scholarly journals Asteroseismic analysis of 15 solar-like oscillating evolved stars

2021 ◽  
Vol 503 (3) ◽  
pp. 4529-4536
Author(s):  
Z Çelik Orhan ◽  
M Yıldız ◽  
C Kayhan
Keyword(s):  
Stellar Structure ◽  
Scaling Relations ◽  
Space Telescopes ◽  
Ionization Zone ◽  
Fundamental Parameters ◽  
Evolved Stars ◽  
Large Numbers ◽  
Analyse Data ◽  
Oscillation Frequencies

ABSTRACT Asteroseismology using space-based telescopes is vital to our understanding of stellar structure and evolution. CoRoT, Kepler, and TESS space telescopes have detected large numbers of solar-like oscillating evolved stars. Solar-like oscillation frequencies have an important role in the determination of fundamental stellar parameters; in the literature, the relations between the two is established by the so-called scaling relations. In this study, we analyse data obtained from the observation of 15 evolved solar-like oscillating stars using the Kepler and ground-based telescopes. The main purpose of the study is to determine very precisely the fundamental parameters of evolved stars by constructing interior models using asteroseismic parameters. We also fit the reference frequencies of models to the observational reference frequencies caused by the He ii ionization zone. The 15 evolved stars are found to have masses and radii within ranges of 0.79–1.47 M⊙ and 1.60–3.15 R⊙, respectively. Their model ages range from 2.19 to 12.75 Gyr. It is revealed that fitting reference frequencies typically increase the accuracy of asteroseismic radius, mass, and age. The typical uncertainties of mass and radius are ∼3–6 and ∼1–2 per cent, respectively. Accordingly, the differences between the model and literature ages are generally only a few Gyr.

scholarly journals On The Seismic Signature of the HeII Ionization Zone in Stellar Envelopes

1998 ◽  
Vol 185 ◽  
pp. 317-318
Author(s):  
Mário J.P.F.G. Monteiro ◽  
Michael J. Thompson
Keyword(s):  
Equation Of State ◽  
Stellar Structure ◽  
Ionization Zone ◽  
Characteristic Signal ◽  
Oscillation Frequencies ◽  
Stellar Envelopes ◽  
Seismic Signature ◽  
Better Than

Sharp variations of the structure of the star create a characteristic signal in its frequencies of oscillation (e.g. [3]). The zone of the second ionization of helium is such a localized feature of the structure whose properties depend mainly on the abundance of helium and the equation of state. Considering that such a signal should easily be detectable provided the frequencies are measured to rather better than 1μHz accuracy (the COROT project should measure oscillation frequencies with an accuracy of 0.1μHz), we present here a tool to study this aspect of stellar structure.

scholarly journals Fundamental properties of Kepler and CoRoT targets – IV. Masses and radii from frequencies of minimum Δν and their implications

2019 ◽  
Vol 489 (2) ◽  
pp. 1753-1769 ◽  
Author(s):  
M Yıldız ◽  
Z Çelik Orhan ◽  
C Kayhan
Keyword(s):  
Rotational Velocity ◽  
Galactic Disc ◽  
Ionization Zone ◽  
Chemical Enrichment ◽  
Fundamental Properties ◽  
Diagnostic Potential ◽  
The Difference ◽  
The Masses ◽  
Oscillation Frequencies

ABSTRACT Recently, by analysing the oscillation frequencies of 90 stars, Yıldız, Çelik Orhan & Kayhan have shown that the reference frequencies (νmin0, νmin1, and νmin2) derived from glitches due to He ii ionization zone have very strong diagnostic potential for the determination of their effective temperatures. In this study, we continue to analyse the same stars and compute their mass, radius, and age from different scaling relations including relations based on νmin0, νmin1, and νmin2. For most of the stars, the masses computed using νmin0 and νmin1 are very close to each other. For 38 stars, the difference between these masses is less than 0.024 M$\odot$. The radii of these stars from νmin0 and νmin1 are even closer, with differences of less than 0.007 R$\odot$. These stars may be the most well known solar-like oscillating stars and deserve to be studied in detail. The asteroseismic expressions we derive for mass and radius show slight dependence on metallicity. We therefore develop a new method for computing initial metallicity from this surface metallicity by taking into account the effect of microscopic diffusion. The time dependence of initial metallicity shows some very interesting features that may be important for our understanding of chemical enrichment of Galactic Disc. According to our findings, every epoch of the disc has its own lowest and highest values for metallicity. It seems that rotational velocity is inversely proportional to 1/2 power of age as given by the Skumanich relation.

