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The spectacular evolution of Supernova 1996al over 15 yr: a low-energy explosion of a stripped massive star in a highly structured environment

Benetti, S ; Chugai, N. N ; Utrobin, V. P ; Cappellaro, E ; Patat, F ; Pastorello, A ; Turatto, M ; Cupani, G ; Neuhäuser, R ; Caldwell, N ; Pignata, G ; Tomasella, L

Monthly notices of the Royal Astronomical Society, 2016-03, Vol.456 (3), p.3296-3317 [Periódico revisado por pares]

London: Oxford University Press

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  • Título:
    The spectacular evolution of Supernova 1996al over 15 yr: a low-energy explosion of a stripped massive star in a highly structured environment
  • Autor: Benetti, S ; Chugai, N. N ; Utrobin, V. P ; Cappellaro, E ; Patat, F ; Pastorello, A ; Turatto, M ; Cupani, G ; Neuhäuser, R ; Caldwell, N ; Pignata, G ; Tomasella, L
  • Assuntos: Asymmetry ; Ejecta ; Emission ; Explosions ; H alpha line ; Hydrogen ; Kinetic energy ; Kinetics ; Luminosity ; Massive stars ; Star & galaxy formation ; Supernovae
  • É parte de: Monthly notices of the Royal Astronomical Society, 2016-03, Vol.456 (3), p.3296-3317
  • Notas: ObjectType-Article-1
    SourceType-Scholarly Journals-1
    ObjectType-Feature-2
    content type line 23
  • Descrição: Spectrophotometry of SN 1996al carried out throughout 15 yr is presented. The early photometry suggests that SN 1996al is a linear Type II supernova, with an absolute peak of M V ∼ −18.2 mag. Early spectra present broad asymmetric Balmer emissions, with superimposed narrow lines with P-Cygni profile, and He i features with asymmetric broad emission components. The analysis of the line profiles shows that the H and He broad components form in the same region of the ejecta. By day +142, the Hα profile dramatically changes: the narrow P-Cygni profile disappears, and the Hα is fitted by three emission components that will be detected over the remaining 15 yr of the supernova (SN) monitoring campaign. Instead, the He i emissions become progressively narrower and symmetric. A sudden increase in flux of all He i lines is observed between 300 and 600 d. Models show that the SN luminosity is sustained by the interaction of low-mass (∼1.15 M⊙) ejecta, expelled in a low kinetic energy (∼1.6 × 1050 erg) explosion, with highly asymmetric circumstellar medium. The detection of Hα emission in pre-explosion archive images suggests that the progenitor was most likely a massive star (∼25 M⊙ ZAMS) that had lost a large fraction of its hydrogen envelope before explosion, and was hence embedded in a H-rich cocoon. The low-mass ejecta and modest kinetic energy of the explosion are explained with massive fallback of material into the compact remnant, a 7–8-M⊙ black hole.
  • Editor: London: Oxford University Press
  • Idioma: Inglês
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  • Realização: ABCD-USP USP   Logos de Redes Sociais: Freepik

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