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The Korean Astronomical Society (한국천문학회)
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INFRARED OBSERVATIONS OF DUST AROUND HELIUM NOVA V445 PUPPIS

  • Shimamoto, Sayaka (Department of Astronomy, Graduate School of Science, The University of Tokyo) ;
  • Sakon, Itsuki (Department of Astronomy, Graduate School of Science, The University of Tokyo) ;
  • Onaka, Takashi (Department of Astronomy, Graduate School of Science, The University of Tokyo) ;
  • Usui, Fumihiko (Department of Astronomy, Graduate School of Science, The University of Tokyo) ;
  • Ootsubo, Takafumi (Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo) ;
  • Doi, Yasuo (Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo) ;
  • Ohsawa, Ryou (Department of Astronomy, Graduate School of Science, The University of Tokyo) ;
  • Ishihara, Daisuke (Graduate School of Science, Nagoya University)
  • Received : 2016.02.29
  • Accepted : 2016.10.27
  • Published : 2017.03.31
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Abstract

We detected bright mid- to far-infrared emission from the helium nova V445 Puppis in the AKARI all-sky survey data taken in 2006. Assuming an optically thin condition, we decomposed the spectral energy distribution (SED) of V445 Puppis in October 2006 by model fitting and found that the SED can be explained by a combination of cold amorphous carbon (125 K and the mass of $4.5^{+6.6}_{-2.7}{\times}10^{-4}M_{\odot}$) and warm amorphous carbon (250 K and the mass of $1.8^{+1.0}_{-0.5}{\times}10^{-5}M_{\odot}$). Assuming that the former is pre-existing dust formed in the past nova outbursts and the latter is newly formed dust in December 2000's nova wind, this result suggests that the amount of dust formed around V445 Puppis in a single outburst is larger than $10^{-5}M_{\odot}$, which is larger than those in any other classical novae ever reported.

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References

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