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Abstract <p>The article presents the results of spectroscopic observations of poorly studied variable star AS 357, proving that it is an S-type symbiotic star. The object’s spectrum contains TiO molecular bands; bright emission lines of H I, He I, [O II], [O III], [N II]; a weak line of He II; etc. Photometric observations show that the system is a long-period variable with a period of <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\( \sim {\kern 1pt} {850^d}\)</EquationSource> <!--AstEng2570244Maslennikova-m1--> </InlineEquation>. This is likely the system’s orbital period. Estimates were obtained for the temperature of the hot component, <InlineEquation ID="IEq2"> <EquationSource Format="TEX">\({T_{\text{h}}} \approx 55\,000\)</EquationSource> <!--AstEng2570244Maslennikova-m2--> </InlineEquation> K, and its luminosity, <InlineEquation ID="IEq3"> <EquationSource Format="TEX">\({L_{\text{h}}} \approx 1300{\kern 1pt} {L_ \odot }\)</EquationSource> <!--AstEng2570244Maslennikova-m3--> </InlineEquation>. The spectral class of the cold component is M3 III, with a luminosity of <InlineEquation ID="IEq4"> <EquationSource Format="TEX">\({L_{\text{c}}} = (2500{-} 3400){\kern 1pt} {L_ \odot }\)</EquationSource> <!--AstEng2570244Maslennikova-m4--> </InlineEquation> and a radius of <InlineEquation ID="IEq5"> <EquationSource Format="TEX">\({R_{\text{c}}} = (130{-} 150){\kern 1pt} {R_ \odot }\)</EquationSource> <!--AstEng2570244Maslennikova-m5--> </InlineEquation>. There is excess radiation in the short-wavelength region of the spectrum that can be attributed to an accretion disk around the hot component. The study is partially based on a talk presented at the Modern Stellar Astronomy 2025 conference.</p>

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AS 357 Is a New Symbiotic Star

  • 期刊论文

  • 发表日期：

    2025年12月1日

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  • M. A. Maslennikova,
  • A. M. Tatarnikov,
  • A. A. Tatarnikova,
  • A. V. Dodin,
  • B. S. Safonov

摘要

Abstract

The article presents the results of spectroscopic observations of poorly studied variable star AS 357, proving that it is an S-type symbiotic star. The object’s spectrum contains TiO molecular bands; bright emission lines of H I, He I, [O II], [O III], [N II]; a weak line of He II; etc. Photometric observations show that the system is a long-period variable with a period of \( \sim {\kern 1pt} {850^d}\) . This is likely the system’s orbital period. Estimates were obtained for the temperature of the hot component, \({T_{\text{h}}} \approx 55\,000\) K, and its luminosity, \({L_{\text{h}}} \approx 1300{\kern 1pt} {L_ \odot }\) . The spectral class of the cold component is M3 III, with a luminosity of \({L_{\text{c}}} = (2500{-} 3400){\kern 1pt} {L_ \odot }\) and a radius of \({R_{\text{c}}} = (130{-} 150){\kern 1pt} {R_ \odot }\) . There is excess radiation in the short-wavelength region of the spectrum that can be attributed to an accretion disk around the hot component. The study is partially based on a talk presented at the Modern Stellar Astronomy 2025 conference.