Masses, Oxygen and Carbon abundances in CHEPS dwarf stars

Reproduced with permission from Astronomy & Astrophysics. © 2019 ESOContext. We report the results from the determination of stellar masses, carbon, and oxygen abundances in the atmospheres of 107 stars from the Calan-Hertfordshire Extrasolar Planet Search (CHEPS) programme. Our stars are drawn from a population with a significantly super-solar metallicity. At least 10 of these stars are known to host orbiting planets. Aims. In this work, we set out to understand the behaviour of carbon and oxygen abundance in stars with different spectral classes, metallicities, and V sin i within the metal-rich stellar population. Methods. Masses of these stars were determined using data from Gaia DR2. Oxygen and carbon abundances were determined by fitting the absorption lines. We determined oxygen abundances with fits to the 6300.304 Å O I line, and we used 3 lines of the C I atom and 12 lines of the C 2 molecule for the determination of carbon abundances. Results. We determine masses and abundances of 107 CHEPS stars. There is no evidence that the [C/O] ratio depends on V sin i or the mass of the star within our constrained range of masses, i.e. 0.82 5 km s -1) are massive stars.Peer reviewedFinal Published versio

A detailed study of Lithium in 107 CHEPS dwarf stars

Reproduced with permission from Astronomy & Astrophysics, © ESO 2018.Context. We report results from lithium abundance determinations using high resolution spectral analysis of the 107 metal-rich stars from the Calan-Hertfordshire Extrasolar Planet Search programme. Aims. We aim to set out to understand the lithium distribution of the population of stars taken from this survey. Methods. The lithium abundance taking account of non-local thermodynamical equilibrium effects was determined from the fits to the Li I 6708 Å resonance doublet profiles in the observed spectra. Results. We find that a) fast rotators tend to have higher lithium abundances; b) log N(Li) is higher in more massive and hot stars; c) log N(Li) is higher in stars of lower log g; d) stars with the metallicities >0.25 dex do not show the lithium lines in their spectra; e) most of our planet hosts rotate slower; and f) a lower limit of lithium isotopic ratio is 7Li/ 6Li > 10 in the atmospheres of two stars with planets (SWP) and two non-SWP stars. Conclusions. Measurable lithium abundances were found in the atmospheres of 45 stars located at distances of 20-170 pc from the Sun, for the other 62 stars the upper limits of log N(Li) were computed. We found well defined dependences of lithium abundances on T eff, V sin i, and less pronounced for the log g. In case of V sin i we see two sequences of stars: with measurable lithium and with the upper limit of log N(Li). About 10% of our targets are known to host planets. Only two SWP have notable lithium abundances, so we found a lower proportion of stars with detectable Li among known planet hosts than among stars without planets. However, given the small sample size of our planet-host sample, our analysis does not show any statistically significant differences in the lithium abundance between SWP and stars without known planets.Peer reviewe

Synthesis, Morphostructure, Surface Chemistry and Preclinical Studies of Nanoporous Rice Husk-Derived Biochars for Gastrointestinal Detoxification

This article summarizes the methodology of synthesis, surface functionalization and structural properties of rice husk-derived nanostructured carbon enterosorbents (biochars) in connection with the preliminary in vitro study results of uraemic toxin adsorption in model experiments, as well as preclinical trials in vivo. The obtained nanostructured carbon sorbents were studied using a number of modern physicochemical methods of investigation: low-temperature nitrogen adsorption, isotherms recording and calculation of the specific surface area, pore volumes were carried out using the Autosorb-1 "Quantachrome" device. Scanning electron microscopy and EDS-analysis. Mercury intrusion porosimetry analysis of the ACs were accomplished using "Quantachrome Poremaster" data analysis software. In vitro adsorption results assessed by use of HPLC and UV-spectroscopy for the nanostructured carbon sorbents with respect to the investigated low-molecule toxins suggest that the rice husks-derived carbon enterosorbents modified with the functional groups are able to reduce clinically significant levels of uraemic toxins and are comparable to the commercial enterosorbents. Based on the results of the comparative analysis for biocompatibility of canine kidney epithelial cells it was determined that the samples of the modified sorbents CRH P 450 and CRH 475 KOH 850 N do not exhibit cytotoxicity in comparison with the commercial carbon enterosorbent «Adsorbix Extra». According to the results of the in vivo studies, it was determined that there was a the positive effect of enterosorbent on uremia and intoxication

IRON ABUNDANCES IN THE ATMOSPHERES OF HD10700 and HD146233

There are many different means to determine physical parameters of stars and their abundances by spectral analysis. In our work we draw our attention to the rotational and microturbulenc velocities as well as metallicities for the stars of known effective temperature and surface gravity. We carried fits of LTE synthetic spectra to the observed spectra of HD10700 and HD146233. These stars are knows aa solar-twins except slightly higher rotational velocities in both cases and higher magnetical activity i of HD10700. We adopted ABEL software (Pavlenko Ya.V.) to fit to HD10700, HD146233 spectra obtained on Camino Observatory, Chilie. Selected stars looks like. We compare our results with previous work of Valenti and Fischer (2005)

Spectroscopy and kinematics of low-mass members of young moving groups

Original article can be found at: http://onlinelibrary.wiley.com/ Copyright Royal Astronomical SocietyWe study a target sample of 68 low-mass objects (with spectral types in the range M4.5–L1) previously selected via photometric and astrometric criteria, as possible members of five young moving groups: the Local Association (Pleiades moving group, age = 20–150 Myr), the Ursa Mayor group (Sirius supercluster, age = 300 Myr), the Hyades supercluster (age = 600 Myr), IC 2391 supercluster (age = 35–55 Myr) and the Castor moving group (age = 200 Myr). In this paper, we assess their membership by using different kinematic and spectroscopic criteria. We use high-resolution echelle spectroscopic observations of the sample to measure accurate radial velocities. Distances are calculated and compared to those of the moving group from the literature, we also calculate the kinematic Galactic components (U,V,W) of the candidate members and apply kinematic criterion of membership to each group. In addition, we measure rotational velocities (v sin i) to place further constraints on membership of kinematic members. We find that 49 targets have young disc kinematics and that 36 of them possibly belong to one of our five moving groups. From the young disc target objects, 31 have rotational velocities in agreement with them belonging to the young disc population. We also find that one of our moving group candidates, 2MASS0123−3610, is a low-mass double lined spectroscopic binary, with probable spectral types around M7.Peer reviewe