Scholarlink

Abstract <p>Results of infrared photometric observations of RW LMi in the <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(JHKLM\)</EquationSource> <!--ASPBull2560067Vakhonin-m1--> </InlineEquation> bands are presented. The observations were carried out from 1994 to 2024. Based on the observations of 17 pulsation cycles of the star, new brightness ephemerides were established: <InlineEquation ID="IEq2"> <EquationSource Format="TEX">\({\textrm{JD}}_{\textrm{max}}=2459677\overset{\textrm{d}}{.}0+610\overset{\textrm{d}}{.}9\,E\)</EquationSource> <!--ASPBull2560067Vakhonin-m2--> </InlineEquation>. A sinusoidal trend of the average brightness level was found. Its period is about 7300 days and its amplitude is approximately <InlineEquation ID="IEq3"> <EquationSource Format="TEX">\(1^{\textrm{m}}\)</EquationSource> <!--ASPBull2560067Vakhonin-m3--> </InlineEquation> in the <InlineEquation ID="IEq4"> <EquationSource Format="TEX">\(JHK\)</EquationSource> <!--ASPBull2560067Vakhonin-m4--> </InlineEquation> bands. From the energy distribution in the spectrum in the wavelength range of 0.5–100 <InlineEquation ID="IEq5"> <EquationSource Format="TEX">\(\mu\)</EquationSource> <!--ASPBull2560067Vakhonin-m5--> </InlineEquation>m, an estimate of the bolometric flux at the maximum brightness was obtained: <InlineEquation ID="IEq6"> <EquationSource Format="TEX">\(F_{\textrm{bol}}=2.6\times 10^{-6}\)</EquationSource> <!--ASPBull2560067Vakhonin-m6--> </InlineEquation> erg s<InlineEquation ID="IEq7"> <EquationSource Format="TEX">\({}^{-1}\)</EquationSource> <!--ASPBull2560067Vakhonin-m7--> </InlineEquation> cm<InlineEquation ID="IEq8"> <EquationSource Format="TEX">\({}^{-2}\)</EquationSource> <!--ASPBull2560067Vakhonin-m8--> </InlineEquation>. This corresponds to the luminosity <InlineEquation ID="IEq9"> <EquationSource Format="TEX">\(L_{\textrm{max}}\approx 8500\;L_{\odot}\)</EquationSource> <!--ASPBull2560067Vakhonin-m9--> </InlineEquation>. Modeling the RW LMi circumstellar envelope radiation was performed with the <Emphasis FontCategory="NonProportional">RAMDC-3D</Emphasis> program. The simulation was carried out in the approximation of a spherically symmetric envelope shape with a constant mass-loss rate. The main envelope parameters are: the optical depth <InlineEquation ID="IEq10"> <EquationSource Format="TEX">\(\tau_{V}\approx 12.7\)</EquationSource> <!--ASPBull2560067Vakhonin-m10--> </InlineEquation>, the inner radius <InlineEquation ID="IEq11"> <EquationSource Format="TEX">\(R_{\textrm{in}}\approx 8\)</EquationSource> <!--ASPBull2560067Vakhonin-m11--> </InlineEquation> AU, the outer radius <InlineEquation ID="IEq12"> <EquationSource Format="TEX">\(R_{\textrm{out}}\approx 17\,000\)</EquationSource> <!--ASPBull2560067Vakhonin-m12--> </InlineEquation> AU, and the mass-loss rate <InlineEquation ID="IEq13"> <EquationSource Format="TEX">\(\dot{M}=6\times 10^{-6}M_{\odot}\)</EquationSource> <!--ASPBull2560067Vakhonin-m13--> </InlineEquation> yr<InlineEquation ID="IEq14"> <EquationSource Format="TEX">\({}^{-1}\)</EquationSource> <!--ASPBull2560067Vakhonin-m14--> </InlineEquation>.</p>

错误：搜索内容不能为空，请输入英文关键词
错误：关键词超出字数限制，请精简
高级检索

Dust Envelope around the Carbon Star RW LMi

  • 期刊论文

  • 发表日期：

    2026年3月1日

查看全文
  • A. A. Vakhonin,
  • B. S. Safonov,
  • I. A. Strakhov,
  • A. M. Tatarnikov,
  • V. I. Shenavrin

摘要

Abstract

Results of infrared photometric observations of RW LMi in the \(JHKLM\) bands are presented. The observations were carried out from 1994 to 2024. Based on the observations of 17 pulsation cycles of the star, new brightness ephemerides were established: \({\textrm{JD}}_{\textrm{max}}=2459677\overset{\textrm{d}}{.}0+610\overset{\textrm{d}}{.}9\,E\) . A sinusoidal trend of the average brightness level was found. Its period is about 7300 days and its amplitude is approximately \(1^{\textrm{m}}\) in the \(JHK\) bands. From the energy distribution in the spectrum in the wavelength range of 0.5–100 \(\mu\) m, an estimate of the bolometric flux at the maximum brightness was obtained: \(F_{\textrm{bol}}=2.6\times 10^{-6}\) erg s \({}^{-1}\) cm \({}^{-2}\) . This corresponds to the luminosity \(L_{\textrm{max}}\approx 8500\;L_{\odot}\) . Modeling the RW LMi circumstellar envelope radiation was performed with the RAMDC-3D program. The simulation was carried out in the approximation of a spherically symmetric envelope shape with a constant mass-loss rate. The main envelope parameters are: the optical depth \(\tau_{V}\approx 12.7\) , the inner radius \(R_{\textrm{in}}\approx 8\) AU, the outer radius \(R_{\textrm{out}}\approx 17\,000\) AU, and the mass-loss rate \(\dot{M}=6\times 10^{-6}M_{\odot}\) yr \({}^{-1}\) .