The early spectrophotometric evolution of V1186 scorpii (nova scorpii 2004 NO. 1)

G. J. Schwarz, C. E. Woodward, M. F. Bode, A. Evans, S. P. Eyres, T. R. Geballe, R. D. Gehrz, M. A. Greenhouse, L. A. Helton, W. Liller, J. E. Lyke, D. K. Lynch, T. J. O'Brien, R. J. Rudy, R. W. Russell, S. N. Shore, Sumner Starrfield, T. Temim, J. W. Truran, C. C. VenturiniR. M. Wagner, R. E. Williams, R. Zamanov

Research output: Contribution to journalArticle

13 Citations (Scopus)

Abstract

We report optical photometry and optical through mid-infrared spectroscopy of the classical nova V1186 Sco. This slowly developing nova had a complex light curve with multiple secondary peaks similar to those seen in PW Vul. The time to decline 2 mag, t2, was 20 days, but the erratic nature of the light curve makes determination of intrinsic properties based on the decline time (e.g., luminosity) problematic, and the often-cited relationship of maximum magnitude versus the rate of decay of the light curve of Della Valle & Livio fails to yield a plausible distance. Spectra covering 0.35-35 μm were obtained in two separate epochs during the first year of outburst. The first set of spectra, taken about 2 months after visible maximum, are typical of a CO-type nova with narrow-line emission from H I, Fe II, O I, and He I. Later data, obtained between 260 and 380 days after maximum, reveal an emerging nebular spectrum. Spitzer spectra show weakening hydrogen recombination emission with the emergence of [Ne II] (12.81 μm) as the strongest line. Strong emission from [Ne III] (15.56 μm) is also detected. Photoionization models with low effective temperature sources and only marginal neon enhancement (Ne ∼ 1.3 Ne⊙) are consistent with these IR fine-structure neon lines indicating that V1186 Sco did not occur on a ONeMg white dwarf. In contrast, the slow and erratic light-curve evolution, spectral development, and photoionization analysis of the ejecta imply that the outburst occurred on a low-mass CO white dwarf. We note that this is the first time strong [Ne II] lines have been detected so early in the outburst of a CO nova and suggest that the presence of mid-infrared neon lines is not directly indicative of a ONeMg nova event.

Original languageEnglish (US)
Pages (from-to)516-526
Number of pages11
JournalAstronomical Journal
Volume134
Issue number2
StatePublished - Aug 2007

Fingerprint

light curve
neon
outburst
erratic
photoionization
hydrogen recombinations
ejecta
infrared spectroscopy
recombination
photometry
emerging
coverings
fine structure
luminosity
time measurement
hydrogen
augmentation
decay
temperature

Keywords

  • Stars: dwarf novae
  • Stars: individual (V1186 Sco)

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Schwarz, G. J., Woodward, C. E., Bode, M. F., Evans, A., Eyres, S. P., Geballe, T. R., ... Zamanov, R. (2007). The early spectrophotometric evolution of V1186 scorpii (nova scorpii 2004 NO. 1). Astronomical Journal, 134(2), 516-526.

The early spectrophotometric evolution of V1186 scorpii (nova scorpii 2004 NO. 1). / Schwarz, G. J.; Woodward, C. E.; Bode, M. F.; Evans, A.; Eyres, S. P.; Geballe, T. R.; Gehrz, R. D.; Greenhouse, M. A.; Helton, L. A.; Liller, W.; Lyke, J. E.; Lynch, D. K.; O'Brien, T. J.; Rudy, R. J.; Russell, R. W.; Shore, S. N.; Starrfield, Sumner; Temim, T.; Truran, J. W.; Venturini, C. C.; Wagner, R. M.; Williams, R. E.; Zamanov, R.

In: Astronomical Journal, Vol. 134, No. 2, 08.2007, p. 516-526.

Research output: Contribution to journalArticle

Schwarz, GJ, Woodward, CE, Bode, MF, Evans, A, Eyres, SP, Geballe, TR, Gehrz, RD, Greenhouse, MA, Helton, LA, Liller, W, Lyke, JE, Lynch, DK, O'Brien, TJ, Rudy, RJ, Russell, RW, Shore, SN, Starrfield, S, Temim, T, Truran, JW, Venturini, CC, Wagner, RM, Williams, RE & Zamanov, R 2007, 'The early spectrophotometric evolution of V1186 scorpii (nova scorpii 2004 NO. 1)', Astronomical Journal, vol. 134, no. 2, pp. 516-526.
Schwarz GJ, Woodward CE, Bode MF, Evans A, Eyres SP, Geballe TR et al. The early spectrophotometric evolution of V1186 scorpii (nova scorpii 2004 NO. 1). Astronomical Journal. 2007 Aug;134(2):516-526.
Schwarz, G. J. ; Woodward, C. E. ; Bode, M. F. ; Evans, A. ; Eyres, S. P. ; Geballe, T. R. ; Gehrz, R. D. ; Greenhouse, M. A. ; Helton, L. A. ; Liller, W. ; Lyke, J. E. ; Lynch, D. K. ; O'Brien, T. J. ; Rudy, R. J. ; Russell, R. W. ; Shore, S. N. ; Starrfield, Sumner ; Temim, T. ; Truran, J. W. ; Venturini, C. C. ; Wagner, R. M. ; Williams, R. E. ; Zamanov, R. / The early spectrophotometric evolution of V1186 scorpii (nova scorpii 2004 NO. 1). In: Astronomical Journal. 2007 ; Vol. 134, No. 2. pp. 516-526.
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AU - Schwarz, G. J.

AU - Woodward, C. E.

AU - Bode, M. F.

AU - Evans, A.

AU - Eyres, S. P.

AU - Geballe, T. R.

AU - Gehrz, R. D.

AU - Greenhouse, M. A.

AU - Helton, L. A.

AU - Liller, W.

AU - Lyke, J. E.

AU - Lynch, D. K.

AU - O'Brien, T. J.

AU - Rudy, R. J.

AU - Russell, R. W.

AU - Shore, S. N.

AU - Starrfield, Sumner

AU - Temim, T.

AU - Truran, J. W.

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N2 - We report optical photometry and optical through mid-infrared spectroscopy of the classical nova V1186 Sco. This slowly developing nova had a complex light curve with multiple secondary peaks similar to those seen in PW Vul. The time to decline 2 mag, t2, was 20 days, but the erratic nature of the light curve makes determination of intrinsic properties based on the decline time (e.g., luminosity) problematic, and the often-cited relationship of maximum magnitude versus the rate of decay of the light curve of Della Valle & Livio fails to yield a plausible distance. Spectra covering 0.35-35 μm were obtained in two separate epochs during the first year of outburst. The first set of spectra, taken about 2 months after visible maximum, are typical of a CO-type nova with narrow-line emission from H I, Fe II, O I, and He I. Later data, obtained between 260 and 380 days after maximum, reveal an emerging nebular spectrum. Spitzer spectra show weakening hydrogen recombination emission with the emergence of [Ne II] (12.81 μm) as the strongest line. Strong emission from [Ne III] (15.56 μm) is also detected. Photoionization models with low effective temperature sources and only marginal neon enhancement (Ne ∼ 1.3 Ne⊙) are consistent with these IR fine-structure neon lines indicating that V1186 Sco did not occur on a ONeMg white dwarf. In contrast, the slow and erratic light-curve evolution, spectral development, and photoionization analysis of the ejecta imply that the outburst occurred on a low-mass CO white dwarf. We note that this is the first time strong [Ne II] lines have been detected so early in the outburst of a CO nova and suggest that the presence of mid-infrared neon lines is not directly indicative of a ONeMg nova event.

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