Optical Properties of X-Ray Novae

Ciatti, F.; Mammano, A.; Vittone, A. A.

doi:10.1007/978-94-010-1217-1_28

Cited by 12 publications

(17 citation statements)

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“…Evidence for high-velocity winds and outflows exists primarily in the symbiotic subclasses known as symbiotic novae and recurrent novae. High-velocity outflows (v h P1000 km s À1 ) have been observed in very broad emission lines and P Cygni profiles in essentially all the symbiotic novae: AG Peg ( Penston & Allen 1985), V1329 Cyg (Crampton et al 1970), RR Tel ( Penston et al 1983;Ponz et al 1982), HM Sge (Ciatti et al 1978(Ciatti et al , 1979Brown et al 1978;Mueller & Nussbaumer 1985), and V1016 Cyg ( Feibelman 1982). Ejection at considerably higher velocity is observed from recurrent novae, e.g., T CrB ($5000 km s À1 ; Livio 1988) and RS Oph ($3500 km s À1 ; Livio 1988; Taylor et al 1988aTaylor et al , 1989.…”

Section: Introductionmentioning

confidence: 99%

Colliding Winds in Symbiotic Binary Systems. I. Analytic and Numerical Solutions

Kenny

Taylor

2005

ApJ

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We present new formulations of binary colliding wind models appropriate to symbiotic star systems. The derived models differ from previous formulations in assuming mixing of the shocked material from both incoming streams, rather than postulating a self-sustaining contact discontinuity. The CWb model (colliding winds, binary) extends the work of Girard and Willson by the derivation of an adiabatic temperature, the consideration of radiative cooling, the inclusion of thermal pressures in the incoming winds, and the treatment of interaction shells of finite thickness and density. The finite thickness of the interaction shell allows for calculation of its radiative intensity distribution. The CWc model (colliding winds, concentric) is a similar extension of the model of Kwok, Purton, and Fitzgerald. It is derived in a manner parallel to that of the CWb model, thereby facilitating a unification of the two models. A unified model is desired since wind collisions in symbiotic systems should include aspects of both CWb and CWc interactions. Two examples of model applications are presented: a comparison of the flux densities arising from colliding winds (CWb model) with those arising from the ionization of the surrounding medium (STB model) in the galactic population of symbiotic stars, and model imaging of the symbiotic nova HM Sge.

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Section: Introductionmentioning

confidence: 99%

Colliding Winds in Symbiotic Binary Systems. I. Analytic and Numerical Solutions

Kenny

Taylor

2005

ApJ

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“…In particular, calibrated tracings of twelve ESO spectra, obtained by R. M. West in 1981 (see below), were used by M. Yu. Skul'sky for a preliminary study (Skul'sky 1985), resulting in a provisional value for the mass ratio (M 1 /M 2 = 0.3) which was used by Antokhina & Cherepashchuk (1988), in connection with the photometric data from Ciatti et al (1980), Kumsiasvili (1985), and Zakirov (1985), to derive photometric elements, in particular i = 84.…”

Section: New Spectrographic Observationsmentioning

confidence: 99%

“…III of the 'General Catalogue of Variable Stars' (Kholopov et al 1987) as having visual magnitude 9.12 at maximum light, with eclipse depths A 1 = 0.60 mag and A 2 = 0.44 mag, respectively, and with the indication that the light curve varies in shape. Ciatti et al (1980) found that the eclipses are partial, that the primary eclipse is an occultation, and that i = 75 • . Earlier, O'Connell (1949) had reported that the width of the primary eclipse is larger than that of the secondary eclipse, the ratio of the widths being 1.76, and that the secondary eclipse is not midway between the deeper minima but that t 1 − t 2 − P/2 = 0.11.…”

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confidence: 98%

A Spectrographic Study of the Interacting Eclipsing Binary RY Scuti: An Episode in the Rapid Mass Loss Stage or a Protoplanetary Nebula ?

