Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase
DOI:
https://doi.org/10.14311/APP.2015.02.0242Abstract
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.Downloads
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2015-02-23
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Line Evolution of the Nova V5587 Sgr from Early to Nebula Phase. (2015). Acta Polytechnica CTU Proceedings, 2(1), 242-245. https://doi.org/10.14311/APP.2015.02.0242