In our investigation of the region of formation of the Fe II emission lines in RR Tel, we have applied the SAC method to the optical Fe II emission line fluxes measured by Crawford et al. (1999). It is possible to determine physical parameters of the line emitting region, because of the presence both of lines with large and much smaller optical thicknesses. The values we obtained, given in Tables 3 and 4, are limits in most cases. The upper limit to the excitation temperature of the metastable levels in the permitted line region of 6600 K, is close to the value of this temperature in the forbidden line region. Other excitation temperature limits corresponding to level population ratios were also found. The permitted lines are formed in a region with a radius between 1.8x10e12 cm and 1.6x10e14 cm, while the forbidden lines are formed in a region with a minimum radius of 5.3x10e12 cm. The populations of the lower levels of the permitted lines indicate a minimum column density of Fe+ of 3.0x10e18 atoms/cm2 and, by assuming cosmic abundances, to a minimum column density of 7.5x10e22 atoms/cm2 for H. If we assume a minimum radius of 1.0x10e14 cm, which is supposed to be that of dust condensation of the cool Mira component of this symbiotic binary, a minimum mass loss rate of 3.5x10e6 Mo/yr is found. Our results support a model according to which both the permitted and the forbidden lines are formed in the wind of the cool Mira component above the regions where absorption by dust is important. The forbidden and the permitted lines are not formed in quite the same region, the former being most probably formed further out in the part of an accelerated wind which is ionized by the hot component.
The Region of feii emission line formation of the Symbiotic nova RR Telescopii
2002
Abstract
In our investigation of the region of formation of the Fe II emission lines in RR Tel, we have applied the SAC method to the optical Fe II emission line fluxes measured by Crawford et al. (1999). It is possible to determine physical parameters of the line emitting region, because of the presence both of lines with large and much smaller optical thicknesses. The values we obtained, given in Tables 3 and 4, are limits in most cases. The upper limit to the excitation temperature of the metastable levels in the permitted line region of 6600 K, is close to the value of this temperature in the forbidden line region. Other excitation temperature limits corresponding to level population ratios were also found. The permitted lines are formed in a region with a radius between 1.8x10e12 cm and 1.6x10e14 cm, while the forbidden lines are formed in a region with a minimum radius of 5.3x10e12 cm. The populations of the lower levels of the permitted lines indicate a minimum column density of Fe+ of 3.0x10e18 atoms/cm2 and, by assuming cosmic abundances, to a minimum column density of 7.5x10e22 atoms/cm2 for H. If we assume a minimum radius of 1.0x10e14 cm, which is supposed to be that of dust condensation of the cool Mira component of this symbiotic binary, a minimum mass loss rate of 3.5x10e6 Mo/yr is found. Our results support a model according to which both the permitted and the forbidden lines are formed in the wind of the cool Mira component above the regions where absorption by dust is important. The forbidden and the permitted lines are not formed in quite the same region, the former being most probably formed further out in the part of an accelerated wind which is ionized by the hot component.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
