Historical light curve and search for previous outbursts of Nova KT Eridani (2009)

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dc.contributor.authorJurdana-Šepić, R
dc.contributor.authorRibeiro, V A R M
dc.contributor.authorDarnley, M J
dc.contributor.authorMunari, U
dc.contributor.authorBode, M F
dc.date.accessioned2021-10-08T11:01:07Z
dc.date.available2021-10-08T11:01:07Z
dc.date.issued2012
dc.description.abstractContext. Nova Eridani (2009) caught the eye of the nova community due to its fast decline from maximum, which was initially missed, and its subsequent development in the radio and X-ray wavelengths. This system also exhibits properties similar to those of the much smaller class of recurrent novae; themselves potential progenitors of Type Ia Supernovae. Aims. We aim to determine the nature and physical parameters of the KT Eri progenitor system. Methods. We searched the Harvard College Observatory archive plates for the progenitor of KT Eri to determine the nature of the system, particularly the evolutionary stage of the secondary.We used the data obtained to search for any periodic signal and the derived luminosity to estimate a recurrence timescale. Furthermore, by comparing the colours of the quiescent system on a colour-magnitude diagram we may infer the nature of the secondary star. Results. We identified the progenitor system of KT Eri and measured a quiescent magnitude of < B >= 14.7 pm 0.4. No previous outburst was found. However, we suggest that if the nova is recurrent it should be on a timescale of centuries. We find a periodicity at quiescence of 737 days which may arise from reflection effects and/or eclipses in the central binary. The periodicity and the quiescence magnitude of the system suggest that the secondary star is evolved and likely in, or ascending, the Red Giant Branch. A second period is evident at 376 days which has a sinusoidal like light curve. Furthermore, the outburst amplitude of ~ 9 magnitudes is inconsistent with those expected for fast classical novae (~ 17 magnitudes) which may lend further support for an evolved secondary. (Abridged)
dc.identifier.apacitationJurdana-Šepić, R., Ribeiro, V. A. R. M., Darnley, M. J., Munari, U., & Bode, M. F. (2012). Historical light curve and search for previous outbursts of Nova KT Eridani (2009). <i>Astronomy and Astrophysics</i>, 537(4), A34 - 177. http://hdl.handle.net/11427/35088en_ZA
dc.identifier.chicagocitationJurdana-Šepić, R, V A R M Ribeiro, M J Darnley, U Munari, and M F Bode "Historical light curve and search for previous outbursts of Nova KT Eridani (2009)." <i>Astronomy and Astrophysics</i> 537, 4. (2012): A34 - 177. http://hdl.handle.net/11427/35088en_ZA
dc.identifier.citationJurdana-Šepić, R., Ribeiro, V.A.R.M., Darnley, M.J., Munari, U. & Bode, M.F. 2012. Historical light curve and search for previous outbursts of Nova KT Eridani (2009). <i>Astronomy and Astrophysics.</i> 537(4):A34 - 177. http://hdl.handle.net/11427/35088en_ZA
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.ris TY - Journal Article AU - Jurdana-Šepić, R AU - Ribeiro, V A R M AU - Darnley, M J AU - Munari, U AU - Bode, M F AB - Context. Nova Eridani (2009) caught the eye of the nova community due to its fast decline from maximum, which was initially missed, and its subsequent development in the radio and X-ray wavelengths. This system also exhibits properties similar to those of the much smaller class of recurrent novae; themselves potential progenitors of Type Ia Supernovae. Aims. We aim to determine the nature and physical parameters of the KT Eri progenitor system. Methods. We searched the Harvard College Observatory archive plates for the progenitor of KT Eri to determine the nature of the system, particularly the evolutionary stage of the secondary.We used the data obtained to search for any periodic signal and the derived luminosity to estimate a recurrence timescale. Furthermore, by comparing the colours of the quiescent system on a colour-magnitude diagram we may infer the nature of the secondary star. Results. We identified the progenitor system of KT Eri and measured a quiescent magnitude of < B >= 14.7 pm 0.4. No previous outburst was found. However, we suggest that if the nova is recurrent it should be on a timescale of centuries. We find a periodicity at quiescence of 737 days which may arise from reflection effects and/or eclipses in the central binary. The periodicity and the quiescence magnitude of the system suggest that the secondary star is evolved and likely in, or ascending, the Red Giant Branch. A second period is evident at 376 days which has a sinusoidal like light curve. Furthermore, the outburst amplitude of ~ 9 magnitudes is inconsistent with those expected for fast classical novae (~ 17 magnitudes) which may lend further support for an evolved secondary. (Abridged) DA - 2012 DB - OpenUCT DP - University of Cape Town IS - 4 J1 - Astronomy and Astrophysics LK - https://open.uct.ac.za PY - 2012 SM - 0004-6361 SM - 1432-0746 T1 - Historical light curve and search for previous outbursts of Nova KT Eridani (2009) TI - Historical light curve and search for previous outbursts of Nova KT Eridani (2009) UR - http://hdl.handle.net/11427/35088 ER - en_ZA
dc.identifier.urihttp://hdl.handle.net/11427/35088
dc.identifier.vancouvercitationJurdana-Šepić R, Ribeiro VARM, Darnley MJ, Munari U, Bode MF. Historical light curve and search for previous outbursts of Nova KT Eridani (2009). Astronomy and Astrophysics. 2012;537(4):A34 - 177. http://hdl.handle.net/11427/35088.en_ZA
dc.language.isoeng
dc.publisher.departmentDepartment of Astronomy
dc.publisher.facultyFaculty of Science
dc.sourceAstronomy and Astrophysics
dc.source.journalissue4
dc.source.journalvolume537
dc.source.paginationA34 - 177
dc.source.urihttps://dx.doi.org/10.1051/0004-6361/201117806
dc.subject.othernovae, cataclysmic variables
dc.subject.otherstars: individual: KT Eri
dc.subject.othernovae
dc.subject.othercataclysmic variables
dc.titleHistorical light curve and search for previous outbursts of Nova KT Eridani (2009)
dc.typeJournal Article
uct.type.publicationResearch
uct.type.resourceJournal Article
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