Table 2: Four-step model-PN evolution. Integrated intensity of representative nebular emissions (relative to I(H $\beta )=100$), absolute H$\beta $ flux, and ionized mass for the adopted, spherically symmetric nebula (Table 1) powered by a hydrogen-burning post-AGB star of 0.605 $M_\odot $.
$\lambda $ ($\rm\AA\/$) Ion   I($\lambda $)    
    Sect. 4.4 Sect. 4.1 Sect. 4.2 Sect. 4.3
    proto-PN + early-PN intermediate-PN late-PN
    "born-again'' low-exc.-PN      
    (very thick) (nearly thin) (thin) (recombining)
    T*=25 000 K T*=50 000 K T*=100 000 K T*=150 000 K
    L*/ $L_\odot =6500$ L*/ $L_\odot =6500$ L*/ $L_\odot =6500$ L*/ $L_\odot =1000$
3425 [Ne V] 0.0 0.0 4.1 14.7
3726+29 [O II] 133.3 231.2 73.8 587.5
3968 [Ne III] 0.02 15.2 49.8 64.9
4686 He II 0.0 0.25 19.0 42.2
4740 [Ar IV] 0.0 0.22 3.4 2.9
4861 H I 100.0 100.0 100.0 100.0
5007 [O III] 5.5 490.0 1510.0 1312.2
5876 He I 3.11 15.5 12.6 10.5
6300 [O I] 1.3 2.5 0.1 26.3
6563 H I 297.2 291.7 285.7 288.4
6584 [N II] 265.5 169.0 37.3 434.5
6717+31 [S II] 43.1 24.4 12.4 107.3
7005 [Ar V] 0.0 0.0 0.77 1.05
7135 [Ar III] 1.6 17.4 21.0 30.7
7320 [O II] 0.8 2.2 1.0 9.8
$\log E$(H$\beta $) (erg s-1) 34.549 35.057 35.019 34.321
$M_{\rm ion}$ ($M_\odot $) 0.10 0.38 0.40 0.07*
          * excluding the ionized mass
          of the recombining halo

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