Sahade¹,

West²,

Skul'Skij³

1992

Evolutionary Processes in Interacting Binary Stars

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RESUMENRY Scuti, la binaria de eclipse de 11 días de período, caracterizada, en su espectro, por presentar líneas de [Fe III], ha sido reinvestigada en base a material espectrográfico obtenido en Chile, en el Observatorio Europeo Austral y en el Observatorio Interamericano de Cerro Tololo, que cubre las regiones 3400-5150Å y 5700-6700Å. Fueron también analizadas observaciones en el ultravioleta obtenidas con el satélite IUE. El espectro de RY Sct es muy complejo y peculiar, y está caracterizado por varios conjuntos de líneas de emisión y de absorción. Entre las emisiones, aparece un grupo de líneas que son características de las nebulosas planetarias. El sistema está formado por una componente B0V y una compañera que parece rodeada por una envoltura opaca que emite en He II λ4686. En la envoltura circumbinaria podemos distinguir: (a) una región de radiación diluida animada de una velocidad de ∼ −178 km s −1 ; (b) regiones donde se originan las líneas de resonancia de Si IV y C IV en el ultravioleta, con velocidades de −1200 y −600 km s −1 ; (c) regiones que dan origen al "espectro nebular" y sugieren la existencia de una triple nebulosidad que rodea al sistema y está caracterizada por un valor de N e probablemente mayor que 10 4 cm −3 , un valor de T e ∼ 15-20,000 K y velocidades de −18, +9 y +48 km s −1 , respectivamente. ABSTRACT RY Scuti, the 11-day [Fe III] eclipsing binary, has been reinvestigated on the basis of spectrographic material obtained in Chile at the European Southern Observatory, La Silla, and at the Cerro Tololo Interamerican Observatory, covering the spectral regions 3400-5150Å and 5700-6700Å. Ultraviolet IUE observations were also analyzed. The spectrum of RY Sct is very complex and peculiar, being characterized by several sets of emission as well as absorption features. Among the emission features, there is a set of lines that are characteristic of planetary nebulae. The system is found to be formed by a B0V component and a companion that appears to be surrounded by an opaque envelope that emits in He II λ4686. In the circumbinary envelope we can distinguish: (a) a region of diluted radiation that suggests a velocity of ∼ −178 km s −1 ; (b) regions of formation of the resonance lines of Si IV and C IV in the IUE UV, characterized by velocities of −1200 and −600 km s −1 ; (c) regions that give rise to the "nebular spectrum" and suggest that there is a triple nebulosity surrounding the system with N e probably larger than 10 4 cm −3 , T e ∼ 15-20,000 K and velocities of −18, +9 and +48 km s −1 , respectively.

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“…The situation in this case is best illustrated by a VLA map made by Gibson (1979) who finds that a shock develops at the surface of interaction of the two winds. In this paper I shall describe another binary system in which two stellar winds are interacting with dramatic effects.HM Sge is a new emission-line star unique in many aspects, brightened by 6 visual magnitudes in 1976 (Dokuchaeva 1976) and has remained in maximum light since (Ciatti et al 1978). After the brightening, an emission line spectrum emerged, suggesting the presence of a clrcumstellar nebula.…”

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confidence: 99%

“…HM Sge is a new emission-line star unique in many aspects, brightened by 6 visual magnitudes in 1976 (Dokuchaeva 1976) and has remained in maximum light since (Ciatti et al 1978). After the brightening, an emission line spectrum emerged, suggesting the presence of a clrcumstellar nebula.…”

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confidence: 99%

Interacting stellar winds in a binary system

Kwok

1981

International Astronomical Union Colloquium

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It is now known that strong stellar winds develop in stars mostly at the red and blue sides of the HR diagram. However, although the mass loss rates observed in 0 and M stars are comparable, the corresponding wind velocities are vastly different. It would thus be of great interest to find a binary system, containing both a cool and a hot star each with its own wind, and observe the resultant interaction. For a long time a Sco (Ml.5 Iab + B2.5 V) was the only known example (Kudritzki and ' Reimers 1978, van der Hucht et al. 1980). The situation in this case is best illustrated by a VLA map made by Gibson (1979) who finds that a shock develops at the surface of interaction of the two winds. In this paper I shall describe another binary system in which two stellar winds are interacting with dramatic effects.HM Sge is a new emission-line star unique in many aspects, brightened by 6 visual magnitudes in 1976 (Dokuchaeva 1976) and has remained in maximum light since (Ciatti et al. 1978). After the brightening, an emission line spectrum emerged, suggesting the presence of a clrcumstellar nebula. Ultraviolet observations of HM Sge show that it has an extremely rich UV emission line spectrum (Bogges et al. 1980). Infrared ob servations by Davidson et al. 1978) found the object to be heavily reddened with most of the energy emitted in the infrared. The 9.7ym silicate feature was also detected, characteristic of a mass-losing M star. The 2.3pm CO absorption feature was

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Optical Properties of X-Ray Novae

Cited by 12 publications

References 0 publications

Colliding Winds in Symbiotic Binary Systems. I. Analytic and Numerical Solutions

Colliding Winds in Symbiotic Binary Systems. I. Analytic and Numerical Solutions

A Spectrographic Study of the Interacting Eclipsing Binary RY Scuti: An Episode in the Rapid Mass Loss Stage or a Protoplanetary Nebula ?

Interacting stellar winds in a binary system

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