The 1979 outburst of U Scorpii

Barlow, M. J.; Brodie, Jean P.; Brunt, Carol; Hanes, David A.; Hill, P. W.; Mayo, Sue; Pringle, J. E.; Ward, M. J.; Watson, M. G.; Whelan, J. A. J.; Willis, A. J.

doi:10.1093/mnras/195.1.61

Cited by 71 publications

(66 citation statements)

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“…Unfortunately, most of the past follow-ups did not monitor the modulation and changes of the narrow emission component with the binary orbital phase. However, Barlow et al (1981) observe that both the He iiλ4686 and the Balmer emission lines profiles change significantly from day +8 to +12; while their Fig. 3 shows that the peak position of the Hγ emission line changes with time and is split by a relatively strong absorption component at orbital phase 0.72, in agreement with our observations (Fig.…”

Section: Discussionsupporting

confidence: 90%

“…3 and 4 of Munari et al (1999) shows a change in the relative intensity and profile of the three emission components, as well as a decrease in the separation of the peaks with time. Combining our results from the U Sco 2010 outburst with the observations of Barlow et al (1981) and Munari et al (1999) we conclude that the U Sco secondary star always resumes mass transfer ∼8−10 days after the outburst.…”

Section: Discussionsupporting

confidence: 84%

“…The spectrum of Iijima (2002), shows, in addition, that on day +11 Bowen fluorescence is still active. Also, the spectrum of Sekiguchi et al (1988) on day +9 and the +8 day spectrum of Barlow et al (1981) show narrow emission components and the first appearance of He iiλ4686. It is therefore tempting to conclude that this is evidence for the resumption of accretion in the early decline spectra of the 1999, 1987, and 1979 outbursts.…”

Section: Discussionmentioning

confidence: 94%

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U Scorpii 2010 outburst: a new understanding of the binary accretion disk and the secondary star

Mason¹,

Ederoclite²,

Williams³

et al. 2012

A&A

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We present optical and near-infrared (NIR) spectroscopic observations of U Sco 2010 outburst. From the analysis of lines profiles we identify a broad and a narrow component and show that the latter originates from the reforming accretion disk. We show that the accretion resumes shortly after the outburst, on day +8, roughly when the super-soft (SSS) X-ray phase starts. Consequently U Sco SSS phase is fueled (in part or fully) by accretion and should not be used to estimate m rem , the mass of accreted material which has not been ejected during the outburst. In addition, most of the He emission lines, and the He ii lies in particular, form in the accretion flow/disk within the binary and are optically thick, thus preventing an accurate abundance determination.A late spectrum taken in quiescence and during eclipse shows Ca ii H&K, the G-band and Mg ib absorption from the secondary star.However, no other significant secondary star features have been observed at longer wavelengths and in the NIR band.

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Section: Discussionsupporting

confidence: 90%

Section: Discussionsupporting

confidence: 84%

Section: Discussionmentioning

confidence: 94%

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U Scorpii 2010 outburst: a new understanding of the binary accretion disk and the secondary star

Mason¹,

Ederoclite²,

Williams³

et al. 2012

A&A

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“…The outbursts are characterized by a fast rise to maximum, by > ∼ 10 mag in 6-12 h, followed by an extremely fast decline from maximum, at a rate of 0.67 mag per day (Payne-Gaposchkin 1957;Sekiguchi et al 1988;Munari et al 1999;Schaefer 2010). The outburst spectra indicate that matter is ejected at extremely high velocities of ∼10 000 km s −1 , and helium enriched (Barlow et al 1981;Williams et al 1981;Sekiguchi et al 1988;Munari et al 1999;Anupama & Dewangan 2000;Iijima 2002;Evans et al 2001). Iijima (2002), however, contests the helium enrichment estimated by others.…”

Section: Introductionmentioning

confidence: 99%

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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“…To put some order and to the aim of better isolating consistently similar phenomena we define as novae showing narrow emission line components those for which (1) the narrow component sits on-top of a clearly distinct and much broader pedestal; (2) it is seen in He ii 4686; and (3) with time the He ii 4686 narrow component overtakes, in strength, that displayed by Hβ. To our knowledge, the novae fulfilling such a criterion are: the two LMC presented here, U Sco (Barlow et al 1981;Sekiguchi et al 1988;Munari et al 1999;Diaz et al 2010;Mason et al 2012;Anupama et al 2013), V394 Cra (Sekiguchi et al 1989;Williams et al 1991), LMC 1990b (Sekiguchi 1990;Williams et al 1991), KT Eri (Munari et al 2014b), DE Cir (Walter et al 2012). V2672 Oph, which has a line profile very similar to YY Dor, cannot be included in the list since it has been observed only in Hα (Munari et al 2011;Walter et al 2012).…”

Section: The Narrow Component In the Literaturementioning

confidence: 99%

On the narrow emission line components of the LMC novae 2004 (YY Doradus) and 2009a

Mason

Munari

2014

A&A

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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 and appearance of a sharp component. We show that the narrow component that characterizes the emission lines in the maximum spectra of nova LMC 2004 originates in the ejecta.The He ii 4686 Å narrow emission which appears at the onset of the nebular phase in both novae is somewhat controversial. Our observations suggest that the corresponding line forming region is physically separated from the rest of the ejecta (the broad line region) and environmentally different. However, the lack of late time observations covering the super-soft source (SSS) phase, the post-SSS phase and the quiescence state does not allow to securely establish any non-ejecta origin/contribution as, instead, in the case of U Sco and KT Eri.

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The 1979 outburst of U Scorpii

Cited by 71 publications

References 0 publications

U Scorpii 2010 outburst: a new understanding of the binary accretion disk and the secondary star

U Scorpii 2010 outburst: a new understanding of the binary accretion disk and the secondary star

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

On the narrow emission line components of the LMC novae 2004 (YY Doradus) and 2009a

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