Sorption of Se (IV) from aqueous solutions with subsequent determination by X-ray fluorescence analysis

2020 ◽  
Vol 86 (10) ◽  
pp. 5-9
Author(s):  
D. G. Filatova ◽  
A. A. Arkhipenko ◽  
M. A. Statkus ◽  
V. V. Es’kina ◽  
V. B. Baranovskaya ◽  
...  
Keyword(s):  
Inductively Coupled Plasma ◽  
Fluorescence Analysis ◽  
Standard Samples ◽  
Phase Contact Time ◽  
Sorbent Phase ◽  
X Ray ◽  
Fundamental Parameters ◽  
Inductively Coupled ◽  
Subsequent Determination

An approach to sorptive separation of Se (IV) from solutions on a novel S,N-containing sorbent with subsequent determination of the analyte in the sorbent phase by micro-x-ray fluorescence method is presented. The sorbent copolymethylenesulfide-N-alkyl-methylenamine (CMA) was synthesized using «snake in the cage» procedure and proven to be stable in acid solutions. Conditions for quantitative extraction of Se (IV) were determined: sorption in 5 M HCl or 0.05 M HNO3 solutions when heated to 60°C, phase contact time being 1 h. The residual selenium content in the solution was determined by inductively coupled plasma mass spectrometry (ICP-MS) using 82Se isotope. The absence of selenium losses is proved and the mechanism of sorption interaction under specified conditions is proposed. The method of micro-x-ray fluorescence analysis (micro-RFA) with mapping revealed a uniform distribution of selenium on the sorbent surface. The possibility of determining selenium in the sorbent phase by micro-RFA is shown. When comparing the obtained results with the results of calculations by the method of fundamental parameters, it is shown the necessity of using standard samples of sorbates to obtain correct results of RFA determination of selenium in the sorbent phase.

scholarly journals Solar structure and evolution

2021 ◽  
Vol 18 (1) ◽  
Author(s):  
Jørgen Christensen-Dalsgaard
Keyword(s):  
Solar Surface ◽  
Solar Neutrinos ◽  
Solar Interior ◽  
Stellar Structure ◽  
The Sun ◽  
Physical Processes ◽  
Solar Evolution ◽  
Internal Properties ◽  
Atmospheric Phenomena

AbstractThe Sun provides a critical benchmark for the general study of stellar structure and evolution. Also, knowledge about the internal properties of the Sun is important for the understanding of solar atmospheric phenomena, including the solar magnetic cycle. Here I provide a brief overview of the theory of stellar structure and evolution, including the physical processes and parameters that are involved. This is followed by a discussion of solar evolution, extending from the birth to the latest stages. As a background for the interpretation of observations related to the solar interior I provide a rather extensive analysis of the sensitivity of solar models to the assumptions underlying their calculation. I then discuss the detailed information about the solar interior that has become available through helioseismic investigations and the detection of solar neutrinos, with further constraints provided by the observed abundances of the lightest elements. Revisions in the determination of the solar surface abundances have led to increased discrepancies, discussed in some detail, between the observational inferences and solar models. I finally briefly address the relation of the Sun to other similar stars and the prospects for asteroseismic investigations of stellar structure and evolution.

