Rise and fall of the dust shell of the classical nova V339 Delphini
We present infrared spectroscopy of the classical nova V339 Del, obtained over an ∼2-yr period. The infrared emission lines were initially symmetrical, with half width half-maximum velocities of 525 km s−1. In later (t ≳ 77 d, where t is the time from outburst) spectra, however, the lines displayed...
Gespeichert in:
| Hauptverfasser: | , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2017 January 13
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2017, Jahrgang: 466, Heft: 4, Pages: 4221-4238 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stw3334 |
| Online-Zugang: | Verlag, kostenfrei, Volltext: http://dx.doi.org/10.1093/mnras/stw3334
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| Verfasserangaben: | A. Evans, D.P.K. Banerjee, R.D. Gehrz, V. Joshi, N.M. Ashok, V.a.R.M. Ribeiro, M.J. Darnley, C.E. Woodward, D. Sand, G.H. Marion, T.R. Diamond, S.P.S. Eyres, R.M. Wagner, L.A. Helton, S. Starrfield, D.P. Shenoy, J. Krautter, W.D. Vacca and M.T. Rushton |
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| 245 | 1 | 0 | |a Rise and fall of the dust shell of the classical nova V339 Delphini |c A. Evans, D.P.K. Banerjee, R.D. Gehrz, V. Joshi, N.M. Ashok, V.a.R.M. Ribeiro, M.J. Darnley, C.E. Woodward, D. Sand, G.H. Marion, T.R. Diamond, S.P.S. Eyres, R.M. Wagner, L.A. Helton, S. Starrfield, D.P. Shenoy, J. Krautter, W.D. Vacca and M.T. Rushton |
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| 520 | |a We present infrared spectroscopy of the classical nova V339 Del, obtained over an ∼2-yr period. The infrared emission lines were initially symmetrical, with half width half-maximum velocities of 525 km s−1. In later (t ≳ 77 d, where t is the time from outburst) spectra, however, the lines displayed a distinct asymmetry, with a much stronger blue wing, possibly due to obscuration of the receding component by dust. Dust formation commenced at approximately day 34.75 at a condensation temperature of 1480 ± 20 K, consistent with graphitic carbon. Thereafter, the dust temperature declined with time as Td ∝ t−0.346, also consistent with graphitic carbon. The mass of dust initially rose, as a result of an increase in grain size and/or number, peaked at approximately day 100, and then declined precipitously. This decline was most likely caused by grain shattering due to electrostatic stress after the dust was exposed to X-radiation. The appendix summarizes Planck means for carbon and the determination of grain mass and radius for a carbon dust shell. | ||
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