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Title: ORIGINS OF ABSORPTION SYSTEMS OF CLASSICAL NOVA V2659 CYG (NOVA CYG 2014)

Abstract

We report on high-dispersion spectroscopy results of a classical nova V2659 Cyg (Nova Cyg 2014) that are taken 33.05 days after the V -band maximum. The spectrum shows two distinct blueshifted absorption systems originating from H i, Fe ii, Ca ii, etc. The radial velocities of the absorption systems are −620 km s{sup −1}, and −1100 to −1500 km s{sup −1}. The higher velocity component corresponds to the P-Cygni absorption features frequently observed in low-resolution spectra. Much larger numbers of absorption lines are identified at the lower velocity. These mainly originate from neutral or singly ionized Fe-peak elements (Fe i, Ti ii, Cr ii, etc.). Based on the results of our spectroscopic observations, we discuss the structure of the ejecta of V2659 Cyg. We conclude that the low- and high-velocity components are likely to be produced by the outflow wind and the ballistic nova ejecta, respectively.

Authors:
;  [1];  [2];  [3]
  1. Koyama Astronomical Observatory, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555 (Japan)
  2. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan)
  3. Subaru Telescope, National Astronomical Observatory of Japan, 650 North A’ohoku Place, Hilo, Hawaii 96720 (United States)
Publication Date:
OSTI Identifier:
22667358
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 830; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION; DISPERSIONS; ELEMENT ABUNDANCE; NOVAE; RADIAL VELOCITY; RESOLUTION; SPECTRA; STELLAR WINDS

Citation Formats

Arai, A., Kawakita, H., Shinnaka, Y., and Tajitsu, A., E-mail: arai6a@cc.kyoto-su.ac.jp. ORIGINS OF ABSORPTION SYSTEMS OF CLASSICAL NOVA V2659 CYG (NOVA CYG 2014). United States: N. p., 2016. Web. doi:10.3847/0004-637X/830/1/30.
Arai, A., Kawakita, H., Shinnaka, Y., & Tajitsu, A., E-mail: arai6a@cc.kyoto-su.ac.jp. ORIGINS OF ABSORPTION SYSTEMS OF CLASSICAL NOVA V2659 CYG (NOVA CYG 2014). United States. doi:10.3847/0004-637X/830/1/30.
Arai, A., Kawakita, H., Shinnaka, Y., and Tajitsu, A., E-mail: arai6a@cc.kyoto-su.ac.jp. Mon . "ORIGINS OF ABSORPTION SYSTEMS OF CLASSICAL NOVA V2659 CYG (NOVA CYG 2014)". United States. doi:10.3847/0004-637X/830/1/30.
@article{osti_22667358,
title = {ORIGINS OF ABSORPTION SYSTEMS OF CLASSICAL NOVA V2659 CYG (NOVA CYG 2014)},
author = {Arai, A. and Kawakita, H. and Shinnaka, Y. and Tajitsu, A., E-mail: arai6a@cc.kyoto-su.ac.jp},
abstractNote = {We report on high-dispersion spectroscopy results of a classical nova V2659 Cyg (Nova Cyg 2014) that are taken 33.05 days after the V -band maximum. The spectrum shows two distinct blueshifted absorption systems originating from H i, Fe ii, Ca ii, etc. The radial velocities of the absorption systems are −620 km s{sup −1}, and −1100 to −1500 km s{sup −1}. The higher velocity component corresponds to the P-Cygni absorption features frequently observed in low-resolution spectra. Much larger numbers of absorption lines are identified at the lower velocity. These mainly originate from neutral or singly ionized Fe-peak elements (Fe i, Ti ii, Cr ii, etc.). Based on the results of our spectroscopic observations, we discuss the structure of the ejecta of V2659 Cyg. We conclude that the low- and high-velocity components are likely to be produced by the outflow wind and the ballistic nova ejecta, respectively.},
doi = {10.3847/0004-637X/830/1/30},
journal = {Astrophysical Journal},
number = 1,
volume = 830,
place = {United States},
year = {Mon Oct 10 00:00:00 EDT 2016},
month = {Mon Oct 10 00:00:00 EDT 2016}
}