SN 2007bi Yoshida, T. & Umeda, H., MNRAS 412, L78-L82 (2011)
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1 SN 2007bi Yoshida, T. & Umeda, H., MNRAS 412, L78-L82 (2011)
2 SN 2007bi SN 2007bi (Gal-Yam et al. 2009) Type Ic subluminous dwarf galaxy Z ~ ( ) Z (Young et al. 2010) 36 (Young et al. 2010)
3 SN2007bi SN2007bi Fλ (10-18 erg s -1 cm -2 A -1 ) Rest Wavelength (A ) (Gal-Yam et al. 2009) (Filippenko 1997) SN 2007bi Type Ic CO H,He Ia II Ic Ib
4 type Type Ia MS WD Type II H He O Si Fe Type Ib O He Si Fe Type Ic O Si Fe or binary
5 超新星typeと爆発機構 核燃焼型 Type Ia 未観測 Pair instability超新星 (II,Ib,Ic?) H MS He O WD 重力崩壊型 Type II H He O Fe Type Ib O Type Ic He O O Fe Si Fe Si Si 巨大質量 or binary 吉田敬 CPSセミナー ６月１日神戸大学CPS
6 SN 2007bi SN 2007bi (Gal-Yam et al. 2009) MR,max = mag Absolute MR (mag) SN 2007bi SN 1987A c.f. M( 56 Ni) = 0.07 M Julian date - 2,450,000 (SN 1987A) (Gal-Yam et al. 2009) 56 Ni M( 56 Ni) ~ 3-10 M
7 SN 2007bi Absolute MR (mag) (Gal-Yam et al. 2009) (Moriya et al. 2010) Pair-instability SN (PISN) Core collapse SN (CCSN) Mf ~ M Mf ~ 43 M Ni M( 56 Ni) ~ 3-10 M
8 Pair-Instability or Core Collapse? SN 2007bi Type Ic M( 56 Ni) ~ 3-10 M He Pair-instability (PISN) Mf ~ M (CCSN) Mf ~ 43 M
9 SN 2007bi 100 M < MMS < 500 M, Z0 = 0.2 Z MMS Mf CO core MCO He M(He) SN 2007bi PISN CCSN
10 MMS > 100 M Saio, Nomoto, and Kato 1988 P Mr = GMr 4πr 4 r Mr = 1 4πr 2 ρ ln T ln P = min( ad, rad) Lr Mr = εnucl - ε ν + εgrav 100 M < MMS < 500 M, Z0 = 0.2 Z, n, H~Br(282 ) Opacity OPAL 1995, etc.
11 MMS > 100 M OB Vink et al. (2001); Z Radiation-driven wind de Jager et al. (1988) Z 0.64 Wolf-Rayet (WR) Nugis and Lamers (2000; NL00) wind
12 MMS > 100 M Case A Case B Case C WR 1.5 (Crowther et al. 2007) 1/2 (Hirschi 2008) (Vink et al. 2001; Pulse et al. 2008)
13 MMS > 100 M WNL H H He He+H He (Xs(H) < 0.4) Wolf-Rayet WO O,C WC O,C WNE He O,C (Ns(He) < Ns(C+O)) (Ns(N) < Ns(C), Ns(He) > Ns(C+O)) (Xs(H) < 10-5, Ns(N) > Ns(C))
14 Mass Fraction WNL 1H 4He 12C Total mass WNLWC WO WNE 1H 4He 12C O O Mtotal / M Case A MMS = 100 M tms-c = 3.19 Myr WNL WNE WC WO Time (Year) 10 4 Total mass MMS = 140 M tms-c = 2.86 Myr
15 Mass Fraction at Center WNLWC WO 1H 4He 12C WNLWC WO 1H 4He 12C 10 6 Time (Year) 10 4 Total mass Total mass O 16O Mtotal / M Case A MMS = 200 M tms-c = 2.61 Myr MMS = 300 M tms-c = 2.51 Myr WNL WNE WC WO
16 Mass Fraction He MMS = 200 M M = 91.9 M WNL He 12C 16O 1H 14N 20Ne Mass Fraction M MS / M MMS = 200 M M = 67.8 M WO C 4He 16O 20Ne M MS / M
17 Mass Fraction MMS = 200 M MMS = 300 M Mf = 59.0 M WO Mf = 71.6 M WO C 16O 4He 20Ne Mass Fraction O 12C 20Ne 4He M MS / M M MS / M
