The 1987 Outburst of the Recurrent Nova U Sco

Sekiguchi, K.; Feast, M. W.; Whitelock, P. A.; Overbeek, M. D.; Wargau, W.; Jones, J. H. Spencer

doi:10.1007/978-94-009-2969-2_72

Cited by 20 publications

(32 citation statements)

References 4 publications

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“…Sekiguchi et al (1990) report t 2 = 5 and t 3 = 9 days for V745 Sco; while Anupama & Sethi (1994) measured t 2 = 12 and t 3 = 17 days, in the case of V3890 Sgr. Their outburst amplitude (A ∼ 7.3 mag for V745 Sco, Sekiguchi et al 1990; 7 ≤ A ≤ 9 mag for V3890 Sgr, Wenzel 1990) are consistent with those typically observed in symbiotic recurrent novae such as RS-Oph and T CrB.…”

Section: Discussionmentioning

confidence: 95%

“…the 4640 Å blend and the HeIIλ4686) and forbidden transitions ([OII](1), Sekiguchi et al 1990; as well as [FeX], [FeVII] and [FeXI], Williams et al 1991). Similarly Anupama & Sethi (1994) observations showed that in less than one month V3890 Sgr has developed forbidden coronal lines from [FeX], [FeXIV], [AX] and [AXI].…”

Section: Discussionmentioning

confidence: 99%

“…V745 Sco spectra were characterized by large velocities (FWHM ∼ 1000 km s −1 and extended wings up to 4000 km s −1 , Sekiguchi et al 1990), and early development of high ionization energy emission lines (e.g. the 4640 Å blend and the HeIIλ4686) and forbidden transitions ([OII](1), Sekiguchi et al 1990; as well as [FeX], [FeVII] and [FeXI], Williams et al 1991).…”

Section: Discussionmentioning

confidence: 99%

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The peculiar nova V1309 Scorpii/nova Scorpii 2008

Mason¹,

Diaz²,

Williams³

et al. 2010

A&A

116

157

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Aims. Nova Scorpii 2008 was the target of our Director Discretionary Time proposal at VLT+UVES in order to study the evolution, origin and abundances of the heavy-element absorption system recently discovered in 80% of classical novae in outburst. Methods. The early decline of nova Scorpii 2008 was monitored with high resolution echelle spectroscopy at 5 different epochs. The analysis of the absorption and the emission lines show many unusual characteristics. Results. Nova Scorpii 2008 is confirmed to differ from a common classical nova as well as a symbiotic recurrent nova, and it shows characteristics which are common to the so called, yet debated, red-novae. The origin of this new nova remains uncertain.

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Section: Discussionmentioning

confidence: 95%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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The peculiar nova V1309 Scorpii/nova Scorpii 2008

Mason¹,

Diaz²,

Williams³

et al. 2010

A&A

116

157

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“…107=Bl 3−14 The finding chart in [18] is good, but the coordinates are reported to disagree with the measured position: α = 17 h 52 m 06 s .4, δ = −29 • 45 49 (1950) [90] (if this is right, our coordinates should also be corrected). 110=V745 Sco V K magnitudes during decline from outburst [284]. 112=AS 255 IR-type S - [18,16], D - [137,172].…”

Section: =As 245mentioning

confidence: 99%

A catalogue of symbiotic stars

Belczyński

Mikołajewska

Munari

et al. 2000

Astron. Astrophys. Suppl. Ser.

379

407

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Abstract. We present a new catalogue of symbiotic stars. In our list we include 188 symbiotic stars as well as 30 objects suspected of being symbiotic. For each star, we present basic observational material: coordinates, V and K magnitudes, ultraviolet (UV), infrared (IR), X-ray and radio observations. We also list the spectral type of the cool component, the maximum ionization potential observed, references to finding charts, spectra, classifications and recent papers discussing the physical parameters and nature of each object. Moreover, we present the orbital photometric ephemerides and orbital elements of known symbiotic binaries, pulsational periods for symbiotic Miras, Hipparcos parallaxes and information about outbursts and flickering.

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“…Multifrequency light curves of V745 Sco for the 1989 and 2014 outbursts. The V light curve of the V745 Sco 1989 (open blue circles, taken from[97]) and 2014 (filled red circles from SMARTS and open green circles from AAVSO) outbursts are plotted on a logarithmic timescale. We also include X-ray (0.3 − 2.0 keV with magenta pluses and 2.0 − 10 keV with cyan crosses) data taken from[84] and radio (filled black triangles, GMRT at 610 MHz) data taken from[53].…”

mentioning

confidence: 99%

Multifrequency behavior of classical novae

Hachisu

Kato²

2018

Proceedings of the Golden Age of Cataclysmic Variables and Related Objects IV — PoS(GOLDEN 2017)

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We review our current understanding of multiwavelength light curves of classical and recurrent novae and show how to determine the WD masses and other binary properties. We pick up PW Vul, U Sco, V745 Sco, RS Oph, and V407 Cyg as representatives of different types of light curves, examine their light curves in detail, discuss physical properties, and clarify the reason of these differences. In the rising phase, the hydrogen-rich envelope expands beyond the size of a close binary in which the companion is embedded deep inside of the photosphere. After the optical maximum, the pseud-photosphere begins to shrink and an optically thin region develops outside of the photosphere. The free-free emission dominates the flux at relatively longer wavelengths (optical and NIR), of which light curves decay along the universal decline law of F ν ∝ t −1.75 (or t −1.55). The physical mechanism of super-Eddington phase is presented. In the presence of shock interaction between ejecta and circumstellar matter, it slows down the decay of optical flux as F ν ∝ t −1.0 as seen in the early phase of V407 Cyg. In final stages of outbursts, the wind mass-loss rate sharply drops so the slope of free-free emission decays like F ν ∝ t −3.5. Supersoft X-ray phase begins and continues until hydrogen nuclear burning ends, and after that the nova enters a cooling phase. Hard X-rays may originate from internal shocks between ejecta (or a bow shock between ejecta and the companion). The behaviors of optical-dominant, UV-dominant, and supersoft X-ray source phase have different dependences on the WD mass and envelope chemical composition, so multiwavelength observations are useful to determine the parameters such as the WD mass. Finally, we should note that the very early phase of nova outbursts remains unexplored. An X-ray flash phase is theoretically identified, but not yet successfully detected. Detections of early X-ray flashes give direct information on thermonuclear runaway.

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The 1987 Outburst of the Recurrent Nova U Sco

Cited by 20 publications

References 4 publications

The peculiar nova V1309 Scorpii/nova Scorpii 2008

The peculiar nova V1309 Scorpii/nova Scorpii 2008

A catalogue of symbiotic stars

Multifrequency behavior of classical novae

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