion rates (2% for 1.6 ×10-7 M yr-1). No substantial silicon (<0.07%) is produced on the 1.0 M WD independently of the mass-accretion rate. If the silicon-rich surface layer is the origin of Si ii HVFs, its characteristics are consistent with that of mass-increasing WDs. We also discuss possible Ca production on very massive WDs (1.38 M ).

Original languageEnglish
Article number125
JournalAstrophysical Journal
Volume863
Issue number2
DOIs
Publication statusPublished - 2018 Aug 20

Fingerprint

silicon
supernovae
accretion
helium
surface layer
surface layers
oxygen
carbon
ashes
flash
ash
rate
shell

Keywords

  • novae, cataclysmic variables
  • stars: individual (V445 Pup)
  • supernovae: general
  • white dwarfs

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Production of Silicon on Mass-increasing White Dwarfs : Possible Origin of High-velocity Features in Type Ia Supernovae. / Kato, Mariko; Saio, Hideyuki; Hachisu, Izumi.

In: Astrophysical Journal, Vol. 863, No. 2, 125, 20.08.2018.

Research output: Contribution to journalArticle

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abstract = "Type Ia supernovae (SNe Ia) often show high-velocity absorption features (HVFs) in their early phase spectra; however, the origin of the HVFs is unknown. We show that a near-Chandrasekhar-mass white dwarf (WD) develops a silicon-rich layer on a carbon-oxygen (CO) core before it explodes as an SN Ia. We calculated the nuclear yields in successive helium shell flashes for 1.0 M ⊙, 1.2 M ⊙, and 1.35 M ⊙ CO WDs accreting helium-rich matter with several mass-accretion rates, ranging from 1 ×10-7 M ⊙ yr-1 to 7.5 ×10-7 M ⊙ yr-1. For the 1.35 M ⊙ WD with the accretion rate of 1.6 ×10-7 M ⊙ yr-1, the surface layer developed as helium burning ash and consisted of 40{\%} 24Mg, 33{\%} 12C, 23{\%} 28Si, and a few percent of 20Ne by weight. For a higher mass-accretion rate of 7.5 ×10-7 M ⊙ yr-1, the surface layer consisted of 58{\%} 12C, 31{\%} 24Mg, and 0.43{\%} 28Si. For the 1.2 M ⊙ WDs, silicon is produced only for lower mass-accretion rates (2{\%} for 1.6 ×10-7 M ⊙ yr-1). No substantial silicon (<0.07{\%}) is produced on the 1.0 M ⊙ WD independently of the mass-accretion rate. If the silicon-rich surface layer is the origin of Si ii HVFs, its characteristics are consistent with that of mass-increasing WDs. We also discuss possible Ca production on very massive WDs (1.38 M ⊙).",
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AB - Type Ia supernovae (SNe Ia) often show high-velocity absorption features (HVFs) in their early phase spectra; however, the origin of the HVFs is unknown. We show that a near-Chandrasekhar-mass white dwarf (WD) develops a silicon-rich layer on a carbon-oxygen (CO) core before it explodes as an SN Ia. We calculated the nuclear yields in successive helium shell flashes for 1.0 M ⊙, 1.2 M ⊙, and 1.35 M ⊙ CO WDs accreting helium-rich matter with several mass-accretion rates, ranging from 1 ×10-7 M ⊙ yr-1 to 7.5 ×10-7 M ⊙ yr-1. For the 1.35 M ⊙ WD with the accretion rate of 1.6 ×10-7 M ⊙ yr-1, the surface layer developed as helium burning ash and consisted of 40% 24Mg, 33% 12C, 23% 28Si, and a few percent of 20Ne by weight. For a higher mass-accretion rate of 7.5 ×10-7 M ⊙ yr-1, the surface layer consisted of 58% 12C, 31% 24Mg, and 0.43% 28Si. For the 1.2 M ⊙ WDs, silicon is produced only for lower mass-accretion rates (2% for 1.6 ×10-7 M ⊙ yr-1). No substantial silicon (<0.07%) is produced on the 1.0 M ⊙ WD independently of the mass-accretion rate. If the silicon-rich surface layer is the origin of Si ii HVFs, its characteristics are consistent with that of mass-increasing WDs. We also discuss possible Ca production on very massive WDs (1.38 M ⊙).

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