()2004.11.17

II. II??III(2004)IV??, 2003V Glich ??, 2004VI 26Al??, 1992 VII. ??, 2002VIII!

: :()():(): 1)( A70): a) (s-); b) (r-); c) (rp)

() ; ()x ()

6(2002)1986(26Al

), (X-)

():

10-4 (1988 ) ~ 104 (1988 )

():()()()

(1980 ):( ) (1983 2000): SNII (1990 ) : SNSNIa (1988 ) : ;(2000): ()(2002): ()(1990 ()): AGB (1995 (,)):

(1990-1992, ); (12C + 12C, 16O + 16O, 14N + 16O )(1993) 19Ne(p,)20Na ()(, 1995 : 2002: (): 13C(, n)16O () (): 3He(, )7Be(, )11C( p, )12N(+)12C :, 26Al (1995), 2004

:: II ()(): 1)? 2)Glitch? 26Al? ? ?

? ?r-?()(: rp-s-)?

II. II

1. (SNIISNIb,SNIc)2. (SNIa)

M(12-25)MH-H-He-C-Ne-O-Si-Fe T (3-5)109K 3109g/cm3

()SNII( SNIbSNIc )(EC)

()

(SNIa )

II:Vr r()

:Vr ~ Vff/2

M ~ 0.6 M

:Vr ~ (1/8 1/4) c ()

nuc (nuc = 2.81014 g/cm3)

P

=5/3, (2-4)nuc

Eshock ~ 1051-52 ergs

1011K 10 MeV, 56Fe ( 8.8MeV):(1 foe = 1050 ergs )

1%( 1049ergs),

:()?;1) (), K 130 ( K 210-220)2)() ()

Wilson(Bowers, Wilson, 1985)0.5(1052ergs)Rs ~ Vff R :, Rns :Re:

1)??(? (u,d)? ) 2) 104 km/s 1049 erg?

:?1995(Dai Z. Peng Q. and Lu T. ApJ., 1995,440:815)-(u,d)-(s,u,d)u + e- d +e , u + e- s +e , u + d u + s 110MeV 1052erg Schwarshild,Fermi1/4(), Kernen et al.,2004, astro-ph/0406448 Neutrino emission and mass ejection in quark novae

? ( e-, e+, p, n, , 0, 16O)( 1049 erg )

Buras et al., 2003, Phys. Rev. Lett., 90 No. 24, 241101 Improved Models of Stellar Core Collapse and Still No Explosions:What is Missing?M.Liebendrfer, 2004, arXiv:astro-ph/0405029 Fifty-Nine Reasons for a supernova to not ExplodeMotizuki, Madokoro and Shimizu,arXiv:astro-ph/0406303 Core-Collapse Supernovae Induced By Anisotropic Neutrino Radiation Prolate explosions caused by globally anisotropic neutrino radiation is the most effective mechanism of increasing energy when the total neutrino luminosity is given.: ?? : OB (Be : P ~ 1 day, V(R) ~200km/s)?M~(10-25) M Be 7,?:?

III (Nucler Physics A738(2004)515-518)

: SN, Mch < Mcore(Fe) ( Mch Ye2 , Ye , Mch ) :: Mcore(Fe) : (Nucler Physics A738(2004)515-518):56Ni:

A) :(): ,

B), M < Eshock/|dE(+Fe)/dM| (), 1011 K -(u,d)- (u,d,s), (1)(Dai, Peng and Lu, 1995) > 1052 erg/s, 10 MeV

C) : Etot= aT4(4/3)R3 =const. ~ kT (Ri/Rf)3/4 (kTi); Ti ~ 1011K, (Ri/Rf) < 1/20, Tf ~ 1011K, kTf

D) ~ 1.610-44(sinW)4 A2 (E/MeV)2 cm2W: Weinberg A: ()(Q.-H. Peng, 2004, Nuclear Physics A738, 515)

I. , 2003

94()V (km/s) 100 71 3/4 300 36 38% 500 14 15% 1000 5 5%10% v 800 1000 km/s! ?(): v ~ (20 50) km/s () kick??(, 1015-1016)35

