A three-dimensional view of the remnant of Nova Persei 1901 (GK Per)
Entity
UAM. Departamento de Física TeóricaPublisher
The American Astronomical SocietyDate
2012-12-10Citation
10.1088/0004-637X/761/1/34
The Astrophysical Journal 761.1 (2012): 34
ISSN
0004-637X (print); 1538-4357 (online)DOI
10.1088/0004-637X/761/1/34Funded by
The work of R.L.M.C. and M.S.G. has been supported by the Spanish Ministry of Science and Innovation (MICINN) under the grantAYA2007-66804. P.R.G. is supported by a Ramón y Cajal fellowship (RYC–2010–05762). E.V. acknowledges the support provided by the Spanish MICINN under grant AYA2010-20630 and to the Marie Curie FP7-People-RG268111. This work was partially supported by the Spanish MICINN under the CONSOLIDER–INGENIO 2010 Program, through the grants “Molecular Astrophysics: The Herschel andALMAEraASTROMOL” (CSD2009–00038) and “First Science with the GTC” (CSD2006–00070). T.L., K.V., and I.K. acknowledge the support of the Estonian Ministry for Education and Science.Project
info:eu-repo/grantAgreement/EC/FP7/268111Editor's Version
http://dx.doi.org/10.1088/0004-637X/761/1/34Subjects
ISM: jets and outflows; Novae, cataclysmic variables; Stars: individual (GK Persei); Stars: winds, outflows; FísicaNote
The Astrophysical Journal 761.1 (2012): 34 reproduced by permission of the AASRights
© 2012. The American Astronomical Society.Abstract
We present a kinematical study of the optical ejecta of GK Per. It is based on proper-motion measurements of 282 knots from 20 images spanning 25 years. Doppler shifts are also computed for 217 knots. The combination of proper motions and radial velocities allows a unique three-dimensional view of the ejecta to be obtained. The main results are as follows: (1) the outflow is a thick shell in which knots expand with a significant range of velocities, mostly between 600 and 1000 km s-1, (2) kinematical ages indicate that knots have suffered only a modest deceleration since their ejection a century ago, (3) no evidence for anisotropy in the expansion rate is found, (4) velocity vectors are generally aligned along the radial direction, but a symmetric pattern of non-radial velocities is also observed at specific directions, and (5) the total Hα+[N II] flux has been linearly decreasing at a rate of 2.6% per year in the past decade. The eastern nebular side is fading at a slower rate than the western side. Some of the knots were displayed a rapid change of brightness during the 2004-2011 period. Over a longer timescale, a progressive circularization and homogenization of the nebula are taking place; (6) a kinematic distance of 400 ± 30 pc is determined. These results raise some problems with the previous interpretations of the evolution of GK Per. In particular, the idea of a strong interaction of the outflow with the surrounding medium in the southwest quadrant is not supported by our data.
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Google Scholar:Liimets, Tiina
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Corradi, Romano L M
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Santander-Garćia, Miguel
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Villaver Sobrino, Eva Gloria
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Rodríguez-Gil, Pablo
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Verro, K.
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Kolka, Indrek
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