Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006rmxac..26r.166a&link_type=abstract
XI IAU Regional Latin American Meeting of Astronomy (Eds. L. Infante & M. Rubio) Revista Mexicana de Astronomía y Astrofísica (S
Astronomy and Astrophysics
Astronomy
Scientific paper
The slow and bright classical nova HR Del 1967 was observed in the optical using GEMINI-NORTH GMOS-IFU in 2002 with a spectral range from 0.4 μm to 1 μm, a resolution of ˜ 300 km/s, and spatial resolution of ˜ 0''.5. Line intensity maps were obtained for Hα +[NII], [OIII] 5007, Hβ and helium lines. The shell showed a bipolar and clumped structure resembling the shell observed in 1998 (Harman and O'Brien 2003). The [OIII] 5007 map showed seven bright knots. Models of the central source, shell and knots spectra were performed using CLOUDY 94 (Ferland et al. 1998) and RA3D (Diaz 2001). Central source spectra were best fitted with a T_{eff} = 60000 K, log(g) = 6 and log(L_*) = 36.6 Rauch atmosphere model. Shell H-density law was modeled using a power law with α parameter -1.2 and mass = 4.1 × 10^{-4} M_&sun;. The knots spectra were fitted as gaussian condensations with ˜ 50000cm^{-3} peak H-density and ˜ 20000cm^{-3} average H-density. HeII 4686 emission was found in the knots. The HeII origin is atributted to projected emission from diffuse matter in front of the knots, hypothesis corroborated by about the same HeII intensity observed outside the knots. Physical parameters of the condensations were obtained from our analysis and helium abundances were recalculated. A peak density contrast N/N_S = 270 was found when compared to the medium outside the knots. Electron temperatures ˜ 9500 K, electron densities ˜ 20000cm^{-3} and helium number abundance ˜ 0.2 were derived. Our results showed a constant helium abundance within a narrow radius range which is consistent with impulsive ejection (Kato and Hachisu 1994).
Augusto A.
Díaz Marco
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