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

Authors

  • T. Kajikawa Kyoto Sangyo University, Koyama Astronomical Observatory
  • A. Arai Kyoto Sangyo University, Koyama Astronomical Observatory
  • M. Nagashima Kyoto Sangyo University, Koyama Astronomical Observatory
  • H. Kawakita Kyoto Sangyo University, Koyama Astronomical Observatory
  • M. Yamanaka Hiroshima University Kyoto University Konan University
  • K. Kawabata Hiroshima University
  • S. Kiyota

DOI:

https://doi.org/10.14311/APP.2015.02.0242

Abstract

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.

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Published

2015-02-23

How to Cite

Kajikawa, T., Arai, A., Nagashima, M., Kawakita, H., Yamanaka, M., Kawabata, K., & Kiyota, S. (2015). Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase. Acta Polytechnica CTU Proceedings, 2(1), 242–245. https://doi.org/10.14311/APP.2015.02.0242

Issue

Vol. 2 No. 1 (2015): THE GOLDEN AGE OF CATACLYSMIC VARIABLES AND RELATED OBJECTS - II

Section

Articles