V2653 Ophiuchii with a pulsating component and Ppuls – Porb, Ppuls – g correlations for γ Dor type pulsators

Çakırlı, Ö.; İbanoǧlu, C.

doi:10.1016/j.newast.2015.10.003

Cited by 11 publications

(4 citation statements)

References 51 publications

(36 reference statements)

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“…Similar studies for other pulsating stars in binaries were made by Cakırlı & İbanoǧlu (2016), who found similar correlations between pulsation-orbital periods and pulsation period -log g for the γ Dor-binary members, and by Skarka et al (2016) who published a review for RR Lyrae type pulsators in binary systems.…”

Section: Introductionsupporting

confidence: 71%

Catalogue and properties of δ Scuti stars in binaries

Liakos

Niarchos

2016

Mon. Not. R. Astron. Soc.

104

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The catalogue contains 199 confirmed cases of binary systems containing at least one pulsating component of δ Sct type. The sample is divided into subgroups in order to describe the properties and characteristics of the δ Sct type stars in binaries according to their Roche geometry. Demographics describing quantitatively our knowledge for these systems as well as the distributions of their pulsating components in the Mass-Radius, Colour-Magnitude and Evolutionary Status-Temperature diagrams are presented and discussed. It is shown that a threshold of ∼13 days of the orbital period regarding the influence of binarity on the pulsations is established. Finally, the correlations between the pulsation periods and the orbital periods, evolutionary status, and companion's gravity influence are updated based on the largest sample to date.

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Section: Introductionsupporting

confidence: 71%

Catalogue and properties of δ Scuti stars in binaries

Liakos

Niarchos

2016

Mon. Not. R. Astron. Soc.

104

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“…If P puls /P orb > 0.1, the star does not pulsate in pmodes, while if P puls /P orb < 0.07, the pulsation could be of p-modes. The studies which claim that there is an exact relation between pulsation and orbital periods can be increased with the samples of Soydugan et al (2006) andÇ akırlı andIbanoglu (2016).…”

Section: Summery and Discussionmentioning

confidence: 99%

STEREO observations of hybrid stars V775 Tau and V483 Tau

Özuyar

2018

Astrophys Space Sci

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In this study, pulsational and physical characteristics of two δ Scuti stars, V775 Tau and V483 Tau, are analysed by using four-year high-precision photometric data of the STEREO satellite. Thus, it is aimed to gain new insights into behaviours of these pulsators and evolution of δ Scuti, γ Dor and Am type stars. The data are taken between 2007-2011 and examined with the help of the Lomb-Scargle method. The detection precision in the four-year combined data is around 10 −5 cd −1 in frequency and 10 −5 mag in amplitude. It is revealed that V775 Tau exhibits weak pulsation characteristic which is interpreted as the existence of the interaction between the helium loss in the partial ionization zone and pulsation intensities. It is also considered that the absence of strong pulsations is also related to the evolution status of the star. Further, its periodogram shows low-frequency peaks. If these oscillations are g-modes, V775 Tau can be thought to be one of the rare stars that show all γ Dor, δ Scuti and Am type variations. V483 Tau is comparatively more luminous, hotter and has higher rotational velocity. Therefore, although it shares the same region with V775 Tau in the H-R diagram, it is not considered to be an Am star. Yet, it exactly overlaps with the γ Dor stars. These clues as well as g-modes detected in its periodogram indicate that V483 Tau is a hybrid star. Finally, both V775 Tau and V483 Tau display period changes whose rates are between 10 −3 and 10 −4 yr −1 . Considering the δ Scuti nature, it may be speculated that these changes are non-evolutionary.

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“…In Figure 5, we show the position of the primary component of KIC 7385478 on Hertzsprung–Russel diagram, together with some eclipsing binaries with known γ Doradus type pulsating components, i.e. VZ CVn (Ibanoǧlu et al 2007), CoRot 102918586 (Maceroni et al 2013), KIC 11285625 (Debosscher et al 2013), KIC 9851142 (Çakırlı 2015), KIC 9851944 (Guo et al 2016), V2653 Oph (Çakırlı & Ibanoglu 2016), CoRot 100866999 (Chapellier & Mathias 2013). Our target is located in the middle of the γ Doradus instability strip given by Warner et al (2003), which takes us to the possibility of γ Doradus type pulsation on the primary component.…”

Section: Discussionmentioning

confidence: 99%

KIC 7385478: An Eclipsing Binary with a γ Doradus Component

Özdarcan

Dal

2017

Publ. Astron. Soc. Aust.

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We present spectroscopic and photometric analysis of the eclipsing binary KIC 7385478. We find that the system is formed by F1V + K4III-IV components. