JpGU-AGU Joint Meeting 2017

Presentation information

[JJ] Poster

P (Space and Planetary Sciences) » P-PS Planetary Sciences

[P-PS09] [JJ] Origin and evolution of materials in space

Mon. May 22, 2017 5:15 PM - 6:30 PM Poster Hall (International Exhibition Hall HALL7)

[PPS09-P07] Mid-infrared observations of the dust-forming classical nova V2676 Oph with Subaru/COMICS

Hideyo Kawakita1, *Takafumi Ootsubo2, Akira Arai1, Shinnaka Yoshiharu3, Masayoshi Nagashima (1.Koyama Astronomical Observatory, Kyoto Sangyo University, 2.Graduate School of Arts and Sciences, University of Tokyo, 3.National Astronomical Observatory of Japan)

Keywords:nova, dust, infrared

A dust-forming nova V2676 Oph (discovered in Mar 2012) was the first nova to provide evidence of both C2 and CN molecules during its near-maximum phase and evidence of CO molecules during its early decline phase (Nagashima et al. 2014). The derived carbon- and nitrogen-isotopic ratios in the nova (Kawakita et al. 2015) are consistent with that the nova explosion was hosted by a CO-rich white dwarf (WD) star. To confirm a type of the hosting WD (CO-rich or ONe-rich), we performed the mid-infrared imaging and low-resolution spectroscopic observations of V2676 Oph with COMICS mounted on the Subaru telescope in June 2013 and May 2014 (482 days and 782 days respectively after its discovery). No clear [Ne II] emission line at 12.8 micron was observed. Based on the absence of [Ne II] emission, the WD hosting V2676 Oph is considered a CO-rich WD. Both types of dust grain, carbon-rich and oxygen- rich, were detected on both dates, although this nova is considered as a Carbon-rich (C/O > 1) based on the presence of C2 observed earlier. The 11.4 micron unidentified infrared emission was also detected on these dates. Non-equilibrium processes are likely to be responsible for the grain formation in the nova.