DISC1,AIMFIR LA-(JR--Ufl-25l7 j) E[jfi016479 . "Ibis repwt WIIS prcpured m tin uccount of work qmnnorcd hy Mq ugcncy or ihc ( Inital SIEICS ( iovcrnmcnt, Ndhcr Ihc IJnitcd SIuIc~(kwcrnmcnl nur uny ugcncy Ihcm)r, nor tiny IM their empl~)y~s, mukcs any wnrrHnly, c~prcss or implied, or nwumcs mry Icgnl liHhllity or rcq'nmni-hUity for the w:urwc y, w~mplc{cnns% or uwfulncw M ony infornrution, nppwrwtun.producl, or poems dindnd, or rcprcccnln thul its usc wuuki not infrirrgc privHtcly owned rlghtn, ltcfcrcnrx herein h) nny specific commercial product, prown, or scrvlcc +V trntlc numc, Irdcmnrk, nmnu(ndurcr, nr ntherwisc Am nnl nccewurily conslilum or imply il! cndmcrncnl, rcwnmcmlntion, or fnvorirrn hy Ihc I Jnilcrl SIIIICS (iovcrnmcnt or nny IIRcrrcy thcrcd. '1'hc vicwt wul opininnn of uuthwrs cqrrcrnscd herein do nut ncccsmrily *MC M TcllKd th.* d the [ Jnilal SIMICn( hwcrnnlcnl or wry u~cncy Ihcrcd.
ABSTRACTThe hydrodynamic shock origin o: cosmic rays in the q nvelope of a Type I presupernova star is reviewed. The possibility of accelerating 18 ultrahigh energy particles to~10 eV is unique to the shock mechanism and currently no other suggested galactic or cxtragalactic site is likely.Since ultruhigh energy is the most difficult part oi any acceleration mechanism, the associated lower energy particles are apriori more likely to dominate all other low qnergy acceleration uechanisms. The nonrelatlvistic hydrodynamic~upernova qxplosion sh~.k becomes relativistic at an external mass fraciion of (l-F) = 3 x 10-6 of the star that is composed primarily of helilunplus heavier nuclei. The resulting ejected relat~vls-Lic energy, (1oF) IIeC2 = 6 x 1048 ergs per SN1 is adequate to explain the Galactlc cosmic ray qnergy. The resulting spectrum beromes, N(>E) = (1-F) aE-2"5, in al -cement with observations. The heavy nuclel arc partially spalled in the shoch transition and par~ially resynthrslzed ]n the postshock qxpansion for E : 10 15 eV dependent upon the largr number of pnirs In Lh? post-shock fluid. Abovr this qnergy the shock pruRresses in the uagnetized photospherc. The high qnergy llmit is = 1021 CV dur LO~.hr coronal dennity of the presupernova star. The objert]on to SN~h[]t-h accelcratrd conmic rays by adinhatic der~leration is qurat]cd?rdon thr Fr~nce, Ed. J. Andouze. Co18ate, S. A. (1983a] 18th Int.
