MIXING CONSTRAINTS ON THE PROGENITOR OF SUPERNOVA 1987A

Transcription

1 MIXING CONSTRAINTS ON THE PROGENITOR OF SUPERNOVA 1987A Victor Utrobin ITEP, Moscow in collaboration with Annop Wongwathanarat (MPA, RIKEN), Hans-Thomas Janka (MPA), and Ewald Müller (MPA) Workshop on The Progenitor-Supernova-Remnant Connection Ringberg Castle, Tegernsee, Germany July 24 28, 2017

2 Core-Collapse Supernova Relative Fractions 1524 N. Smith et al. Figure 1. Relative fractions of CCSN types in a volume-limited sample from LOSS. This is slightly different from the fractions quoted in Paper II, in order to better suit the aim of this paper as explained in the text. The main broad-lined SNe Ic such as SN 2002ap th We have moved these to the SN Ic catego this paper, since they clearly correspond to fully shed their H and He envelopes. This h overall statistics, because broad-lined SNe sample, contributing only 1 2 per cent of agreement with the recent study of Arcavi ordinary that broad-lined SNe IIPSNe Ic 50% contribute only 1.8 (Li large et al. galaxies. 2011, It Smith is noteworthy, et al. 2011) however, th find broad-lined SNe Ic to be much more c of CCSNe) in low-metallicity dwarf host ga SNe occurring in highly inclined galaxies, w SN 1987A-like events 1 3% may introduce statistical problems that are (Pastorello a result of these et al. minor 2012) adjustments, made b vestigating implications for massive-star evo the goal of deriving relative rates and corre biases, the relative fractions of various SN Fig. 1 differ slightly from the results in Pape In quoting fractions of various SN types galaxy class, and other properties, although importance of these properties and consider below. The galaxies included in the LOSS luminosity, with most of the CCSN hosts to metallicities of Z (Garnett 2002; ple spans a range of M K from about 20 to the CCSN hosts are in the range of 22 t II). We note some trends in Paper II, such a

3 Light Curve of Peculiar Type IIP SN 1987A Open circles (Catchpole et al. 1987,1988); open triangles (Hamuy et al. 1988).

4 SN 1987A: Evidence for H and 56 Ni Mixing The [Ni II] 6.64 µm profile at day 640 gives v FWHM = 3100 km s 1 (Colgan et al. 1994). Not flat-topped Hα profile on day 498 (Phillips et al. 1990) implies that there is no cavity free of hydrogen at zero velocity.

5 SN 1987A: Bochum Event and Fast Ni Clump Fast 56 Ni clump: v 3D 4700 km s 1, M Ni 10 3 M (Utrobin et al. 1995).

6 First approach Modeling of Supernovae: Three Approaches No fit Second approach 3D simulations No fit Third approach Fit

7 Light Curve: Radioactive 56 Ni and Mixing SN 1987A originates from BSG; its light curve is powered by radioactive decays.

8 Presupernova Models for Blue Supergiants Model R psn MHe core M psn M ZAMS X surf Y surf Z surf Rot. Ref. (R ) (M ) (10 2 ) B No 1 W Yes 2 W Yes 2 W18r Yes 3 W18x Yes 2 N No 4 W No 5 (1) Woosley et al. (1988), (2) Sukhbold et al. (2016), (3) Woosley (priv. comm.), (4) Shigeyama & Nomoto (1990), (5) Woosley et al. (1997)

9 Presupernova Models: Density vs. Interior Mass

10 Presupernova Models: Density vs. Radius

11 Pre-SN Models: Mass Fractions vs. Interior Mass

12 Hydrodynamic Models Model M NS M env E exp M min Ni MNi max M Ni vni bulk (M ) (B) (10 2 M ) (km s 1 ) v tail Ni B W W W18r W18x W18x N20-P W

13 Morphology of 56 Ni-rich Matter in Model B15-2

14 Morphology of 56 Ni-rich Matter in Model W18

15 More Massive Helium Core, Lower 56 Ni Velocity Only model B15-2 yields maximum Ni velocity consistent with the observations!

16 Hertzsprung-Russell Diagram for SN 1987A Progenitors. Single Star Scenario Sukhbold et al. (2016)

17 Two Possible Solutions of The Problem A rapid rotation of Fe core producing more extent of Ni mixing. A binary evolution scenario for the BSG Sanduleak Credit: (ESA/STScI), HST, NASA The triple-ring system was explained by Morris & Podsiadlowski (2009) in the scenario of a binary merger model.

18 Hertzsprung-Russell Diagram for SN 1987A Progenitors. Binary Merger Scenario 5.6 Sk log (L/L ) log (T eff ) (K) 3.6 M 2 = 2 M M 2 = 4 M M 2 = 6 M M 2 = 8 M He core 3.73 M 3.63 M 3.61 M 3.52 M M 1 = 16 M Menon & Heger (2017), see also A. Menon s talk.

19 Bolometric Light Curves The total 56 Ni mass is scaled to fit the observed luminosity in the radioactive tail.

20 Light Curves: Artificial Mixing The total 56 Ni mass is scaled to fit the observed luminosity in the radioactive tail.

21 Summary 3D neutrino-driven explosion simulations of SN 1987A are able to synthesize the 56 Ni mass estimated from the observed luminosity in the radioactive tail. The extent of outward 56 Ni mixing in the framework of the 3D simulations decreases with He-core masses of the corresponding progenitor models. In 3D simulations only the model with He-core mass of 4 M yields a maximum velocity of the bulk of 56 Ni consistent with SN 1987A observations. In a single star scenario Sk seems to require a progenitor with a 6 M He core, and a 4 M He core is not able to explain the colorluminosity properties before collapse. Rapid rotation of the iron core might lead to more mixing. Investigations are needed. Binary progenitor models with 4 M He cores can account for the colorluminosity properties of Sk (see A. Menon s talk). But do they yield the extent of mixing to explain SN 1987A observations? Inward hydrogen mixing leads to minimum velocities of H-rich matter of less than 100 km s 1 in a good agreement with SN 1987A observations. Future 3D neutrino-driven explosion simulations on the basis of binary merger models of Menon & Heger (2017) for the progenitor of SN 1987A.