NSV()(, 2003, 25IAU ): 1980-1982()(Peng et al. 1982;Malov,2001): : 200-300 years Vmax 1000 km/s P0 < 0.7 ms Vmax>100 km/s P0< (2-3)ms Vmax > 2500 km/s P0 ~0.4msCrab PSR Vela PSR

P/P0

. Glich , 2004

Glitch(10-6-10-10),GlitchVela PRS Crab PSR, 3-4Glitch(10-12)19Glitch Vela PSR 11glitchPSR1737-30 9glitchglitchPtGlitch:

Glitch1. (Baym, 1969); 2.()(Pines et al., 1972);3.(Anderson and Ruderman,1984); 4. - (Ruderman, Zhu and Chen, 1998)()(1967): (Peng, Huang & Huang, 1980 ; Huang, Lingenfelter, Peng and Huang, 1982): 3P2 Cooper,(x-), 2004, 3P2

Glich3P2: kT= n(3P2 ) 0.05 MeV, T5.8108K:T, T= T , 3P2 3P2 (x-) T > T ,3P2 3P2 , ()Glitch

Glitch: 3P2 NSV(X-ray) T(3P2(n)) 3P2(Fermi) Glitch () T(3P2(n)) 3P2 SNV 3P2 NSV (Fermi) 3P2 NSVt 3P2 NSV n2(3P2(n)), 3P2 NSV : n2(3P2(n)) < n1(3P2(n)) Glitch()

Glitchglitch 3P2 NSV 3P2 NSV ()x ray() 3P2 NSV 3P2 NSV x ray3P2 NSV ,GlitchLyne (2000) P > 0.7s GlitchGlitchglitchGlitchGlitch

V I. 26Al , 1992

26Al1982-1984, 26Al ()- 26Al (1/2 7.2105) 2M 26Al ?201526AlIIWR(26AlrpMg-Al):Mg-Al

, 10-4, 1988104, 8 , WR26Al(1995)

26Al SNIa1995 27Al44Ti1992rp:

SNIa26Al26Al(SNIaSNII) 1992,( )( 12C+12C 16O+16O) (3-4) (7-10)[, 1992]

20Na 0.446s 18Ne 1.675s 19Ne 17.3s 18F 109.8m 17F 64.5s 20Ne 15O122s 19F 16O 17O 18O 15N14O70.6s 14N13N9.96m13C12C

VI I. (UHECR) , 2002

2.75 3.1

GZK (cutoff) (Greisen-Zatsepin-Kuz'min, 1966)

-(CR), (E > Ecut ) , D 50 Mpc GZKEcut()GZK E > 1020eV UHECR

E(eV) >1019 >41019 >1020 N(E) 581 57 8(Exposure: m2 s sr (AGASA, 20005) N(E) ~ 24 , E > 1020 eV ( 31020 eV) (P.L. Biermann(2001)): 3.21020 eV ( Flys Eye ) 2.11020 eV ( AGASA) : F( E>1020 eV) ~ 1 particle (km)-2(100yr)-1~ (1-3)10-20 particles cm-2sec-1 ~ 410-30 GeV-1 cm -2 sec-1

:ISM - SN: 100 Z TeV (TeV =1012eV)b) wind - SN: 100 Z PeV (PeV =1015eV) 31018 eV Fermi,c):(Hillas, A.M., Ann. Rev. Astron. Astrophys. 22 (1984) 425; Biermann, P.L.& Strittmatter, P.A., ApJ., 322(1987)643):50Mpc M87 10-2gauss, 103d)()()(Blasi et al., 2000) e)(C. Litwin and R. Rosner, 2001) Bottom-Up

Top-Down topological defects, superheavy relic particles, : , , (Peng, 2002)1020eV A toy model ()

VIII.

1968, Davis 1/330,20016SNO S-K

:

SNO()SNO( 8B):S-K ( 8B): 20016::8B

SNO 8B :SNO 8B 5.05 1.0 106 cm-2 s-1 Ahmad et al. Phys. Rev. Lett.89 (2002) 011302

2001SNO