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Title: MID-INFRARED SPECTROSCOPIC OBSERVATIONS OF THE DUST-FORMING CLASSICAL NOVA V2676 OPH

Abstract

The dust-forming nova V2676 Oph is unique in that it was the first nova to provide evidence of C{sub 2} and CN molecules during its near-maximum phase and evidence of CO molecules during its early decline phase. Observations of this nova have revealed the slow evolution of its lightcurves and have also shown low isotopic ratios of carbon ({sup 12}C/{sup 13}C) and nitrogen ({sup 14}N/{sup 15}N) in its envelope. These behaviors indicate that the white dwarf (WD) star hosting V2676 Oph is a CO-rich WD rather than an ONe-rich WD (typically larger in mass than the former). We performed mid-infrared spectroscopic and photometric observations of V2676 Oph in 2013 and 2014 (respectively 452 and 782 days after its discovery). No significant [Ne ii] emission at 12.8 μ m was detected at either epoch. These provided evidence for a CO-rich WD star hosting V2676 Oph. Both carbon-rich and oxygen-rich grains were detected in addition to an unidentified infrared feature at 11.4 μ m originating from polycyclic aromatic hydrocarbon molecules or hydrogenated amorphous carbon grains in the envelope of V2676 Oph.

Authors:
; ;  [1];  [2];  [3]
  1. Koyama Astronomical Observatory, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555 (Japan)
  2. Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo, 3-8-1 Komaba, Meguro-ku, Tokyo 153-8902 (Japan)
  3. Department of Physics, Faculty of Science, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto 603-8555 (Japan)
Publication Date:
OSTI Identifier:
22666286
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astronomical Journal (Online); Journal Volume: 153; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTROPHYSICS; CARBON 12; CARBON 13; CARBON MONOXIDE; CARBON NITRIDES; COSMIC DUST; COSMOCHEMISTRY; CYANIDES; HYDROGENATION; INTERMEDIATE INFRARED RADIATION; ISOTOPE RATIO; MOLECULES; NITROGEN 14; NITROGEN 15; NOVAE; POLYCYCLIC AROMATIC HYDROCARBONS; WHITE DWARF STARS

Citation Formats

Kawakita, Hideyo, Arai, Akira, Shinnaka, Yoshiharu, Ootsubo, Takafumi, and Nagashima, Masayoshi, E-mail: kawakthd@cc.kyoto-su.ac.jp. MID-INFRARED SPECTROSCOPIC OBSERVATIONS OF THE DUST-FORMING CLASSICAL NOVA V2676 OPH. United States: N. p., 2017. Web. doi:10.3847/1538-3881/153/2/74.
Kawakita, Hideyo, Arai, Akira, Shinnaka, Yoshiharu, Ootsubo, Takafumi, & Nagashima, Masayoshi, E-mail: kawakthd@cc.kyoto-su.ac.jp. MID-INFRARED SPECTROSCOPIC OBSERVATIONS OF THE DUST-FORMING CLASSICAL NOVA V2676 OPH. United States. doi:10.3847/1538-3881/153/2/74.
Kawakita, Hideyo, Arai, Akira, Shinnaka, Yoshiharu, Ootsubo, Takafumi, and Nagashima, Masayoshi, E-mail: kawakthd@cc.kyoto-su.ac.jp. Wed . "MID-INFRARED SPECTROSCOPIC OBSERVATIONS OF THE DUST-FORMING CLASSICAL NOVA V2676 OPH". United States. doi:10.3847/1538-3881/153/2/74.
@article{osti_22666286,
title = {MID-INFRARED SPECTROSCOPIC OBSERVATIONS OF THE DUST-FORMING CLASSICAL NOVA V2676 OPH},
author = {Kawakita, Hideyo and Arai, Akira and Shinnaka, Yoshiharu and Ootsubo, Takafumi and Nagashima, Masayoshi, E-mail: kawakthd@cc.kyoto-su.ac.jp},
abstractNote = {The dust-forming nova V2676 Oph is unique in that it was the first nova to provide evidence of C{sub 2} and CN molecules during its near-maximum phase and evidence of CO molecules during its early decline phase. Observations of this nova have revealed the slow evolution of its lightcurves and have also shown low isotopic ratios of carbon ({sup 12}C/{sup 13}C) and nitrogen ({sup 14}N/{sup 15}N) in its envelope. These behaviors indicate that the white dwarf (WD) star hosting V2676 Oph is a CO-rich WD rather than an ONe-rich WD (typically larger in mass than the former). We performed mid-infrared spectroscopic and photometric observations of V2676 Oph in 2013 and 2014 (respectively 452 and 782 days after its discovery). No significant [Ne ii] emission at 12.8 μ m was detected at either epoch. These provided evidence for a CO-rich WD star hosting V2676 Oph. Both carbon-rich and oxygen-rich grains were detected in addition to an unidentified infrared feature at 11.4 μ m originating from polycyclic aromatic hydrocarbon molecules or hydrogenated amorphous carbon grains in the envelope of V2676 Oph.},
doi = {10.3847/1538-3881/153/2/74},
journal = {Astronomical Journal (Online)},
number = 2,
volume = 153,
place = {United States},
year = {Wed Feb 01 00:00:00 EST 2017},
month = {Wed Feb 01 00:00:00 EST 2017}
}