UV emission line shifts of symbiotic binaries

Friedjung, M.; Mikołajewska, J.; Zajczyk, A.; Eriksson, Mattias

doi:10.1051/0004-6361/200913438

Cited by 4 publications

(3 citation statements)

References 23 publications

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“…The measured heliocentric radial velocities (see Table 2) point for a possible ionization-potential-dependent stratification in EF Aql. Similar effect is detected in the D-type symbiotic RR Tel (Kotnik-Karuza et al 2004) and in some S-type symbiotic stars (Friedjung et al 2010). A velocity stratification of various spectral lines is also detected in some Mira-type variables (Scholz 1992).…”

Section: Discussionsupporting

confidence: 76%

Optical spectroscopy and X-ray observations of the D-type symbiotic star EF Aql

Stoyanov

Iłkiewicz

Luna

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We performed high-resolution optical spectroscopy and X-ray observations of the recently identified Mira-type symbiotic star EF Aql. Based on high-resolution optical spectroscopy obtained with the Southern African Large Telescope (SALT), we determine the temperature (∼55 000 K) and the luminosity (∼5.3 L⊙) of the hot component in the system. The heliocentric radial velocities of the emission lines in the spectra reveal possible stratification of the chemical elements. We also estimate the mass-loss rate of the Mira donor star. Our Swift observation did not detect EF Aql in X-rays. The upper limit of the X-ray observations is 10−12 erg cm−2 s−1, which means that EF Aql is consistent with the faintest X-ray systems detected so far. Otherwise we detected it with the UltraViolet and Optical Telescope (UVOT) instrument with an average UVM2 magnitude of 14.05. During the exposure, EF Aql became approximately 0.2 UVM2 magnitudes fainter. The periodogram analysis of the V-band data reveals an improved period of 320.4 ± 0.3 d caused by the pulsations of the Mira-type donor star.

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Section: Discussionsupporting

confidence: 76%

Optical spectroscopy and X-ray observations of the D-type symbiotic star EF Aql

Stoyanov

Iłkiewicz

Luna

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…8) show a strong correlation with the long term optical variations (based on the AAVSO archive), especially the strong outburst between MJD 46000 and 47000. In the figure, the zero flux values are the conjunctions when it is heavily obscured (according to Friedjung et al 2010) that were otherwise well exposed (not, as in several symbiotic stars, over-or underexposures that we have ignored in the analysis).…”

Section: Notes and Correlationsmentioning

confidence: 99%

The O I] 1641 Å line as a probe of symbiotic star winds

Shore

Wahlgren

2010

A&A

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Aims. The neutral oxygen resonance λ1302 Å line can, if the optical depth is sufficiently high, de-excite by an intercombination transition at λ1641 Å to a metastable state. This has been noted in a number of previous studies but never systematically investigated as a diagnostic of the neutral red giant wind in symbiotic stars and symbiotic-like recurrent novae. Methods. We used archival IUE high resolution, and HST GHRS and STIS medium and high resolution, spectra to study a sample of symbiotic stars. The integrated fluxes were measured, where possible, for the O I λ1302 Å and O I] λ1641 Å lines. Results. The intercombination λ1641 Å line is detected in a substantial number of symbiotic stars with optical depths that give column densities comparable with direct eclipse measures (EG And) and the evolution of the recurrent nova RS Oph 1985 in outburst. In four systems (EG And, Z And, V1016 Cyg, and RR Tel), we find that the O I] variations are strongly correlated with the optical light curve and outburst activity. This transition can also be important for the study of a wide variety of sources in which an ionization-bounded H II region is imbedded in an extensive neutral medium, including active galactic nuclei, and not only for evaluations of extinction.

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“…Their emission line narrowing can then be associated with decreasing emission from the di f f use-enhanced system compared with that of the principal system, which can be both due to a decreasing wind mass loss rate and increasing ionisation with time of principal system material. V1500 Cyg is particularly instructive as the appearance of di f f use-enhanced absorption (Duerbeck and Wolf 1977) was associated with rapid line widening (Friedjung et al 1999), followed by slower line narrowing (Boyarchuk et al 1976).…”

Section: Evidence For the Presence Of Optically Thick Winds During Ou...mentioning

confidence: 99%

Do novae have optically thick winds during outburst with large deviations from spherical symmetry?

Friedjung

2011

A&A

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Context. The evidence for the presence of optically thick winds that are produced by classical novae after optical maximum has been challenged in recent papers. In addition, signs of orbital phase-dependent photometric variations, sometimes seen quite early in the development of nova outbursts, are hard to interpret in the framework of optically thick envelopes and especially winds. Aims. A general discussion of the assumption of optically thick winds with increasing ejection velocities during the early stages of novae after their explosion is needed, also to clarify ideas about novae and in particular to contribute to the understanding of the behaviour of novae V1500 Cyg and V1493 Aql, which show phase-dependent variations during the very early decline after the outburst. Methods. We considered possible ways of overcoming the apparent contradiction of phase-ependent variations through the production of deviations from spherical symmetry of the winds and made order-of-magnitude estimates for different theoretical scenarios that might produce these deviations. Results. We found that large deviations from the spherical symmetry of the optically thick winds in early phases after the explosion can easily explain the problem of variations. In particular, the presence of a magnetic field might have had a non-negligible effect on the wind of V1500 Cyg, while at the present there is not enough information available concerning V1493 Aql. Conclusions. Optically thick winds/envelopes are almost certainly present in the early stages after the optical maximum of a nova, while it is difficult to make pure Hubble-flow models fit the observations of those stages. New more detailed observational and theoretical work, in particular including the effects of magnetic fields on the winds, is needed.

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UV emission line shifts of symbiotic binaries

Cited by 4 publications

References 23 publications

Optical spectroscopy and X-ray observations of the D-type symbiotic star EF Aql

Optical spectroscopy and X-ray observations of the D-type symbiotic star EF Aql

The O I] 1641 Å line as a probe of symbiotic star winds

Do novae have optically thick winds during outburst with large deviations from spherical symmetry?

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