Abstract <p>We present the results of a comprehensive study of four spectroscopic binary Cepheids with long orbital periods. The study makes use of all the available photometric, spectroscopic, and astrometric information and previously developed analysis techniques. The paper is based on a new catalog containing 702 radial velocity measurements of V496 Aql (232 measurements), V1344 Aql (194 measurements), V1334 Cyg (138 measurements), and AW Per (138 measurements). All the measurements were obtained over 1997–2021 with the Zeiss-1000 telescope of the Institute of Astronomy of the Russian Academy of Sciences Simeiz Observatory using the correlation Radial Velocity Meter (RVM) designed by A.A. Tokovinin. Using other published observations, the orbital periods and other orbital parameters were significantly refined: V496 Aql: <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(P_{\textrm{orb}}\approx 1351\overset{\textrm{d}}{.}\text{}3\pm 0\overset{\textrm{d}}{.}\text{}7\)</EquationSource>  </InlineEquation>; V1344 Aql: <InlineEquation ID="IEq2"> <EquationSource Format="TEX">\(P_{\textrm{orb}}\approx 635\overset{\textrm{d}}{.}8\pm 30^{\textrm{d}}\)</EquationSource>  </InlineEquation>; V1344 Cyg: <InlineEquation ID="IEq3"> <EquationSource Format="TEX">\(P_{\textrm{orb}}\approx 1934\overset{\textrm{d}}{.}\text{}4\pm 0\overset{\textrm{d}}{.}\text{}8\)</EquationSource>  </InlineEquation>; AW Per: <InlineEquation ID="IEq4"> <EquationSource Format="TEX">\(P_{\textrm{orb}}\approx 13\,663\pm 128^{\textrm{d}}\)</EquationSource>  </InlineEquation>. Using the mass function, we have found additional constraints on the companion masses and the orientation of the orbital plane. For V496 Aql and V1344 Aql, a complete set of astrophysical parameters was found including the color excess, pulsational radii, luminosity, and mass estimates based on the evolutionary tracks (for V496 Aql, <InlineEquation ID="IEq5"> <EquationSource Format="TEX">\(M\sim 5.6{-}5.8M_{\odot}\)</EquationSource>  </InlineEquation>; for V1334 Aql, <InlineEquation ID="IEq6"> <EquationSource Format="TEX">\(M\sim 5.8{-}6.0M_{\odot}\)</EquationSource>  </InlineEquation>). For the V1334 Cyg Cepheid with a massive companion, the strong constraint <InlineEquation ID="IEq7"> <EquationSource Format="TEX">\(i\sim 56^{\circ}{-}60^{\circ}\)</EquationSource>  </InlineEquation> on the inclination of its orbital plane was found based on the high mass function. AW Per, with an orbital period of over 37 years and a high mass function, has a companion of a comparable mass. The calculated pulsational radius and luminosity of the Cepheid are in good agreement with the evolutionary mass estimate <InlineEquation ID="IEq8"> <EquationSource Format="TEX">\(M\sim 5.6{-}5.9\,M_{\odot}\)</EquationSource>  </InlineEquation>. We show that at inclination angles smaller than <InlineEquation ID="IEq9"> <EquationSource Format="TEX">\(63^{\circ}{-}65^{\circ}\)</EquationSource>  </InlineEquation>, the companion can only be a close binary system consisting of two hot stars near the main-sequence turnoff point.</p>

Orbital and Astrophysical Parameters of Spectroscopic Binary Cepheids V496 Aql, V1344 Aql, V1334 Cyg, and AW Per

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2026年3月1日

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A. S. Rastorguev,
M. V. Zabolotskikh,
N. A. Gorynya

摘要

Abstract

We present the results of a comprehensive study of four spectroscopic binary Cepheids with long orbital periods. The study makes use of all the available photometric, spectroscopic, and astrometric information and previously developed analysis techniques. The paper is based on a new catalog containing 702 radial velocity measurements of V496 Aql (232 measurements), V1344 Aql (194 measurements), V1334 Cyg (138 measurements), and AW Per (138 measurements). All the measurements were obtained over 1997–2021 with the Zeiss-1000 telescope of the Institute of Astronomy of the Russian Academy of Sciences Simeiz Observatory using the correlation Radial Velocity Meter (RVM) designed by A.A. Tokovinin. Using other published observations, the orbital periods and other orbital parameters were significantly refined: V496 Aql: \(P_{\textrm{orb}}\approx 1351\overset{\textrm{d}}{.}\text{}3\pm 0\overset{\textrm{d}}{.}\text{}7\) ; V1344 Aql: \(P_{\textrm{orb}}\approx 635\overset{\textrm{d}}{.}8\pm 30^{\textrm{d}}\) ; V1344 Cyg: \(P_{\textrm{orb}}\approx 1934\overset{\textrm{d}}{.}\text{}4\pm 0\overset{\textrm{d}}{.}\text{}8\) ; AW Per: \(P_{\textrm{orb}}\approx 13\,663\pm 128^{\textrm{d}}\) . Using the mass function, we have found additional constraints on the companion masses and the orientation of the orbital plane. For V496 Aql and V1344 Aql, a complete set of astrophysical parameters was found including the color excess, pulsational radii, luminosity, and mass estimates based on the evolutionary tracks (for V496 Aql, \(M\sim 5.6{-}5.8M_{\odot}\) ; for V1334 Aql, \(M\sim 5.8{-}6.0M_{\odot}\) ). For the V1334 Cyg Cepheid with a massive companion, the strong constraint \(i\sim 56^{\circ}{-}60^{\circ}\) on the inclination of its orbital plane was found based on the high mass function. AW Per, with an orbital period of over 37 years and a high mass function, has a companion of a comparable mass. The calculated pulsational radius and luminosity of the Cepheid are in good agreement with the evolutionary mass estimate \(M\sim 5.6{-}5.9\,M_{\odot}\) . We show that at inclination angles smaller than \(63^{\circ}{-}65^{\circ}\) , the companion can only be a close binary system consisting of two hot stars near the main-sequence turnoff point.