THE EXPANDING NEBULAR REMNANT OF THE RECURRENT NOVA RS OPHIUCHI (2006). II. MODELING OF COMBINED<i>HUBBLE SPACE TELESCOPE</i>IMAGING AND GROUND-BASED SPECTROSCOPY

Ribeiro, V. A. R. M.; Bode, M. F.; Darnley, M. J.; Harman, D. J.; Newsam, A. M.; O’Brien, T. J.; Bohigas, J.; Echevarría, J.; Bond, Howard E.; Chavushyan, V.; Costero, R.; Coziol, R.; Evans, A.; Eyres, S. P. S.; León-Tavares, J.; Richer, M. G.; Tovmassian, G.; Starrfield, S.; Zharikov, S. V.

doi:10.1088/0004-637x/703/2/1955

Cited by 57 publications

(55 citation statements)

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“…It is noteworthy that this expansion velocity is also comparable to the RN LMC 2009a (Bode et al, in prep. ) however, lower than those observed in other RNe (for example, RS Oph and U Sco, Ribeiro et al 2009;and Munari et al 1999, respectively) although still higher than a typical CN (e.g., Slavin et al 1995).…”

Section: Introductionmentioning

confidence: 55%

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

Jurdana-Šepić

Ribeiro

Darnley

et al. 2011

A&A

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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 ± 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 mag is inconsistent with those expected for fast classical novae (∼17 mag) which may lend further support for an evolved secondary. Conclusions. We investigated the probable recurrent nova KT Eri for which we suggest an inter-outburst period of order centuries and an evolved secondary. This may suggest that there is a whole range of possible inter-outburst periods in between the "typical" classical and recurrent novae nomenclature. Archival searches are an excellent tool in order to investigate the nature of astrophysical objects, in order to determine the nature and physical parameters.

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Section: Introductionmentioning

confidence: 55%

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

Jurdana-Šepić

Ribeiro

Darnley

et al. 2011

A&A

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“…In the case of U Sco, the red/blue velocities are much higher than those expected from an accretion disk surrounding the WD, so this line shape likely represents the projected geometry of the ejected shell on the orbital plane. The exact shape of the ejected material is not known for U Sco, however modeling of HST and radio observations of the recurrent nova RS Ophiuchi argues for an hourglass shape of the ejecta (Ribeiro et al 2009). It is possible that the U Sco ejecta are also lobe-like, expanding perpendicular to the orbital plane of the binary.…”

Section: Data Analysis and Discussionmentioning

confidence: 99%

The 2010 early outburst spectrum of the recurrent nova U Scorpii

Kafka

Williams

2010

A&A

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Aims. We present optical spectra of the fast recurrent nova U Sco during its recent outburst, obtained within 24 h of maximum light. Methods. We use medium resolution (R ∼ 4000) spectra taken with the with the MagE spectrograph on the Magellan (Clay) 6.5 m telescope of the Las Campanas Observatories. Results. The spectrum is notable for its lack of a low ionization transient heavy element absorption system that is visible in the large majority of novae near maximum light. We suggest that this may be due to the dominance of inner Lagrangian L1 mass transfer and the absence of a circumbinary gas reservoir in this object.

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“…Some recent examples suggest that bipolarity in the ejecta of classical/recurrent novae may be relatively frequent: RS Oph (Ribeiro et al 2009;Bode et al 2007;Chesneau et al 2007), V445 Pup (Woudt et al 2009), V1280 Sco (Chesneau et al 2008;Chesneau et al, in prep. ) or HR Del (Harman & O'Brien 2003).…”

Section: A Face-on Bipolar Eventmentioning

confidence: 99%

The 2011 outburst of the recurrent nova T Pyxidis. Evidence for a face-on bipolar ejection

Chesneau¹,

Meilland²,

Banerjee³

et al. 2011

A&A

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Aims. T Pyx is the first recurrent nova ever historically studied. It was seen in outburst six times between 1890 and 1966 and then not for 45 years. We report on near-IR interferometric observations of the recent outburst of 2011. Methods. We obtained near-IR observations of T Pyx at dates ranging from t = 2.37 d to t = 48.2 d after the outburst, with the CLASSIC recombiner located at the CHARA array and with the PIONIER and AMBER recombiners located at the VLTI array. These data are supplemented with near-IR photometry and spectra obtained at Mount Abu, India. We compare expansion of the H and K band continua and the Brγ emission line, and infer information on the kinematics and morphology of the early ejecta. Results. Slow expansion velocities were measured (≤300 km s −1 ) before t = 20 d. From t = 28 d on, the AMBER and PIONIER continuum visibilities (K and H band, respectively) are best simulated with a two-component model consisting of an unresolved source plus an extended source whose expansion velocity onto the sky plane is lower than ∼700 km s −1 . The expansion of the Brγ lineforming region, as inferred at t = 28 d and t = 35 d, is slightly larger, implying velocities in the range 500−800 km s −1 , which is still strikingly lower than the velocities of 1300−1600 km s −1 inferred from the Doppler width of the line. Moreover, a remarkable pattern was observed in the Brγ differential phases. A semi-quantitative model using a bipolar flow with a contrast of 2 between the pole and equator velocities, an inclination of i = 15• , and a position angle PA = 110• provides a good match to the AMBER observables. At t = 48 d, a PIONIER dataset confirms the two-component nature of the H band emission, consisting of an unresolved stellar source and an extended region whose appearance is circular and symmetric within error bars. Conclusions. These observations are most simply interpreted within the frame of a bipolar model, oriented nearly face-on. This finding has profound implications for interpreting past, current, and future observations of the expanding nebula.

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THE EXPANDING NEBULAR REMNANT OF THE RECURRENT NOVA RS OPHIUCHI (2006). II. MODELING OF COMBINEDHUBBLE SPACE TELESCOPEIMAGING AND GROUND-BASED SPECTROSCOPY

Cited by 57 publications

References 20 publications

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

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

The 2010 early outburst spectrum of the recurrent nova U Scorpii

The 2011 outburst of the recurrent nova T Pyxidis. Evidence for a face-on bipolar ejection

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