ANALYSIS OF SOLDERS ON TIN AND LEAD BASES BY X-RAY FLOORESCENT SPECTROSCOPY

2021 ◽  
pp. 124-131
Author(s):  
A.V. Alekseev ◽  
◽  
G.V. Orlov ◽  
P.S. Petrov ◽  
A.V. Slavin ◽  
...  
Keyword(s):  
Emission Spectroscopy ◽  
High Resolution Mass Spectrometry ◽  
Analytical Signal ◽  
Atomic Emission ◽  
Standard Samples ◽  
X Ray ◽  
Fundamental Parameters ◽  
The Matrix ◽  
Resolution Mass

The determination of the elements Cu, Ni, Sb, Bi, Pb, Zn and Fe in the tin-based solder VPr35, as well as the elements Sn, Ni, Sb, Bi and In in the lead-based VPr40 solder by the method of х-ray fluorescence spectroscopy has been carried out. The calibration dependences are corrected taking into account the superposition of signals from interfering elements on the analytical signal and changes in intensity caused by inter-element influences in the matrix. The analysis was carried out by the method of fundamental parameters without using standard samples. The correctness of the results obtained was confirmed by their comparative analysis by atomic emission spectroscopy and high-resolution mass spectrometry with a glow discharge.

scholarly journals Using non-solar-scaled opacities to derive stellar parameters

2018 ◽  
Vol 620 ◽  
pp. A54 ◽  
Author(s):  
C. Saffe ◽  
M. Flores ◽  
P. Miquelarena ◽  
F. M. López ◽  
M. Jaque Arancibia ◽  
...  
Keyword(s):  
High Precision ◽  
Chemical Species ◽  
Model Atmosphere ◽  
Condensation Temperature ◽  
Spectroscopic Methods ◽  
Fundamental Parameters ◽  
Evolved Stars ◽  
Solar Type ◽  
Scaled Models ◽  
Previous Step

Aims. In an effort to improve spectroscopic methods of stellar parameters determination, we implemented non-solar-scaled opacities in a simultaneous derivation of fundamental parameters and abundances. We wanted to compare the results with the usual solar-scaled method using a sample of solar-type and evolved stars. Methods. We carried out a high-precision determination of stellar parameters and abundances by applying non-solar-scaled opacities and model atmospheres. Our sample is composed of 20 stars, including main sequence and evolved objects. The stellar parameters were determined by imposing ionization and excitation equilibrium of Fe lines, with an updated version of the FUNDPAR program, together with plane-parallel ATLAS12 model atmospheres and the MOOG code. Opacities for an arbitrary composition and vmicro were calculated through the opacity sampling (OS) method. We used solar-scaled models in the first step, and then continued the process, but scaled to the abundance values found in the previous step (i.e. non-solar-scaled). The process finishes when the stellar parameters of one step are the same as in the previous step, i.e. we use a doubly iterated method. Results. We obtained a small difference in stellar parameters derived with non-solar-scaled opacities compared to classical solar-scaled models. The differences in Teff, log g, and [Fe/H] amount to 26 K, 0.05 dex, and 0.020 dex for the stars in our sample. These differences can be considered the first estimation of the error due to the use of classical solar-scaled opacities to derive stellar parameters with solar-type and evolved stars. We note that some chemical species could also show an individual variation greater than those of the [Fe/H] (up to ~0.03 dex) and varying from one species to another, obtaining a chemical pattern difference between the two methods. This means that condensation temperature Tc trends could also present a variation. We include an example showing that using non-solar-scaled opacities, the solution found with the classical solar-scaled method indeed cannot always verify the excitation and ionization balance conditions required for a model atmosphere. We discuss in the text the significance of the differences obtained when using solar-scaled versus non-solar-scaled methods. Conclusions. We consider that the use of the non-solar-scaled opacities is not mandatory in every statistical study with large samples of stars. However, for those high-precision works whose results depend on the mutual comparison of different chemical species (such as the analysis of condensation temperature Tc trends), we consider its application to be worthwhile. To date, this is probably one of the most precise spectroscopic methods for stellar parameter derivation.

scholarly journals Rapid Production of Graphite Without Contamination for Biomedical AMS

Radiocarbon ◽  
1992 ◽  
Vol 34 (3) ◽  
pp. 344-350 ◽  
Author(s):  
John S. Vogel
Keyword(s):  
Isotopic Fractionation ◽  
Cross Contamination ◽  
Biological Variability ◽  
Muffle Furnace ◽  
New Class ◽  
Large Numbers ◽  
Rapid Production ◽  
Disposable Plastic ◽  
Single Reaction