18 Mass Fraction MMS = 100 M MMS = 140 M Mf = 40.8 M WNE Mf = 53.1 M WO O 4He 20Ne 12C 14N Mass Fraction O 20Ne 12C 4He M MS / M M MS / M
19 M f / M MMS Mf Case A Case C Case A Case B M MS / M WN WC (He-rich) WC WO Mf ~ M : WO MMS Mf
20 CO core MMS CO core MCO 150 M CO / M Case C Case A Case B M MS / M WN WC (He-rich) WC WO SN 2007bi
21 Pair-Instability 56 Ni Pair-Instability (Heger & Woosley 2002) III He Z0=0 M( 56 Ni) / M M CO / M SN 2007bi 56 Ni (Gal-Yam et al. 2009) PISN MCO ~ M Umeda & Nomoto (2002)
22 56 Ni III (Umeda & Nomoto 2008) 56 Ni M( 56 Ni) / M 10 8 E51 = 30 6 E51 = E51 = 10 E51 = M CO / M E51 = Eexp/(10 51 ergs) SN 2007bi 56 Ni (Gal-Yam et al. 2009) MCO > 35 M ~ MCO > 60 M PISN (Heger & Woosley 2002) CCSN: MCO ~ M
23 CO core M CO / M MMS CO core MCO PISN Case B Case C Case A CCSN PISN CCSN PISN CCSN M MS / M MMS ~ M (MMS ~ M for Case C) MMS ~ M (MMS ~ M for Case B) (MMS ~ M for Case C) M( 56 Ni) = 3-10 M (Gal-Yam et al. 2009) MCO ~ M MCO ~ M (Umeda & Nomoto 2002, 2008; Heger & Woosley 2002)
24 He Type Ic He He?
25 He Type Ic He He? He 56 Ni 56 Co γ He I line (5876A ) (Lucy 1991) He 56 Ni (e.g. Woosley & Eastman 1997) Type Ic He
26 He M(He) / M Z0 = Z0 = Z0 = M MS / M Wellstein & Langer (1999); Yoon et al. (2010) WN WC He Georgy et al. (2009) type : : WN : WC,WO binary Type Ib, Ic M(He) < 0.5 M Type Ic ( > 0.98 M Ib) M(He) < M Type Ic WC,WO M(He) < 0.6 M M(He) < M Type Ic
27 He M(He) / M He SN 2007bi CCSN M MS / M Case C Case A Case B PISN M(He) < M Ic M(He) < 0.5 M SN 2007bi M(He) < 1.5 M CO core SN 2007bi WC, WO Ic
28 rpi/cc : SN 2007bi PISN, CCSN Salpeter IMF ( MMS ) Case PISN (M ) CCSN (M ) rpi/cc A B C M(He) < 1.5 M XS(He) < 0.5 *M(He) < 0.5 M PISN IMF SN2007bi
29 100 M < MMS < 500 M, Z0 = 0.2 Z PISN, CCSN Type Ic SN 2007bi MMS Case PISN (M ) CCSN (M ) rpi/cc A B C M(He) < 0.5 M ( - ) ( - ) - ( - ) M(He) < 1.5 M XS(He) < 0.5 ( ) ( ) ( - ) SN2007bi (CCSN)
H+He H+He M > 10 M He He Wolf-Rayet Minit = 13 ~ 100 M, Zinit = 0.0001 ~ 0.02 CNO SN 2007bi (Type Ic) progenitor Minit > 100 M, Zinit = 0.004 WO star? Core collapse Rotating star model Saio, Nomoto, and
超新星残骸Cassiopeia a と 非球対称爆発
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23 1 Section ( ) ( ) ( 46 ) , 238( 235,238 U) 232( 232 Th) 40( 40 K, % ) (Rn) (Ra). 7( 7 Be) 14( 14 C) 22( 22 Na) (1 ) (2 ) 1 µ 2 4
23 1 Section 1.1 1 ( ) ( ) ( 46 ) 2 3 235, 238( 235,238 U) 232( 232 Th) 40( 40 K, 0.0118% ) (Rn) (Ra). 7( 7 Be) 14( 14 C) 22( 22 Na) (1 ) (2 ) 1 µ 2 4 2 ( )2 4( 4 He) 12 3 16 12 56( 56 Fe) 4 56( 56 Ni)
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