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

Ribeiro, VARM, Bode, MF, Darnley, MJ, Barnsley, RM, Munari, U and Harman, DJ (2013) Morpho-kinematical modelling of Nova Eridani 2009 (KT Eri). MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 433 (3). pp. 1991-1996. ISSN 0035-8711

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Modelling the morphology of a nova outburst provides valuable information on the shaping mechanism in operation at early stages following the outburst. We performed morphokinematical studies, using shape, of the evolution of the Hα 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 fit 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+6−7 degrees 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.

Item Type: Article
Additional Information: This is a pre-copyedited, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The version of record Morpho-kinematical modelling of Nova Eridani 2009 (KT Eri), V. A. R. M. Ribeiro1, M. F. Bode, M. J. Darnley, R. M. Barnsley, U. Munari and D. J. Harman. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY Volume:433 Issue:3 Article Published: Jun 8 2013 is available online at:http://dx.doi.org/10.1093/mnras/stt856
Uncontrolled Keywords: 0201 Astronomical And Space Sciences
Subjects: Q Science > QB Astronomy
Divisions: Astrophysics Research Institute
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Date Deposited: 12 Sep 2016 09:44
Last Modified: 04 Sep 2021 12:32
DOI or ID number: 10.1093/mnras/stt856
URI: https://researchonline.ljmu.ac.uk/id/eprint/4133
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