Hostname: page-component-cd9895bd7-lnqnp Total loading time: 0 Render date: 2024-12-26T04:28:03.850Z Has data issue: false hasContentIssue false
  • English
  • Français

Prospects for Detecting Unseen Companions of Periodic Variables

Published online by Cambridge University Press:  07 August 2017

A. Pigulski
A. Pigulski*
Affiliation:
Wrocław University Observatory, Kopernika 11, 51-622 Wrocław, Poland

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

All periodic variables with stable periods such as pulsating stars, eclipsing binaries and pulsars offer the possibility of detecting unseen companion(s) by means of the light-time effect. We discuss the limitations of the method (the visibility of the effect) for different types of periodic variables. Special attention is paid to the ranges of mass ratios and orbital periods in which unseen companions can be found. We also indicate several systems with light-time effect in which hypothetical companions can be detected by speckle interferometry or precise astrometric observations. In these cases, the detection of the companions may lead to the determination of the components' masses.

Type
2. Current and Future Needs for Very Accurate Astrometry
Information
Symposium - International Astronomical Union , Volume 166: Astronomical and Astrophysical Objectives of Sub-Milliarcsecond Optical Astrometry , 1995 , pp. 205 - 208
Copyright
Copyright © Kluwer 1995 

References

Bartolini, C. and Zoffali, M. (1986) Light-time effect in IM Aurigae, Astron. & Astroph., 168, pp. 377–379 Google Scholar
Drechsel, H., Lorenz, R. and Mayer, P. (1989) Solution of the light curves with third light contribution: the eclipsing binaries LY Aurigae and AH Cephei reconsidered, Astron. & Astroph., 221, pp. 49–61 Google Scholar
Liu, Y., Jiang, S. and Cao, M. (1991) A further proof on the binary model of HD 94033, IBVS No. 3606.Google Scholar
Mayer, P. and Drechsel, H. (1987) Up-to-date parameters of the eclipsing triple system IU Aur, Astron. & Astroph., 183, pp. 61–65 Google Scholar
Moffat, A.F.J., Vogt, N., Vaz, L.P.R. and Grønbech, B. (1983) The early B-type eclipsing binary FZ CMa (HD 52942): a masive triple system, Astron. & Astroph., 120, pp. 278–286 Google Scholar
Paparó, M., Szeidl, B. and Mahdy, H.A. (1988) The high amplitude Delta Scuti star SZ Lyncis revisited, Space Science Review, 149, pp. 73–82 CrossRefGoogle Scholar
Phinney, E.S. and Verbunt, F. (1991) Binary pulsars before spin-up and PSR 1820–11, Monthly Not. Royal Astron. Soc., 248, pp. 21P–23P CrossRefGoogle Scholar
Pigulski, A. (1993) The light-time effect as the cause of period changes in β Cephei stars. III. BW Vulpeculae, Astron. & Astroph., 274, pp. 269–273 Google Scholar
Szabados, L. (1988) Possible light-time effect in the cepheids FN Aquilae and RX Aurigae, Publ. Astron. Soc. Pacific, 100, pp. 589–593 CrossRefGoogle Scholar
Szeidl, B., Oláh, K. and Mizser, A. (1986) Period changes of RR Lyrae stars II, TW Her, VZ Her, AV Peg and TU UMa, Comm. Konkoly Obs. No. 89, pp. 57–110 Google Scholar