UV observations of the symbiotic star EG And

EG And is a S-type symbiotic star. Here is present UV observations made by IUE from 1978 to 1991. From these observations the electronic density and the electronic temperature were obtained. The size of He II emitting region was estimated as 7.3R . Line and continuum variations confirm the binary nature of EG And.     

Reticon observations of the yellow symbiotic star AG Draconis

Reticon spectroscopic observations of the yellow symbiotic star AG Draconis are reported. Small rapid (15–30 min) changes in the intensities of the Hei λ5015 Å and Hei λ6678 Å singlet lines, and of the Hγ line are observed. The first observational evidence of presence of the unidentified band at 7088 Å in this star is also reported.     

Classical symbiotic star Z And during the recent activity period

The results of study of the classical symbiotic star Z And during the recent activity period that began in 2000 are presented. Up to now series of six outbursts took place. Comparison of observational data with the results of gasdynamic modeling allow us to suggest the possible scenario for activity in this system describing all stages of an outburst development—from the mechanism of transition to the outburst and outburst development to the behavior of the system during all the activity period. Particularly, the proposed scenario explains the principal difference between outbursts—the presence of high-velocity bipolar collimated optical outflows in strong recurring outbursts. We have not found contradictions with the available data for previous outbursts of Z And. We assume that the proposed scenario could be also typical for other classic symbiotic stars. In order to check and improve our model additional observations are highly desirable and the UV spectral range could provide us with very useful data.     

Spectroscopic and photometric observations of the eclipsing star UV Leo

High-resolution spectroscopic observations around the Hα line and BVRI photometry of the eclipsing short-period RS CVn star UV Leo are presented. The simultaneous light-curve solution and radial velocity-curve solution led to the following values of the global parameters of the binary: temperatures   T ₁= 6000 ± 100 K  and   T ₂= 5970 ± 20 K  ; masses   M ₁= 0.976 ± 0.067 M_⊙  and   M ₂= 0.931 ± 0.052 M_⊙  ; separation   a = 3.716 ± 0.048 R_⊙  ; orbital inclination     ; radii   R ₁= 1.115 ± 0.052 R_⊙  and   R ₂= 1.078 ± 0.051 R_⊙  ; equatorial velocities   V ₁= 98.8 ± 2.3 km s⁻¹  and   V ₂= 89.6 ± 2.7 km s⁻¹  . These results lead to the conclusion that the two components of UV Leo are slightly oversized for their masses and lie within the main-sequence band on the mass–radius diagram, close to the isochrone 9 × 10¹⁰ yr.     

The symbiotic binary system EG Andromedae

Photometric observations of the symbiotic star EG and confirm that the binary system is eclipsing. The epoch of primary minimum is computed. The new period 474 days instead of 470 days is estimated by a comparison of line profiles of Balmer lines taken in 1967–69 and 1982–84. The new ephemeris is 1 $$JD_{min.} = 2 446 336.7 + 474 E.$$      

Circumstellar matter in the symbiotic binary EG and

We present a quantitative model of a proposed common slowly expanding envelope corotating with a symbiotic binary system. The geometry of the envelope is defined by the equipotential surface containing the Lagrangian pointL ₂. The model was applied to the symbiotic binary EG And. The orbital inclination,i = 45°, and mass ratio of the cool to the hot component,q = 2.8–3.0, are determined. The nature of the primary as well as the secondary minima in the light curves, development of the line profiles, radial velocities and equivalent widths of the H line through an orbital revolution are explained by this model.     

Photometric and spectroscopic observations of the variable star ET And. II

New spectroscopic and photometric observations of the variable Ap star ET And carried out 1982 and 1983 confirm once again the existence of short-time variations. For the radial velocity variations a period of 0.19771 days and for the light variations a period of 0.0989 days was found. Some spectrograms show a velocity progression of the Balmer lines. The gradient is of such a kind that the radial velocity values increase from the line H_γ to H₁₅. Different models for the interpreation of the velocity progression are discussed.     

Photometric and spectrophotometric observations of the classical symbiotic star YY Her during its return to quiescence

We present new photometric UBVRI and spectroscopic observations of the symbiotic star YY Her during its return to quiescence after a strong outburst in 1993. High-resolution spectra of YY Her at similar phases at outburst maximum ?=0.48) and in quiescence ?=0.37) are presented for the first time. The ephemeris of YY Her has been refined P=586^d). The last two observed minima (in 1999 and 2000) differed radically in shape from the 1997 minimum described previously. Both were sharp and deep $(\Delta U \sim 1\mathop .\limits^m 6, \Delta V \sim 0\mathop .\limits^m 9)$ . To explain this shape of the V light curve, which is only slightly affected by nebular emission, it should be assumed that the cool component of YY Her fills much of its Roche lobe and has a hot spot on the hemisphere facing the hot component. The emission spectrum rich in Fe II lines, which is characteristic of symbiotic stars, was observed during the outburst, but high-ionization lines (He II λ4686) were also observed. The He I λλ5876, 7065 lines exhibit distinct P Cyg profiles; the centers of the absorption components are shifted from the emission ones by V _r≈100 km s^?1, suggesting moderate outflow velocities.     

