THE SPECTRAL EVOLUTION AND EJECTA OF RECURRENT NOVA U Sco IN THE 2010 OUTBURST

Diaz, Marcos P.; Williams, Robert E.; Luna, G. J. M.; Moraes, Manoel Odoríco de; Takeda, L.

doi:10.1088/0004-6256/140/6/1860

Cited by 36 publications

(46 citation statements)

References 30 publications

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“…The spectrum of day +33.78 presented in Fig. 7 Anupama & Dewangan (2000) and in the spectrum of ∼day 50 presented by Thoroughgood et al (2001) Diaz et al (2010) and Mason (2011). However, its identification in the spectrum presented is uncertain since the region is affected by noise.…”

Section: Nebular Phasementioning

confidence: 90%

“…In addition, a few new phenomena have also been detected during the evolution of the outburst. Optical and near-infrared data on the evolution of the 2010 outburst are presented by Munari et al (2010), Yamanaka et al (2010), Diaz et al (2010), Kafka & Williams (2011), Banerjee et al (2010), Mason 2011, Maxwell et al (2012 and Mason et al (2012), while the X-ray observations are presented by Ness et al (2012) and Orio et al (2013).…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Nebular Phasementioning

confidence: 90%

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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“…The broad emission components of H I lines nearly disappeared at day 23 in the outburst of U Sco in 2010 (Diaz et al 2010), then the forbidden lines were first detected at day 51. In contrast, in the cases of T Pyx, IM Nor, and CI Aql, the [O III] and [N II] emission lines appeared when the H I emission lines were still broad.…”

Section: Classification Of CI Aqlmentioning

confidence: 97%

“…In contrast, no forbidden line was detected in the outbursts of U Sco type recurrent novae until Diaz et al (2010) (Rosino & Iijima 1988;Sekiguchi et al 1988;Munari et al 1999;Iijima 2002), V394 CrA (Sekiguchi et al 1989), and Nova LMC 1990-2 (Sekiguchi et al 1990). …”

Section: Classification Of CI Aqlmentioning

confidence: 99%

Spectroscopic observations of the recurrent nova CI Aquilae during the 2000 outburst

Iijima¹

2012

A&A

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High-and low-resolution optical spectra of CI Aql were obtained during the outburst in 2000. Multiple absorption components of H I and Fe II lines were detected at the early decline stage. Their radial velocities were roughly −2500 km s −1 , −2200 km s −1 , −1700 km s −1 , and −1400 km s −1 , among which only the last components were likely still accelerating during the early decline stage. Prominent emission lines of [O III] and [N II] appeared about one month after light maximum. The duration of the nebular stage, however, was only one month and a few weeks. The ejected gas shells seem to have started to shrink about 70 days after light maximum. The amount of interstellar extinction is estimated to be E(B − V) = 0.92 ± 0.15 from the equivalent widths of the diffuse interstellar absorption bands. The helium abundance in the ejecta is estimated to be N(He) = 0.19 ± 0.05 and the mass of the ejecta to be about 2 × 10 −6 M . This object has been classified as a U Sco type recurrent nova, but its spectral evolution during the outburst resembled those of T Pyx type recurrent novae. It is doubtful whether the peak of m V 9 mag on 2000 May 5 was the true light maximum or an earlier brighter peak had been overlooked, because the spectral data suggest that the ejections of gas shells occurred prior to the discovery of the outburst on 2000 April 28.

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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 SPECTRAL EVOLUTION AND EJECTA OF RECURRENT NOVA U Sco IN THE 2010 OUTBURST

Cited by 36 publications

References 30 publications

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

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

Spectroscopic observations of the recurrent nova CI Aquilae during the 2000 outburst

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

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