Morpho-kinematical modelling of Nova Eridani 2009 (KT Eri)

V. A.R.M. Ribeiro; M. F. Bode; M. J. Darnley; R. M. Barnsley; U. Munari; D. J. Harman

doi:10.1093/mnras/stt856

Morpho-kinematical modelling of Nova Eridani 2009 (KT Eri)

V. A.R.M. Ribeiro, M. F. Bode, M. J. Darnley, R. M. Barnsley, U. Munari, D. J. Harman

Physics & Astronomy

Research output: Contribution to journal › Article › peer-review

21 Citations (Scopus)

Abstract

Modelling the morphology of a nova outburst provides valuable information on the shaping mechanism in operation at early stages following the outburst. We performed morpho-kinematical studies, using SHAPE, of the evolution of the Ha line profile following the outburst of the nova KT Eridani. We applied a series of geometries in order to determine the morphology of the system. The best-fitting morphology was that of a dumbbell structure with a ratio between the major to minor axis of 4:1, with an inclination angle of 58 _-7⁺⁶ deg and a maximum expansion velocity of 2800 ± 200 km s^-1. Although, we found that it is possible to define the overall structure of the system, the radial density profile of the ejecta is much more difficult to disentangle. Furthermore, morphology implied here may also be consistent with the presence of an evolved secondary as suggested by various authors.

Original language	English
Pages (from-to)	1991-1996
Number of pages	6
Journal	Monthly Notices of the Royal Astronomical Society
Volume	433
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stt856
Publication status	Published - Jan 1 2013

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/mnras/stt856

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abstract = "Modelling the morphology of a nova outburst provides valuable information on the shaping mechanism in operation at early stages following the outburst. We performed morpho-kinematical studies, using SHAPE, of the evolution of the Ha line profile following the outburst of the nova KT Eridani. We applied a series of geometries in order to determine the morphology of the system. The best-fitting morphology was that of a dumbbell structure with a ratio between the major to minor axis of 4:1, with an inclination angle of 58 -7+6 deg and a maximum expansion velocity of 2800 ± 200 km s-1. Although, we found that it is possible to define the overall structure of the system, the radial density profile of the ejecta is much more difficult to disentangle. Furthermore, morphology implied here may also be consistent with the presence of an evolved secondary as suggested by various authors.",

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AU - Bode, M. F.

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AU - Barnsley, R. M.

AU - Munari, U.

AU - Harman, D. J.

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