Cezary Galan

Chemical abundance analysis of symbiotic giants – I. RW Hya and SY Mus

The study of symbiotic systems is of considerable importance in our understanding of binary system stellar evolution in systems where mass-loss or transfer takes place. Elemental abundances are of special significance since they can be used to track mass exchange. However, there are few symbiotic giants for which the abundances are fairly well determined. Here, we present for the first time a detailed analysis of the chemical composition for the giants in the RW Hya and SY Mus systems. The analysis is based on high-resolution (R similar to 50 000), high signal-to-noise (S/N), near-IR spectra. Spectrum synthesis employing standard local thermal equilibrium (LTE) analysis and atmosphere models was used to obtain photospheric abundances of CNO and elements around the iron peak (Sc, Ti, Fe, and Ni). Our analysis reveals a significantly sub-solar metallicity, [Fe/H] similar to -0.75, for the RW Hya giant confirming its membership in the Galactic halo population and a near-solar metallicity for the SY Mus giant. The very low C-12/C-13 isotopic ratios, similar to 6-10, derived for both objects indicate that the giants have experienced the first dredge-up.

Chemical abundance analysis of symbiotic giants – III. Metallicity and CNO abundance patterns in 24 southern systems

The elemental abundances of symbiotic giants are essential to address the role of chemical composition in the evolution of symbiotic binaries, to map their parent population, and to trace their mass transfer history. However, the number of symbiotic giants with fairly well determined photospheric composition is still insufficient for statistical analyses. This is the third in a series of papers on the chemical composition of symbiotic giants determined from high resolution (R ~ 50000), near-IR spectra. Here we present results for 24 S-type systems. Spectrum synthesis methods employing standard local thermal equilibrium analysis and atmosphere models were used to obtain photospheric abundances of CNO and elements around the iron peak (Fe, Ti, Ni, and Sc). Our analysis reveals metallicities distributed in a wide range from slightly supersolar ([Fe/H] ~ +0.35 dex) to significantly subsolar ([Fe/H] ~ -0.8 dex) but principally with near-solar and slightly subsolar metallicity ([Fe/H] ~ -0.4 to -0.3 dex). The enrichment in 14N isotope, found in all these objects, indicates that the giants have experienced the first dredge-up. This was confirmed in a number of objects by the low 12C/13C ratio (5-23). We found that the relative abundance of [Ti/Fe] is generally large in red symbiotic systems.

Chemical abundance analysis of 13 southern symbiotic giants from high-resolution spectra at ∼1.56 μm

Symbiotic stars (SySt) are binaries composed of a star in the later stages of evolution and a stellar remnant. The enhanced mass-loss from the giant drives interacting mass exchange and makes these systems laboratories for understanding binary evolution. Studies of the chemical compositions are particularly useful since this parameter has strong impact on the evolutionary path. The previous paper in this series presented photospheric abundances for 24 giants in S-type SySt enabling a first statistical analysis. Here we present results for an additional sample of 13 giants. The aims are to improve statistics of chemical composition involved in the evolution of SySt, to study evolutionary status, mass transfer and to interpret this in terms of Galactic populations. High-resolution, near-IR spectra are used, employing the spectrum synthesis method in a classical approach, to obtain abundances of CNO and elements around the iron peak (Fe, Ti, Ni). Low-resolution spectra in the region around the Ca II triplet were used for spectral classification. The metallicities obtained cover a wide range with a maximum around ~-0.2 dex. The enrichment in the 14N isotope indicates that these giants have experienced the first dredge-up. Relative O and Fe abundances indicate that most SySt belong to the Galactic disc; however, in a few cases, the extended thick-disc/halo is suggested. Difficult to explain, relatively high Ti abundances can indicate that adopted microturbulent velocities were too small by ~0.2-0.3 km/s. The revised spectral types for V2905 Sgr, and WRAY 17-89 are M3 and M6.5, respectively.

Chemical abundance analysis of symbiotic giants – II. AE Ara, BX Mon, KX TrA, and CL Sco

Knowledge of the elemental abundances of symbiotic giants is essential to address the role of chemical composition in the evolution of symbiotic binaries, to map their parent population, and to trace their mass transfer history. However, there are few symbiotic giants for which the photospheric abundances are fairly well determined. This is the second in a series of papers on chemical composition of symbiotic giants determined from high-resolution (R ~ 50000) near-IR spectra. Results are presented for the late-type giant star in the AE Ara, BX Mon, KX TrA, and CL Sco systems. Spectrum synthesis employing standard local thermal equilibrium (LTE) analysis and stellar atmosphere models were used to obtain photospheric abundances of CNO and elements around the iron peak (Sc, Ti, Fe, and Ni). Our analysis resulted in sub-solar metallicities in BX Mon, KX TrA, and CL Sco by [Fe/H] ~ -0.3 or -0.5 depending on the value of microturbulence. AE Ara shows metallicity closer to solar by ~0.2 dex. The enrichment in 14N isotope found in all these objects indicates that the giants have experienced the first dredge-up. In the case of BX Mon first dredge-up is also confirmed by the low 12C/13C isotopic ratio of ~8.

A new look at the long-period eclipsing binary V383 Scorpii

V383Sco was discovered to be an eclipsing binary at the beginning of the XX century. This system has one of the longest orbital periods known (13.5yr) and was initially classified as a zet_Aur-type variable. It was then forgotten for decades. This study provides a detailed look at the V383Sco, using new data obtained around the last eclipse in 2007/8. There was a suspicion that this system could be similar to eclipsing systems with extensive dusty disks like EECep and eps_Aur. This and other, alternative hypotheses are considered. The ASAS-3 VI light curves have been used to examine photometric changes. Low-(LRS) and high-res.(HRS) spectra have been used for spectral classification, to analyse line profiles, as well as to determine the reddening, radial velocities (RVs) and distance. The SED was analysed. Using original numerical code, we performed a simplified model of the eclipse, taking into account the pulsations of one of the components. The LRS shows traces of molecular bands, characteristic of an M-type supergiant. The presence of this star in the system is confirmed by SED, by a strong dependence of the eclipse depth on the photometric bands, and by pulsational changes. The presence of a low excitation nebula around the system has been inferred from [OI] 6300A emission. Analysis of the RVs, reddening, and P-L relation for Mira-type stars imply a distance to the V383Sco of 8.4+-0.6 kpc. The distance to the nearby V381Sco is 6.4+-0.8 kpc. The very different and oppositely directed RVs of these systems (89.8 vs -178.8 km/s) seem to be in agreement with a bulge/bar kinematic model of the Galactic centre and inconsistent with purely circular motion. We have found evidence for the presence of a pulsating M-type supergiant in the V383Sco which periodically obscures the much more luminous F0I-type star, causing the deep (possibly total) eclipses which vary in duration and shape.