A Multiwavelength Light-curve Analysis of the Classical Nova KT Eri: Optical Contribution from a Large Irradiated Accretion Disk
KT Eri is a classical nova that went into outburst in 2009. Recent photometric analysis in quiescence indicates a relatively longer orbital period of 2.6 days, so that KT Eri could host a very bright accretion disk during the outburst like in the recurrent nova U Sco, the orbital period of which is...
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2025-01-01
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| author | Izumi Hachisu Mariko Kato Frederick M. Walter |
| author_facet | Izumi Hachisu Mariko Kato Frederick M. Walter |
| author_sort | Izumi Hachisu |
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| description | KT Eri is a classical nova that went into outburst in 2009. Recent photometric analysis in quiescence indicates a relatively longer orbital period of 2.6 days, so that KT Eri could host a very bright accretion disk during the outburst like in the recurrent nova U Sco, the orbital period of which is 1.23 days. We reproduced the optical V light curve as well as the supersoft X-ray light curve of KT Eri in outburst, assuming a large irradiated disk during a nova wind phase of the outburst while a normal size disk after the nova winds stop. This result is consistent with the temporal variation of wide-band V brightness that varies almost with the intermediate-band Strömgren y brightness, because the V flux is dominated by continuum radiation, the origin of which is a photospheric emission from the very bright disk. We determined the white dwarf mass to be M _WD = 1.3 ± 0.02 M _⊙ , the hydrogen-burning turnoff epoch to be ∼240 days after the outburst, the distance modulus in the V band to be ( m − M ) _V = 13.4 ± 0.2, and the distance to KT Eri to be d = 4.2 ± 0.4 kpc for the reddening of E ( B − V ) = 0.08. The peak absolute V brightness is about ${M}_{V,{\rm{\max }}}=-8.0$ and the corresponding recurrence time is ∼3000 yr from its ignition mass together with the mean mass-accretion rate of ${\dot{M}}_{{\rm{acc}}}\sim 1\times 1{0}^{-9}\,{M}_{\odot }$ yr ^−1 in quiescence. Thus, we suggest that KT Eri is not a recurrent nova. |
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| institution | Kabale University |
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| publishDate | 2025-01-01 |
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| spelling | doaj-art-1d8dd34b5bd84f0dbc92944ceacbd0422025-02-10T07:34:37ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01980114210.3847/1538-4357/adae08A Multiwavelength Light-curve Analysis of the Classical Nova KT Eri: Optical Contribution from a Large Irradiated Accretion DiskIzumi Hachisu0https://orcid.org/0000-0002-0884-7404Mariko Kato1https://orcid.org/0000-0002-8522-8033Frederick M. Walter2https://orcid.org/0000-0001-7796-1756Department of Earth Science and Astronomy, College of Arts and Sciences, University of Tokyo , Komaba 3-8-1, Meguro-ku, Tokyo 153-8902, Japan ; izumi.hachisu@outlook.jpDepartment of Astronomy, Keio University , Hiyoshi 4-1-1, Kouhoku-ku, Yokohama 223-8521, JapanDepartment of Physics and Astronomy, Stony Brook University , StonyBrook, NY 11794, USAKT Eri is a classical nova that went into outburst in 2009. Recent photometric analysis in quiescence indicates a relatively longer orbital period of 2.6 days, so that KT Eri could host a very bright accretion disk during the outburst like in the recurrent nova U Sco, the orbital period of which is 1.23 days. We reproduced the optical V light curve as well as the supersoft X-ray light curve of KT Eri in outburst, assuming a large irradiated disk during a nova wind phase of the outburst while a normal size disk after the nova winds stop. This result is consistent with the temporal variation of wide-band V brightness that varies almost with the intermediate-band Strömgren y brightness, because the V flux is dominated by continuum radiation, the origin of which is a photospheric emission from the very bright disk. We determined the white dwarf mass to be M _WD = 1.3 ± 0.02 M _⊙ , the hydrogen-burning turnoff epoch to be ∼240 days after the outburst, the distance modulus in the V band to be ( m − M ) _V = 13.4 ± 0.2, and the distance to KT Eri to be d = 4.2 ± 0.4 kpc for the reddening of E ( B − V ) = 0.08. The peak absolute V brightness is about ${M}_{V,{\rm{\max }}}=-8.0$ and the corresponding recurrence time is ∼3000 yr from its ignition mass together with the mean mass-accretion rate of ${\dot{M}}_{{\rm{acc}}}\sim 1\times 1{0}^{-9}\,{M}_{\odot }$ yr ^−1 in quiescence. Thus, we suggest that KT Eri is not a recurrent nova.https://doi.org/10.3847/1538-4357/adae08Classical novaeFast novaeStellar windsX-ray astronomyShocks |
| spellingShingle | Izumi Hachisu Mariko Kato Frederick M. Walter A Multiwavelength Light-curve Analysis of the Classical Nova KT Eri: Optical Contribution from a Large Irradiated Accretion Disk The Astrophysical Journal Classical novae Fast novae Stellar winds X-ray astronomy Shocks |
| title | A Multiwavelength Light-curve Analysis of the Classical Nova KT Eri: Optical Contribution from a Large Irradiated Accretion Disk |
| title_full | A Multiwavelength Light-curve Analysis of the Classical Nova KT Eri: Optical Contribution from a Large Irradiated Accretion Disk |
| title_fullStr | A Multiwavelength Light-curve Analysis of the Classical Nova KT Eri: Optical Contribution from a Large Irradiated Accretion Disk |
| title_full_unstemmed | A Multiwavelength Light-curve Analysis of the Classical Nova KT Eri: Optical Contribution from a Large Irradiated Accretion Disk |
| title_short | A Multiwavelength Light-curve Analysis of the Classical Nova KT Eri: Optical Contribution from a Large Irradiated Accretion Disk |
| title_sort | multiwavelength light curve analysis of the classical nova kt eri optical contribution from a large irradiated accretion disk |
| topic | Classical novae Fast novae Stellar winds X-ray astronomy Shocks |
| url | https://doi.org/10.3847/1538-4357/adae08 |
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