Neutino-diven explosions of ulta-stipped type Ic supenovae geneating binay neuton stas Yudai Suwa 1, 2 1 Yukawa Institute fo Theoetical Physics, Kyoto U. 2 Max Planck Institute fo Astophysics, Gaching Collaboation with: T. Yoshida, M. Shibata (YITP), H. Umeda, K. Takahashi (U. Tokyo)
Yudai Suwa, MG14 @ Univ. of Rome 2 /14 Binay neuton stas cedit: NASA one of the best candidates of stong gavitational wave (GW) souces will be detected by GW in a couple of yeas (?) estimated mege ates ~1-4000 /gal/my, lage uncetainty! Abadie+ 2010 let me emind you that NSs ae bon to supenovae (SNe) supenova suveys might be able to give constaint on NS mege ates
Binay evolutions Thee ae two SNe fist one may be usual (type- Ibc o type II) second one explodes afte close binay inteactions, e.g. common envelope phase (if they ae close enough) How does a second SN look like? Is thee any diffeence fom nomal SNe? 14/7/2015 Tauis & van den Heuvel 2006 Yudai Suwa, MG14 @ Univ. of Rome 3 /14
Yudai Suwa, MG14 @ Univ. of Rome 4 /14 Ulta-stipped supenovae? Tauis, Lange, Podsiadlowski (2015) We theefoe suggest to define ulta-stipped SNe as exploding stas whose pogenitos ae stipped moe than what is possible with a non-degeneate companion. In othe wods, ultastipped SNe ae exploding stas which contain envelope masses < ~ 0.2 M and having a compact sta companion.
Yudai Suwa, MG14 @ Univ. of Rome 5 /14 Small ejecta mass Tauis+ 2013 Mej 0.2M 0.1M SN 2005ek
Yudai Suwa, MG14 @ Univ. of Rome 6 /14 Rapidly evolving supenovae Dout+ 2013 Dout+ 2014 ealy samples (05ek, 10X, 05E)+10 moe discoveies by Pan-STARRS t1/2<12 day diffusion time; τc Mej 3/4 EK -1/4 (Anett 1982) small Mej
Yudai Suwa, MG14 @ Univ. of Rome 7 /14 What we have done axiv:1506.08827
Stella evolutionay simulations-1: setups 14/7/2015 Stella evolution code fo massive stas (Umeda, Yoshida, Takahashi 2012; Takahashi, Yoshida, Umeda 2013; Yoshida, Okita, Umeda 2014) P = GM 1 M 4 4 4 4 t 2, = 1 M 4 2, ln T ln P = min( ad, ad), L = nucl M + gav. Nucleosynthesis and enegy geneation netwok with ~300 species Initial condition bae CO coes (mimicking mass loss) composition: cental abundance of massive stas just afte He buning XC(C) = 0.33-0.36 MCO=1.45, 1.5, 1.6, 1.8 and 2.0 M Yudai Suwa, MG14 @ Univ. of Rome 8 /14
Stella evolutionay simulations-1: setups 14/7/2015 Stella evolution code fo massive stas (Umeda, Yoshida, Takahashi 2012; Takahashi, Yoshida, Umeda 2013; Yoshida, Okita, Umeda 2014) P = GM 1 M 4 4 4 4 t 2, = 1 M 4 2, ln T ln P = min( ad, ad), L = nucl M + gav. Nucleosynthesis and enegy geneation netwok with ~300 species Initial condition bae CO coes (mimicking mass loss) composition: cental abundance of massive stas just afte He buning XC(C) = 0.33-0.36 MCO=1.45, 1.5, 1.6, 1.8 and 2.0 M Yudai Suwa, MG14 @ Univ. of Rome 8 /14
Stella evolutionay simulations-1: setups 14/7/2015 Stella evolution code fo massive stas (Umeda, Yoshida, Takahashi 2012; Takahashi, Yoshida, Umeda 2013; Yoshida, Okita, Umeda 2014) P = GM 1 M 4 4 4 4 t 2, = 1 M 4 2, ln T ln P = min( ad, ad), L = nucl M + gav. Nucleosynthesis and enegy geneation netwok with ~300 species Initial condition bae CO coes (mimicking mass loss) composition: cental abundance of massive stas just afte He buning XC(C) = 0.33-0.36 MCO=1.45, 1.5, 1.6, 1.8 and 2.0 M Yudai Suwa, MG14 @ Univ. of Rome 8 /14
