Astronomy and Astrophysics – Astrophysics – Solar and Stellar Astrophysics
Scientific paper
2010-09-04
Astronomy and Astrophysics
Astrophysics
Solar and Stellar Astrophysics
in press in New Astronomy
Scientific paper
The photometric and spectroscopic evolution of the He/N and very fast Nova Cyg 2008 N2 (V2491 Cyg) is studied in detail. A primary maximum was reached at V=7.45 +/-0.05 on April 11.37 (+/-0.1) 2008 UT, followed by a smooth decline characterized by t2(V)=4.8 days, and then a second maximum was attained at V=9.49 +/-0.03, 14.5 days after the primary one. This is the only third nova to have displayed a secondary maximum, after V2362 Cyg and V1493 Aql. The development and energetics of the secondary maximum is studied in detail. The smooth decline that followed was accurately monitored until day +144 when the nova was 8.6 mag fainter than maximum brightness, well into its nebular phase, with its line and continuum emissivity declining as t-3. The reddening affecting the nova was E(B-V)=0.23 +/-0.01, and the distance of 14 kpc places the nova at a height above the galactic plane of 1.1 kpc, larger than typical for He/N novae. The expansion velocity of the bulk of ejecta was 2000 km/sec, with complex emission profiles and weak P-Cyg absorptions during the optically thick phase, and saddle-like profiles during the nebular phase. Photo-ionization analysis of the emission line spectrum indicates that the mass ejected by the outburst was 5.3 10(-6) Msun and the mass fractions to be X=0.573, Y=0.287, Z=0.140, with those of individual elements being N=0.074, O=0.049, Ne=0.015. The metallicity of the accreted material was [Fe/H]=-0.25, in line with ambient value at the nova galacto-centric distance. Additional spectroscopic and photometric observations at days +477 and +831 show the nova returned to the brightness level of the progenitor and to have resumed the accretion onto the white dwarf.
Cherini G.
Dallaporta Sandrine
Munari Ulisse
Siviero Alessandro
Tomasella Lina
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