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- W2115698380 abstract "The physical conditions which characterize individ- ual Liners are obtained by tting the observational spectra of the Ho et al. (1993) sample by model calculations. Composite models which consistently account both for shocks, accompa- nying the radial outward motion of the gaseous clouds, and a photoionizing radiation flux are used. Power-law or black body radiation is considered, depending on the characteristics of the line spectra. The SUMA code is used. The contributions of the differentionizationmechanismstothespectrumemittedbyeach object are calculated and compared with the observations. ThemostsignicantlineratiosofLinerspectraareanalyzed to show the relative importance of photoionization by radiation from the active center or from starbursts, of photoionization by diffuse radiation, and of collisional ionization by shocks. Model results show that (NeV) lines can be strong due to collisional ionization and/or photoionization. Lines from the II and III ionization levels are usually due to photoionization, but a strong contribution by collisional ionization appears in case of high densities and/or of a strong shock. Neutral lines are enhanced by diffuse radiation. The contribution of high density gastothelineintensitiesinLinerspectraisverysmall,indicating that the high density region, located between the NLR and the BLR, is also small. The results show that shocks play an important role, even if a photoionizing flux is present. On average, higher than cosmic N/H and lower S/H are indicated. The physical characteristics of Seyfert galaxies and of starburst galaxies are conrmed. The satisfactory results obtained interpreting the heteroge- neous observational sample by SUMA strengthen the hypothe- sis that shock signature in AGN spectra is due to cloud motions in galaxies." @default.
- W2115698380 created "2016-06-24" @default.
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- W2115698380 date "1997-07-01" @default.
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- W2115698380 title "Line spectra of Liners. The contribution of the different ionization mechanisms" @default.
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