Does The System Theta Virginis Represent A New Class of Pulsating Star?

Beardsley, W. R.; Zizka, E. R.

doi:10.1017/s0252921100052532

Cited by 2 publications

(1 citation statement)

References 5 publications

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“…Various orbital solutions for this pair were published in the literature. According to comments received from the author of the MSC (Tokovinin 2018), Dr. A. Tokovinin, the solution with the semimajor axis and orbital period of a = 0 219 and P = 33 yr is certainly wrong, and the solution a = 0 116 and P = 17.8 yr (Beardsley & Zizka 1977) is inconsistent with speckle observations (A. A.…”

Section: Hd 114330 = Wds 13099-0532 = θ Virmentioning

confidence: 99%

Searching For Wide Binary Stars with Non-coeval Components in the Southern Sky

Knyazev

Malkov

2023

Res. Astron. Astrophys.

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We have completed our observational programme to search for wide binary systems with non-coeval components in the southern sky and report our results here. The final set of four systems was spectroscopically investigated in this paper. No binary systems with components of different ages were found among them. Taking into account our previous studies, we estimate the fraction of such binaries (i.e., binaries formed, presumably, by capture) not higher than 0.06 per cent. The study will be continued on the northern sky.

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Section: Hd 114330 = Wds 13099-0532 = θ Virmentioning

confidence: 99%

Searching For Wide Binary Stars with Non-coeval Components in the Southern Sky

Knyazev

Malkov

2023

Res. Astron. Astrophys.

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The spectroscopic binaries 21 Her andγGem

Lehmann

Andrievsky²,

Егорова

et al. 2002

A&A

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Abstract. In the framework of a search campaign for short-term oscillations of early-type stars we analysed recently obtained spectroscopic and photometric observations of the early A-type spectroscopic binaries 21 Her and γ Gem. From the radial velocities of 21 Her we derived an improved orbital period and a distinctly smaller eccentricity in comparison with the values known up to now. Moreover, fairly convincing evidence exists for an increase of the orbital period with time. In addition to the orbital motion we find further periods in the orbital residuals. The longest period of 57.d 7 is most likely due to a third body which has the mass of a brown dwarf, whereas the period of 1.d 48 could be related to the half rotational period of the star. For the spectral types we deduced A1 III for the primary and M for the secondary. Two further periods of 0.d 21 and 0. d 22 give hint to the existence of short-term pulsations in 21 Her. Their period difference is of the order of the expected rotational period so that one possible explanation could be rotational splitting of nonradial pulsation modes. Because of the very strong aliasing of the data this finding has to be confirmed by observations having a more suitable time sampling, however. The analysis of photometric series and the Hipparcos photometry give no certain evidence for periodic light variations. For γ Gem, besides the orbital RV variation, no variations with amplitudes larger than about 100 m s −1 could be detected. The orbital elements of γ Gem are only slightly changed compared to the previously known orbital solution by including our new radial velocities, but their accuracy is improved. For some chemical elements we determined their abundances, NLTE values of C, O, and Na as well as LTE values of Mg, Sc, Fe, Cr, and Ti. We find the abundances to be rather close to the solar values, only carbon shows a little underabundance.

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Does The System Theta Virginis Represent A New Class of Pulsating Star?

Cited by 2 publications

References 5 publications

Searching For Wide Binary Stars with Non-coeval Components in the Southern Sky

Searching For Wide Binary Stars with Non-coeval Components in the Southern Sky

The spectroscopic binaries 21 Her andγGem

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