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 | |
| Publication status | Published - Jan 1 2013 |
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All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
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Morpho-kinematical modelling of Nova Eridani 2009 (KT Eri). / Ribeiro, V. A.R.M.; Bode, M. F.; Darnley, M. J.; Barnsley, R. M.; Munari, U.; Harman, D. J.
In: Monthly Notices of the Royal Astronomical Society, Vol. 433, No. 3, 01.01.2013, p. 1991-1996.Research output: Contribution to journal › Article
TY - JOUR
T1 - Morpho-kinematical modelling of Nova Eridani 2009 (KT Eri)
AU - Ribeiro, V. A.R.M.
AU - Bode, M. F.
AU - Darnley, M. J.
AU - Barnsley, R. M.
AU - Munari, U.
AU - Harman, D. J.
PY - 2013/1/1
Y1 - 2013/1/1
N2 - 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.
AB - 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.
UR - http://www.scopus.com/inward/record.url?scp=84896693743&partnerID=8YFLogxK
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U2 - 10.1093/mnras/stt856
DO - 10.1093/mnras/stt856
M3 - Article
VL - 433
SP - 1991
EP - 1996
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 3
ER -