Acta Polytechnica CTU Proceedings (Feb 2015)

Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase

  • T. Kajikawa,
  • A. Arai,
  • M. Nagashima,
  • H. Kawakita,
  • M. Yamanaka,
  • K. Kawabata,
  • S. Kiyota

DOI
https://doi.org/10.14311/APP.2015.02.0242
Journal volume & issue
Vol. 2, no. 1
pp. 242 – 245

Abstract

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The spectral evolution of the nova V5587 Sgr has been monitored at Koyama Astronomical Observatory and Higashi-Hiroshima Observatory, Japan, from the early to nebula phase. The nova rebrightened several times. The spectra during the early phase showed emission lines of H α, H β, O I, He I, He II, N II, Fe II. Nova V5587 Sgr is classified into the Fe II type. The helium abundance of the nova is estimated as N(He)/N(H) = 0.134 ± 0.09. The light curve, the spectral evolution, and the helium abundance in V5587 Sgr are similar to those of the nova PW Vul.