The Change of the Orbital Periods Across Eruptions and the Ejected Mass for Recurrent Novae Ci Aquilae and U Scorpii

Schaefer, Bradley E.

doi:10.1088/0004-637x/742/2/112

Cited by 34 publications

(26 citation statements)

References 58 publications

(129 reference statements)

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“…An upper limit on the ejected mass of order 10 −6  M is suggested from the expansion velocity and t on based on the simple homogenous and uniformly expanding shell models of Schwarz et al (2011, see their Figure 8). This low mass is very similar to those of fast recurrent novae (for example, see Schaefer 2011;Anupama 2013).…”

Section: Xrtsupporting

confidence: 67%

Pan-Chromatic Observations of the Remarkable Nova Large Magellanic Cloud 2012

Schwarz

Shore

Page

et al. 2015

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We present the results of an intensive multiwavelength campaign on nova LMC 2012. This nova evolved very rapidly in all observed wavelengths. The time to fall two magnitudes in the V band was only 2 days. In X-rays the super soft phase began 13 ± 5 days after discovery and ended around day 50 after discovery. During the super soft phase, the Swift/XRT and Chandra spectra were consistent with the underlying white dwarf (WD) being very hot, ∼1 MK, and luminous, ∼10 38 erg s −1 . The UV, optical, and near-IR photometry showed a periodic variation after the initial and rapid fading had ended. Timing analysis revealed a consistent 19.24 ± 0.03 hr period in all UV, optical, and near-IR bands with amplitudes of ∼0.3 mag which we associate with the orbital period of the central binary. No periods were detected in the corresponding X-ray data sets. A moderately high inclination system, i = 60 ± 10, was inferred from the early optical emission lines. The HST/STIS UV spectra were highly unusual with only the N V (1240 Å) line present and superposed on a blue continuum. The lack of emission lines and the observed UV and optical continua from four epochs can be fit with a low mass ejection event, ∼10 −6  M , from a hot and massive WD near the Chandrasekhar limit. The WD, in turn, significantly illuminated its subgiant companion which provided the bulk of the observed UV/optical continuum emission at the later dates. The inferred extreme WD characteristics and low mass ejection event favor nova LMC 2012 being a recurrent nova of the U Sco subclass.

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Section: Xrtsupporting

confidence: 67%

Pan-Chromatic Observations of the Remarkable Nova Large Magellanic Cloud 2012

Schwarz

Shore

Page

et al. 2015

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“…In addition, the values are strongly dependent on the assumed geometry. The ejected mass of M H ∼ 4.6 × 10 −6 M for a spherically symmetric geometry is similar to M ejecta = 4.3 × 10 −6 M based on orbital period changes (Schaefer 2011), and 3 × 10 −6 M based on photoionisation models of a clumpy ejecta (Diaz et al 2010).…”

Section: Discussionmentioning

confidence: 51%

The 2010 outburst and pre-outburst optical spectrum of the recurrent nova U Scorpii

Anupama

Kamath

Ramaprakash

et al. 2013

A&A

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Aims. We study the evolution of the recurrent nova U Scorpii during its outburst in 2010. Methods. Optical spectroscopic observations of the nova were obtained during 0.83-162.5 days after outburst maximum. Optical linear polarisation observations were made before the onset of the super soft X-ray source (SSS) phase and during the SSS phase. Radio continuum observations were made in the 1280 MHz band during the early decline phase, and in the 610 MHz band at the onset and end of the SSS phase. We also present optical spectra obtained in the pre-outburst quiescence phase. Results. The overall spectral evolution during the 2010 outburst is similar to the previous outbursts. However, the dense temporal coverage, especially during the early phases, reveals several short term variations not reported previously. The early phase emission line widths indicate extremely high velocities for the nova ejecta, ∼10 000 km s −1 . The line profiles are broad, boxy and structured. Narrow P-Cygni absorptions, at ∼500 km s −1 are seen associated with the He I lines, and also the Ca II, N I and hydrogen lines (at wavelengths >8000 Å) in the spectrum of day 6.83, obtained immediately after an optical flare. This absorption component could be arising in the plasma emitting the Nitrogen lines seen in X-rays, that probably lies outside the binary orbit. Rapid variations are detected in the strength of the 4660 Å N III feature, which shows a significant increase in the line strength on days 8.83 and 13.82, at orbital phases of 0.75 and 0.25, respectively. Instrinsic polarisation is detected just before the onset, and during the SSS phase, with p v ∼ 1.4% during the SSS phase. The flux variations of the N III feature and the intrinsic polarisation are most likely associated with the reforming accretion disc/stream. We estimate the mass of the ejected (hydrogen) shell to be ∼4.6 × 10 −6 M , for a spherical shell geometry. The non-detection of U Sco in the 1280 MHz and 610 MHz radio bands is consistent with the low mass of the nova ejecta, subgiant nature of the secondary, and the distance to the nova.

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“…the mass of accreted materials during the quiescent phase minus that ejected at a nova eruption) is positive. The general answer for this is not yet clear, 43 but given the nearly Chandrasekhar mass WD as derived for some recurrent nova systems, at least a part of systems undergoing novae are viable candidates as an SN Ia progenitor.…”

Section: +008mentioning

confidence: 99%

Progenitors of type Ia supernovae

Maeda

Terada

2017

The Fourteenth Marcel Grossmann Meeting

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Natures of progenitors of type Ia Supernovae (SNe Ia) have not yet been clarified. There has been long and intensive discussion on whether the so-called single degenerate (SD) scenario or the double degenerate (DD) scenario, or anything else, could explain a major population of SNe Ia, but the conclusion has not yet been reached. With rapidly increasing observational data and new theoretical ideas, the field of studying the SN Ia progenitors has been quickly developing, and various new insights have been obtained in recent years. This paper aims at providing a summary of the current situation regarding the SN Ia progenitors, both in theory and observations. It seems difficult to explain the emerging diversity seen in observations of SNe Ia by a single population, and we emphasize that it is important to clarify links between different progenitor scenarios and different sub-classes of SNe Ia.

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The Change of the Orbital Periods Across Eruptions and the Ejected Mass for Recurrent Novae Ci Aquilae and U Scorpii

Cited by 34 publications

References 58 publications

Pan-Chromatic Observations of the Remarkable Nova Large Magellanic Cloud 2012

Pan-Chromatic Observations of the Remarkable Nova Large Magellanic Cloud 2012

The 2010 outburst and pre-outburst optical spectrum of the recurrent nova U Scorpii

Progenitors of type Ia supernovae

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