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High-resolution Spectroscopy and Spectropolarimetry of Selected Delta Scuti Pulsating Variables
Solar and Stellar Astrophysics · Submitted 11 Jan 2017
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The location of these stars in the H-R diagram demonstrate that all the sample stars are evolved from the Zero-Age-Main-Sequence towards Terminal-Age-Main-Sequence and occupy the region of $\delta$ Sct instability strip.
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The abstract, sentence by sentence
The combination of photometry, spectroscopy and spectropolarimetry of the chemically peculiar stars often aims to study the complex physical phenomena such as stellar pulsation, chemical inhomogeneity, magnetic field and their interplay with stellar atmosphere and circumstellar environment. The prime objective of the present study is to determine the atmospheric parameters of a set of Am stars to understand their evolutionary status. Atmospheric abundances and basic parameters are determined using full spectrum fitting technique by comparing the high-resolution spectra to the synthetic spectra. To know the evolutionary status we derive the effective temperature and luminosity from different methods and compare them with the literature. The location of these stars in the H-R diagram demonstrate that all the sample stars are evolved from the Zero-Age-Main-Sequence towards Terminal-Age-Main-Sequence and occupy the region of $\delta$ Sct instability strip. The abundance analysis shows that the light elements e.g. Ca and Sc are underabundant while iron peak elements such as Ba, Ce etc. are overabundant and these chemical properties are typical for Am stars. The results obtained from the spectropolarimetric analysis shows that the longitudinal magnetic fields in all the studied stars are negligible that gives further support their Am class of peculiarity.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The combination of photometry, spectroscopy and spectropolarimetry of the chemically peculiar stars often aims to study the complex physical phenomena such as stellar pulsation, chemical inhomogeneity, magnetic field and their interplay with stellar atmosphere and circumstellar environment. | background 1.00 | 0.07 | 0.02 | asserted 0.77 |
| s1 | The prime objective of the present study is to determine the atmospheric parameters of a set of Am stars to understand their evolutionary status. | contribution 0.97 | 0.35 | 0.05 | asserted 0.94 |
| s2 | Atmospheric abundances and basic parameters are determined using full spectrum fitting technique by comparing the high-resolution spectra to the synthetic spectra. | method 1.00 | 0.91 | 0.03 | asserted 1.00 |
| s3 | To know the evolutionary status we derive the effective temperature and luminosity from different methods and compare them with the literature. | method 0.90 | 0.92 | 0.04 | asserted 0.83 |
| s4 | The location of these stars in the H-R diagram demonstrate that all the sample stars are evolved from the Zero-Age-Main-Sequence towards Terminal-Age-Main-Sequence and occupy the region of $\delta$ Sct instability strip. | result 0.69 | 0.90 | 0.41 | asserted 1.00 |
| s5 | The abundance analysis shows that the light elements e.g. Ca and Sc are underabundant while iron peak elements such as Ba, Ce etc. are overabundant and these chemical properties are typical for Am stars. | result 0.98 | 0.92 | 0.18 | asserted 1.00 |
| s6 | The results obtained from the spectropolarimetric analysis shows that the longitudinal magnetic fields in all the studied stars are negligible that gives further support their Am class of peculiarity. | result 0.79 | 0.95 | 0.17 | asserted 0.99 |
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Original abstract
The combination of photometry, spectroscopy and spectropolarimetry of the chemically peculiar stars often aims to study the complex physical phenomena such as stellar pulsation, chemical inhomogeneity, magnetic field and their interplay with stellar atmosphere and circumstellar environment. The prime objective of the present study is to determine the atmospheric parameters of a set of Am stars to understand their evolutionary status. Atmospheric abundances and basic parameters are determined using full spectrum fitting technique by comparing the high-resolution spectra to the synthetic spectra. To know the evolutionary status we derive the effective temperature and luminosity from different methods and compare them with the literature. The location of these stars in the H-R diagram demonstrate that all the sample stars are evolved from the Zero-Age-Main-Sequence towards Terminal-Age-Main-Sequence and occupy the region of $\delta$ Sct instability strip. The abundance analysis shows that the light elements e.g. Ca and Sc are underabundant while iron peak elements such as Ba, Ce etc. are overabundant and these chemical properties are typical for Am stars. The results obtained from the spectropolarimetric analysis shows that the longitudinal magnetic fields in all the studied stars are negligible that gives further support their Am class of peculiarity.
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Since for cooler stars ( $<$ 8000 K), the hydrogen lines are the best indicator of , hence we used the $H_β$ line fitting technique implemented within IDL-based SME[<http://www.stsci.edu/ṽalenti/sme.html>] (Spectroscopy Made Easy) software written by [ref] .
Spectroscopy Made Easy: Evolution · Spectroscopic Indicators · 1.00
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