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in general temperature fluctuations are fairly large The values of are very large for filling factors larger than 0 001 they are in fact above the 5 mark for burst ages of 3 to 7 Myr Figure 1 Dependence of with the age of the burst and with the filling factor of the gas The model results shown are for solar metallicity 3 DISCUSSION Peimbert 1995 summarizes
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τα επιβεβαιωμένα κρούσματα σε 42 χώρες με 86 ανθρώπους να έχουν χάσει τη ζωή τους Σε περιπτώσεις που ο ιός Η1Ν1 είναι ευρέως διαδεδομένος και κυκλοφορεί στη
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봉사자를 찾는다고 하면서 특히 전문분야에 종사하시는 전문인들을 찾고 있다 관심 있는 봉사자들은 한미봉사회로 문의하면 된다 408 920 9733
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temperature fluctuations are consequently larger A similar explanation is put forward by KF95 to explain the increasing trend of t2 with the effective temperature of the ionizing source Figure 4 Spectral energy distribution of the ionizing cluster as a function of wavelength and energy for ages 1 Myr to 7 Myr Note the dramatic changes at 3 Myr when the SED hardens
2 Temperature structure of the model nebula as a function of depth into the nebula and of the burst age The model results shown are for solar metallicity and a filling factor of 0 1 Figure 3 Hydrogen and oxygen ionization structures at two epochs 2 Myr and 3 Myr The temperature structure is also plotted for reference The model results shown are for solar metallicity
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+3 and higher ionization stages Thus in effect the O +2 region decreases in relation to the H + region which in turn becomes hotter on average due to the new hot highly ionized zone Figure 2 Temperature structure of the model nebula as a function of depth into the nebula and of the burst age The model results shown are for solar metallicity and a filling factor of 0 1
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