Broad H<i>α</i>wings from the optically thin stellar wind of the hot components in symbiotic binaries

Skopal, A.

doi:10.1051/0004-6361:20064935

Cited by 46 publications

(83 citation statements)

References 32 publications

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“…L = 2700 ± 700 L and L H = (1.4 ± 0.4) × 10 47 s −1 ), as representative values for the active A21, page 6 of 10 phases of AG Dra, Z And, AX Per, AE Ara, and AR Pav. The parameters v ∞ andṀ for these systems are available in Table 1 of Skopal (2006) and Table 7 of Skopal et al (2011). The X(Ṁ) quantities of active symbiotic stars lie well within the possibility of creation of the flared neutral disk-like zone predicted by the WCZ model (the grey belt in Fig.…”

Section: (ṁ) Relationship During Active Phasesmentioning

confidence: 52%

“…Calculations were performed for i.c. Table 1 of Skopal 2006). To compare the observed values of n H with the model (i.e.…”

Section: Column Density Of the Neutral Hydrogenmentioning

confidence: 99%

“…Mürset et al 1991;Mikołajewska et al 2002;Skopal 2005). Using the Hα method, Skopal (2006) found that the mass loss rate of the hot star during quiescent phases is significantly smaller, being of a few ×10 −8 M yr −1 .…”

Section: Introductionmentioning

confidence: 99%

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Ionization structure of hot components in symbiotic binaries during active phases

Cariková

Skopal

2012

A&A

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Context. During active phases of symbiotic binaries, an optically thick medium in the form of a flared disk develops around their hot stars. During quiescent phases, this structure is not evident. Aims. We propose the formation of a flared neutral disk-like structure around the rotating white dwarf (WD) in symbiotic binaries. Methods. We applied the wind compression model and calculated the ionization boundaries in the compressed wind from the WD using the equation of photoionization equilibrium. Results. During active phases, the compression of the enhanced wind from the rotating WD can form a neutral disk-like zone at the equatorial plane, while the remainder of the sphere above/below the disk is ionized. The hydrogen column density throughout the neutral zone and the emission measure of the ionized fraction of the wind, calculated for the mass loss rate from the WD, M = 2 × 10 −6 M yr −1 with v ∞ = 2000 km s −1 , are consistent with those derived from observations. During quiescent phases, the neutral disk-like structure cannot be created because of insufficient mass loss rate. Conclusions. Formation of the neutral disk-like zone at the equatorial plane is connected with the enhanced wind from the rotating WD, observed during active phases of symbiotic binaries. This probably represents a common origin of warm pseudophotospheres, indicated in the spectrum of active symbiotic binaries with a high orbital inclination.

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Section: (ṁ) Relationship During Active Phasesmentioning

confidence: 52%

“…Calculations were performed for i.c. Table 1 of Skopal 2006). To compare the observed values of n H with the model (i.e.…”

Section: Column Density Of the Neutral Hydrogenmentioning

confidence: 99%

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Ionization structure of hot components in symbiotic binaries during active phases

Cariková

Skopal

2012

A&A

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“…According to Skopal (2006), during active phases, the enhanced wind from the hot star becomes a vital source of the nebular radiation in the system. In addition, an optically thick warm (1-2×10 4 K) source develops during the active phases around the hot star (e.g.…”

Section: Introductionmentioning

confidence: 99%

Recent photometry of symbiotic stars

et al. 2012

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We present new multicolour (UBVRCIC) photometric observations of classical symbiotic stars, EG And, Z And, BF Cyg, CH Cyg, CI Cyg, V1329 Cyg, TX CVn, AG Dra, Draco C1, AG Peg, and AX Per, carried out between 2007.1 and 2011.9. The aim of this paper is to present new data of our monitoring programme, to describe the main features of their light curves (LC) and to point problems for their future investigation. The data were obtained by the method of the classical photoelectric and CCD photometry.

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“…Skopal 2006) and T Tauri stars (e.g, Edwards et al 1987). Raman scattering of Lyβ, which leads to Hα with a width a factor 6.4 larger than the Lyβ width and a λ −2 wing profile, was proposed as the best mechanism to explain them (Arrieta & TorresPeimbert 2003;ATP03).…”

Section: Broad Hα Emission From the Central Regions Of Ppnementioning

confidence: 99%

Understanding the immediate progenitors of planetary nebulae

Sahai¹,

Morris²,

Contreras³

et al. 2011

Proc. IAU

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Abstract. Pre-Planetary Nebulae (PPNe) are believed to represent a relatively short, intermediate evolutionary phase in the evolution of AGB stars to Planetary Nebulae (PNe). Our unbiased, high-resolution imaging surveys with HST of young PNe and PPNe show very strong morphological similarities between these classes, enabling us to extend our morphological scheme for PPN classification to young PNe, preserving virtually all of the primary and secondary descriptors, and adding a few new ones. These morphological surveys show that the primary shaping of PNe begins during the PPNe and/or late-AGB phase, and the key to understanding the shaping process lies in the study of these PNe progenitors. Here we present results from two recent studies of PNe progenitors: (i) Hα emission with very broad wings and P-Cygni profiles as probes of the region where the fast post-AGB outflows that do the shaping are most likely launched from, and (ii) equatorial waists with large-sized dust grains and large masses.

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Broad Hαwings from the optically thin stellar wind of the hot components in symbiotic binaries

Cited by 46 publications

References 32 publications

Ionization structure of hot components in symbiotic binaries during active phases

Ionization structure of hot components in symbiotic binaries during active phases

Recent photometry of symbiotic stars

Understanding the immediate progenitors of planetary nebulae

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