Stella evolutionay simulations-1: setups 14/7/2015 Stella evolution code fo massive stas (Umeda, Yoshida, Takahashi 2012; Takahashi, Yoshida, Umeda 2013; Yoshida, Okita, Umeda 2014) P = GM 1 M 4 4 4 4 t 2, = 1 M 4 2, ln T ln P = min( ad, ad), L = nucl M + gav. Nucleosynthesis and enegy geneation netwok with ~300 species Initial condition bae CO coes (mimicking mass loss) composition: cental abundance of massive stas just afte He buning XC(C) = 0.33-0.36 MCO=1.45, 1.5, 1.6, 1.8 and 2.0 M Yudai Suwa, MG14 @ Univ. of Rome 8 /14
Stella evolutionay simulations-1: setups 14/7/2015 Stella evolution code fo massive stas (Umeda, Yoshida, Takahashi 2012; Takahashi, Yoshida, Umeda 2013; Yoshida, Okita, Umeda 2014) P = GM 1 M 4 4 4 4 t 2, = 1 M 4 2, ln T ln P = min( ad, ad), L = nucl M + gav. Nucleosynthesis and enegy geneation netwok with ~300 species Initial condition bae CO coes (mimicking mass loss) composition: cental abundance of massive stas just afte He buning XC(C) = 0.33-0.36 MCO=1.45, 1.5, 1.6, 1.8 and 2.0 M Yudai Suwa, MG14 @ Univ. of Rome 8 /14
Yudai Suwa, MG14 @ Univ. of Rome 9 /14 Stella evolutionay simulations-2: esults C-buning Off cente Ne-buning Off cente O-buning Off cente Si-buning Si shell-buning M CO =1.45 M Time befoe coe collapse (yea)
Yudai Suwa, MG14 @ Univ. of Rome 10/14 Explosion simulations-1: setups 2D (axial symmety) (ZEUS-2D; Stone & Noman 92) MPI+OpenMP hybid paallelized Hydodynamics+spectal neutino tansfe (neutino-adiation hydodynamics) hydodynamics See Suwa et al., PASJ, 62, L49 (2010) Suwa et al., ApJ, 738, 165 (2011) Suwa et al., ApJ, 764, 99 (2013) Suwa, PASJ, 66, L1 (2014) Suwa et al., axiv:1406.6414 Suwa et al., axiv:1506.08827 fo moe details ν tansfe Isotopic diffusion souce appoximation (IDSA) fo neutino tansfe (Liebendöfe+ 09) Ray-by-ay plus appoximation fo multi-d tansfe (Buas+ 06) EOS: Lattime-Swesty (K=180,220,375MeV) / H. Shen
Yudai Suwa, MG14 @ Univ. of Rome 11/14 Explosion simulations-2: movie entopy [kb/bayon] v /c
Yudai Suwa, MG14 @ Univ. of Rome 12/14 Explosion simulations-3: esults ALL models explode Final NS mass ~1.3-1.6M (bayonic) ~1.2-1.4M (gavitational) Tauis+ 2013 Ejecta mass=mco-mns ~ O(0.1)M Explosion enegy ~O(10 50 ) eg Ni mass ~O(10-2 )M
Yudai Suwa, MG14 @ Univ. of Rome 13/14 Implications small kick velocity due to small ejecta mass small eccenticity (e~0.1), compatible with binay pulsas J0737-3039 (e=0.088 now and ~0.11 at bith of second NS) even ate (~1% of coe-collapse SN) Pian & Shaviv 05 Tauis+13, 15, Dout+ 13, 14 SN suveys (e.g., HSC, PTF, Pan-STARRS, and LSST) will give constaint on NS mege ate adiation tansfe simulations will be done based on ou model
Yudai Suwa, MG14 @ Univ. of Rome 14/14 Summay Ulta-stipped SN might be second explosion in close binay foming binay NSs To test this conjectue, we pefomed stella evolutionay simulations of bae C/O coes hydodynamic simulations fo neutino-diven explosions Compatible with paametes explaining obsevations Eexp=O(10 50 ) eg Dout+ 13, Tauis+13 Mej~O(0.1) M MNi~O(10-2 )M MNS~1.2-1.4M (gavitational) See Suwa, Yoshida, Shibata, Umeda, Takahashi axiv:1506.08827 fo moe details