The application of AMS to the detection of 14C makes possible a new class of sensitive experiments in molecular biology. Such experiments inherently produce large numbers of samples for the determination of biological variability in molecular interactions. The samples vary in 14C concentration over many orders of magnitude. We added TiH2 to aid the reduction of CO2 by zinc in a sealed tube to reproducibly make graphite without sample cross-contamination. The CO2 is transferred from a combustion tube to the reaction tube through a disposable plastic manifold. The sealed tubes are heated to a single-reaction temperature in a muffle furnace. The process is complete within 5 h. Bulk isotopic fractionation in the finished graphite is less than 0.5%.

Nucleon structure as a background for determination of fundamental parameters

1993 ◽  
Vol 48 (1) ◽  
pp. 129-136
Author(s):  
V. A. Bednyakov ◽  
Yu. P. Ivanov ◽  
S. G. Kovalenko
Keyword(s):  
Nucleon Structure ◽  
Fundamental Parameters

Direct solid-phase enzymoimmunoassay of testosterone in saliva.

1989 ◽  
Vol 35 (10) ◽  
pp. 2044-2047 ◽  
Author(s):  
K Howard ◽  
M Kane ◽  
A Madden ◽  
J P Gosling ◽  
P F Fottrell
Keyword(s):  
Detection Limit ◽  
Analytical Procedure ◽  
Solid Phase ◽  
Medical Applications ◽  
Microtiter Plates ◽  
Large Numbers ◽  
Coefficients Of Variation ◽  
Serial Sampling ◽  
Direct Solid

Abstract This competitive, solid-phase enzymoimmunoassay for testosterone in saliva is carried out on microtiter plates and involves no chromatographic or extraction steps. With an overnight incubation the detection limit of the assay is 230 fg per well (16.1 pmol/L). There was a good correlation (correlation coefficient 0.95) between testosterone concentrations measured with and without prior extraction of the saliva samples. Repeated assay of three control saliva samples containing a range of testosterone concentrations (200-1000 pmol/L) gave within- and between-assay coefficients of variation of 5.5-13.2%. The analytical procedure is simple and closely resembles already published procedures for the determination of progesterone and estrone (with extraction) in saliva. One person can assay 200 samples in 24 h and the assay is suitable for reproductive and sports medical applications, particularly for projects involving serial sampling and yielding large numbers of samples.

An electrical method of measuring non-electrolyte permeability

1969 ◽  
Vol 172 (1028) ◽  
pp. 203-225 ◽  
Keyword(s):  
Gall Bladder ◽  
Streaming Potential ◽  
Concentration Gradients ◽  
Bladder Epithelium ◽  
Electrical Method ◽  
Streaming Potentials ◽  
Unstirred Layers ◽  
Large Numbers ◽  
Tracer Methods

A rapid procedure based on that of Smyth & Wright (1966) is described for obtaining a measure of the permeability of rabbit gall-bladder epithelium to non-electrolytes. The underlying principles are that concentration gradients of permeant molecules produce lower rates of osmotic flow across a membrane than does the same gradient of an impermeant molecule, and that streaming potentials in the gall-bladder are directly proportional to the flow rate. Hence reflexion coefficients (cr’s) were calculated as the ratio of the streaming potential produced by a 0* 1 m gradient of the test solute to the streaming potential produced by a 0T m gradient of an impermeant reference solute, sucrose. The method yields results in agreement with those obtained in the gall-bladder by a zero-flow procedure. In general, the patterns of permeation derived are similar to those obtained in other tissues by the same procedure, by other osmotic procedures, or by direct chemical or tracer methods. The advantages of the method are that (a) large numbers of cr’s can be determined in one experiment with an average standard deviation of ± 8 % ; and (b) the minimum elapsed time between the preparation of a solution and the determination of or is about 90 s, so that cr’s may be obtained for some non-electrolytes subject to gradual chemical transformation in aqueous solution, such as aldehydes. The principles underlying osmotic methods of measuring permeability, and the effects of unstirred layers, are discussed.

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