Spectral evolution of the extremely fast classical nova V838 Herculis

Issue		A&A Volume 516, June-July 2010


Article Number		A54
Number of page(s)		5
Section		Stellar atmospheres
DOI		http://dx.doi.org/10.1051/0004-6361/200913287
Published online		24 June 2010

A&A 516, A54 (2010)

Spectral evolution of the extremely fast classical nova V838 Herculis

T. Iijima¹ and A. Cassatella²^,3

¹ Astronomical Observatory of Padova, Asiago Section, Osservatorio Astrofisico, 36012 Asiago (Vi), Italy e-mail: takashi.iijima@oapd.inaf.it
² INAF, Istituto di Fisica dello Spazio Interplanetario, via del Fosso del Cavaliere 100, 00133 Roma, Italy
³ Departmento de Astrofisica, Facultad de Fisica, Universidad Complutense, 28040 Madrid, Spain

Received: 12 September 2009
Accepted: 28 March 2010

Abstract

Spectral evolution of nova V838 Her 1991 was monitored at Asiago Astrophysical Observatory from 1991 March 31 to July 2. The spectra in the early decline stage showed emission lines of H I, He I, He II, N II, N III, C II, C III, C IV, Si II, [S III], [Ne III], and Fe II, where some identifications are different from those reported in the previous works. The emission lines of [Ne III] and carbon ions were unusually intense. New emission peaks appeared at the blue-ward edges of the emission lines of H I and He I about one week after maximum luminosity. It seems that a new clump of gas was ejected at that time along the line of sight towards us. The helium abundance is estimated at N(He) = 0.11 ± 0.01. 

Key words: stars: individual: V838 Her / novae, cataclysmic variables / ISM: general

© ESO, 2010

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