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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 environmentстатья
Статья опубликована в высокорейтинговом журнале
Информация о цитировании статьи получена из
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Статья опубликована в журнале из списка Web of Science и/или Scopus
Дата последнего поиска статьи во внешних источниках: 10 июля 2019 г.
- Авторы: Benetti S., Чугай Николай Николаевич, Utrobin V.P., Cappellaro E., Patat F., Pastorello A., Turatto M., Cupani G., Neuhäuser R., Caldwell N., Pignata G., Tomasella L.
- Журнал: Monthly Notices of the Royal Astronomical Society
- Том: 456
- Номер: 3
- Год издания: 2016
- Издательство: Oxford Journals, Oxford University Press
- Местоположение издательства: Oxford, UK, England
- Первая страница: 3296
- Последняя страница: 3317
- DOI: 10.1093/mnras/stv2811
- Аннотация: 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 MV ∼ −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.
- Добавил в систему: Кузнецов Артем Сергеевич