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Type Ia SN 2019ein: New Insights into the Similarities and diversities among High-Velocity SNe Ia | | Miho Kawabata
; Miho Kawabata
; Keiichi Maeda
; Masayuki Yamanaka
; Tatsuya Nakaoka
; Koji Kawabata
; Ryo Adachi
; Hiroshi Akitaya
; Umut Burgaz
; Hidekazu Hanayama
; Takashi Horiuchi
; Ryohei Hosokawa
; Kota Iida
; Fumiya Imazato
; Keisuke Isogai
; Jiang Jian
; Noriyuki Katoh
; Hiroki Kimura
; Masaru Kino
; Daisuke Kuroda
; Hiroyuki Maehara
; Kazuya Matsubayashi
; Kumiko Morihana
; Katsuhiro Murata
; Takashi Nagao
; Masafumi Niwano
; Daisaku Nogami
; Motoki Oeda
; Tatsuharu Ono
; Hiroki Onozato
; Masaaki Otsuka
; Tomoki Saito
; Mahito Sasada
; Kazuki Shiraishi
; Haruki Sugiyama
; Kenta Taguchi
; Jun Takahashi
; Kengo Takagi
; Seiko Takagi
; Masaki Takayama
; Miyako Tozuka
; Kazuhiro Sekiguchi
; | | Date: |
8 Aug 2019 | | Abstract: | We present optical observations of type Ia supernova (SN) 2019ein, starting
at 0.3 days since the discovery. The spectra and the light curves show that SN
2019ein belongs to the High-Velocity (HV) group with relatively rapid decline
in the light curves (delta m15(B)=1.36+-0.02 mag) and the short rise time. The
Si ii 6355 velocity, associated with a photospheric component but not with a
detached high-velocity feature, reached 20,000 km s-1 in our first spectrum
taken at 12 days before the B-band maximum. This is among the highest velocity
seen in SNe Ia. The line velocity however decreased very rapidly and smoothly
toward the maximum light, where it was 13,000 km s-1 as relatively low among HV
SNe. The rapid spectral evolution and the short rise time are probably linked
to the rapidly evolving light curves, suggesting that not only the (maximum)
velocity but also the light curve decline rate are controlling functions of the
observational properties of HV SNe. The earliest light curves did not show
noticeable excess, ruling out a giant companion star. Spectral synthesis
modeling shows that the outermost layer at >17,000 km s-1 is well described by
the O-Ne-C burning layer extending to at least 25,000 km s-1, and there is no
unburnt carbon below 30,000 km s-1; these properties are largely consistent
with the delayed detonation scenario, and it is shared with the prototypical HV
SN 2002bo despite large difference in delta m15(B). This structure is
strikingly different from that derived for the well-studied NV
(Normal-Velocity) SN 2011fe; we suggest that the relation between the mass of
56Ni (or delta m15) and the extent of the O-Ne-C provides an important
constraint on the explosion mechanism(s) of HV and NV SNe. | | Source: | arXiv, 1908.3001 | | Services: | Forum | Review | PDF | Favorites | |
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