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The Early Ultraviolet Evolution of the ONeMg Nova V382 Velorum 1999 | | S. N. Shore
; G. Schwarz
; H. E. Bond
; R. A. Downes
; S. Starrfield
; A. Evans
; R. D. Gehrz
; P. H. Hauschildt
; J. Krautter
; C. E. Woodward
; | | Date: |
21 Dec 2002 | | Subject: | astro-ph | | Affiliation: | IUSB, Univ. of Pisa), G. Schwarz (Steward Obs.), H. E. Bond (STScI), R. A. Downes (STScI), S. Starrfield (ASU), A. Evans (Keele), R. D. Gehrz (Univ. Minn.), P. H. Hauschildt (Hamburg Obs.), J. Krautter (Heidelberg Obs.), C. E. Woodward (Univ. Minn. | | Abstract: | We present a multiwavelength study of the ONeMg Galactic nova V382 Velorum 1999 using HST/STIS and FUSE ultraviolet spectra and comparisons with published groundbased optical spectra. We find a close match to the basic phenomenology of another well-studied ONeMg nova, V1974 Cygni (Nova Cygni 1992), in particular to the spectral development through the start of the nebular phase. Following an ``iron curtain’’ phase, the nova proceeded through a stage of P Cygni line profiles on all important resonance lines, as in many ONeMg novae and unlike the CO class. Emergent emission lines displayed considerable structure, as seen in V1974 Cyg, indicating fragmentation of the ejecta at the earliest stages of the outburst. Analysis and modeling of our ultraviolet spectra suggest that 4 - 5 $ imes$ 10$^{-4}$M$_{odot}$ of material was ejected and that the distance to the nova is $simeq 2.5$ kpc. Relative to solar values, we find the following abundances: He = 1.0, C = 0.6$pm$0.3, N = 17$pm$4, O = 3.4$pm$0.3, Ne = 17$pm$3, Mg = 2.6$pm$0.1, Al = 21$pm$2, and Si = 0.5$pm$0.3. Finally, we briefly draw comparisons with Nova LMC 2000, another ONeMg nova, for which similar data were obtained with HST and FUSE. | | Source: | arXiv, astro-ph/0301415 | | Services: | Forum | Review | PDF | Favorites | |
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