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

  title={Historical light curve and search for previous outbursts of Nova KT Eridani (2009)},
  author={Rajka Jurdana-{\vS}epi{\'c} and Val{\'e}rio A. R. M. Ribeiro and Matthew J. Darnley and U. Munari and Michael F. Bode},
  journal={Astronomy \& Astrophysics},
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… 

Figures and Tables from this paper

On the progenitors of local group novae. II. the red giant nova rate of M31
In our preceding paper, Liverpool Telescope data of M31 novae in eruption were used to facilitate a search for their progenitor systems within archival Hubble Space Telescope data, with the aim of
Optical observations of ‘hot’ novae returning to quiescence
We have monitored the return to quiescence of novae previously observed in outburst as supersoft X-ray sources, with optical photometry of the intermediate polar (IP) V4743 Sgr and candidate IP V2491
On the Progenitors of Galactic Novae
Of the approximately 400 known Galactic classical novae, only 10 of them, the recurrent novae, have been seen to erupt more than once. At least eight of these recurrents are known to harbor evolved
Review of light curves of novae in the modified scales. I. Recurrent novae
We reviewed the light curves of 10 known recurrent novae (RNs) in the modified scales of the "logarithmic of time, amplitude of outburst". A unified rule was established to normalize the time scale.
On the narrow emission line components of the LMC novae 2004 (YY Doradus) and 2009a
We present early decline spectra of the two Large Magellanic Cloud novae: LMC 2004 (YY Dor) and LMC 2009a and discuss their spectral an line profile evolution with special emphasis on the existence
We report the results of a survey of M31 novae in quiescence. This is the first catalog of extragalactic systems in quiescence to be published, and contains data for 38 spectroscopically confirmed
Nova KT Eri 2009: infrared studies of a very fast and small amplitude He/N nova
We present near-infrared spectroscopic and photometric observations of the nova KT Eridani taken during the first 100 days following its discovery in 2009 November. The JHK spectra of the object have
Accrete, Accrete, Accrete… Bang! (and repeat): The remarkable Recurrent Novae
  • M. Darnley
  • Physics
    Proceedings of The Golden Age of Cataclysmic Variables and Related Objects V — PoS(GOLDEN2019)
  • 2021
All novae recur, but only a handful have been observed in eruption more than once. These systems, the recurrent novae (RNe), are among the most extreme examples of novae. RNe have long been thought


On the Progenitor System of Nova V2491 Cygni
Nova V2491 Cyg is one of just two detected pre-outburst in X-rays. The light curve of this nova exhibited a rare "re-brightening" which has been attributed by some as the system being a polar, whilst
Supersoft X-Ray Light Curve of RS Ophiuchi (2006)
One of the candidates for Type Ia supernova progenitors, the recurrent nova RS Ophiuchi, underwent its sixth recorded outburst in 2006 February, and for the first time a complete light curve of
Exquisite Nova Light Curves from the Solar Mass Ejection Imager (SMEI)
We present light curves of three classical novae (CNe; KT Eridani, V598 Puppis, V1280 Scorpii) and one recurrent nova (RS Ophiuchi) derived from data obtained by the Solar Mass Ejection Imager (SMEI)
Swift observations of the X-ray and UV evolution of V2491 Cyg (Nova Cyg 2008 No. 2)
Observing the X-ray emission from only one day after the nova discovery, the source is followed through the initial brightening, the super-soft source phase and back to the pre-outburst flux level, demonstrating the evolution of the spectrum throughout the outburst.
The morphology of the expanding ejecta of V2491 Cygni (2008 N.2)
Determining the evolution of the ejecta morphology of novae provides valuable information on the shaping mechanisms in operation at early stages of the nova outburst. Understanding such mechanisms
Properties, evolution and morpho-kinematical modelling of the very fast nova V2672 Oph (Nova Oph 2009), a clone of U Sco
Nova Oph 2009 (V2672 Oph) reached maximum brightness V = 11.35 on 2009 August 16.5. With observedt2(V) = 2.3 andt3(V) = 4.2 d decline times, it is one of the fastest known novae, being rivalled only
Symbiotic stars on Asiago archive plates. II
The Asiago photographic archive has been searched for plates containing the symbiotic stars Hen 2-468, QW Sge, LT Del, V407 Cyg, K 3-9, V335 Vul, FG Ser and Draco C-1. A total of 635 plates imaging
We report Hubble Space Telescope (HST) imaging, obtained 155 and 449 days after the 2006 outburst of the recurrent nova RS Ophiuchi, together with ground-based spectroscopic observations, obtained
A classical nova, V2487 Oph 1998, seen in x-rays before and after its explosion.
Observations of the recent nova V2487 Oph 1998 by the X-ray Multi-Mirror satellite provide evidence that accretion (probably on a magnetic white dwarf) was reestablished as early as 2.7 years after the explosion.