Periodic variations in the symbiotic star spectra

Periodic variations of emission line intensities and radial velocities in three S-type symbiotic stars: BF Cyg, CI Cyg and AX Per are presented and discussed. The behavior of emission lines is different in these objects and suggests that significant differences in physical conditions and geometry may occur in these seemingly similar systems.Paper presented at the IAU Colloquium No. 93 on Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments, held at Dr. Remeis-Sternwarte Bamberg, F.R.G., 16–19 June, 1986.     

Spectroscopic observations of the classical symbiotic star V1413 AQL at the phase of its transition to quiescence

We present the results of our spectroscopic and photometric observations of the classical symbiotic star V1413 Aql in 2003–2007, which cover the transition phase of its hot component from activity to quiescence. Various quiescence criteria for the hot component of the system are analyzed. Judging by its photometric characteristics, the system had not yet returned to quiescence by 2007, although a fairly strong He II λ4686 Å line observed previously during quiescence in 1993 appeared in its spectrum. We model the continuum energy distribution for V1413 Aql based on a standard three-component model and a model with an accretion disk. Analysis of the forbidden [O III] and [Ne III] lines shows that the neon abundance in V1413 Aql may be enhanced with respect to the oxygen abundance. The cool component of V1413 Aql has been found to be a variable M5-type red giant, with the variability amplitude at λ = 7500 Å being at least 2 ^m .     

Eclipsing phenomena of the symbiotic star CH Cygni

Eclipsing phenomena of the inner binary with a period of 756 d in the triple symbiotic system CH Cyg may have been detected in detailed spectrophotometric observations. The eclipse of the hot component by the red giant started on 1994 October 11 and finished between 1995 January 8 and 18. The ingress duration was less than one day. The radius of the red giant is estimated to be 288 ± 15 R⊙ from the duration of the eclipse. Assuming the bolometric correction of the red giant (M7 III) as 4, the distance to this object is estimated to be 307 ± 32 pc, which agrees well with that obtained in the observations by Hipparcos . The interstellar extinction in the direction of this object may be much lower than that in the nearby areas. It has been suggested that the outer binary system with an orbital period of about 15 yr is an eclipsing one. It seems unlikely, however, that the variation of the activity of this object with a time-scale of more than 10 yr was a result of eclipses.     

Orbital eccentricity of the symbiotic star MWC 560

We present projected rotational velocity measurements of the red giant in the symbiotic star MWC 560, using the high‐resolution spectroscopic observations with the FEROS spectrograph. We find that the projected rotational velocity of the red giant is v sin i = 8.2 ± 1.5 km s^–1, and estimate its rotational period tobe P_rot = 144–306 days. Using the theoretical predictions of tidal interaction and pseudosynchronization, we estimate the orbital eccentricity e = 0.68–0.82. We briefly discuss the connection of our results with the photometric variability of the object (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Infrared observations of symbiotic stars

Near infrared measurements in the J, H and K bands have been carried out for a number of symbiotic stars with the 1.5 m telescope at the Rothney Astrophysical Observatory (RAO). A comparison with the earlier observations shows that the S-type symbiotic stars do not have any significant variation in the infrared flux over the past five years. However a small variation ∼ 0.3 magnitude in the infrared flux has been detected for CH Cygni. The observations of HM Sagittae show large decreases in the infrared flux compared to the previous measurements. The variability in the infrared fluxes of both these objects could be attributed to a variation in the temperature due to the cooling of the dust shell. The variability observed for V1016 Cygni is found consistent with the previous measurements.     

A model for symbiotic star Z Andromedae

An analysis of the results of observations of the symbiotic star Z And has shown that no definite model can be derived at present on their basis. If the hot component is essentially an accreting white dwarf with a hydrogen-burning shell source, then the gas envelope must be optically thin for Lc-emission and itsT _e must be in the neighborhood of 2.6×10⁴K. And if the hot component is a Main-Sequence star with an accretion disk around it, then it is classified with red dwarfs. The electron temperature of the gas envelope must be 1.5×10⁴K. The luminosity of the hot component at the minimum of its visual brightness is only a few times lower than its Eddington limit. Therefore, as the accretion rate goes up, the initial increase in its brightness (U1 ^m .5), unaccompanied by any perceptible changes in the spectrum of Z And, will be followed by disintegration of the regular disk and flare of the star in the visible range. In the same model, partial eclipses of the hot source must occur. They seem to be observable on the star's light curve in theU band. Substitution of a solar-type star for the first-named component in the binary red dwarf + red giant system will lead to a significant decrease in the excitation of the combination spectrum.     

Photometric minimum confirmation and eclipse modelling for the symbiotic system EG Andromedae

Photometric observations carried out from October to November 1991 of the symbiotic system EG Andromedae are here presented. The secondary minimum has been repeated with a period of about 480 days, as inferred from the orbital elements (P = 482 days, Skopalet al., 1991). The light curve shape led us to suggest a model in which two hot spots result through evaporation from a low mass red giant by a compact object.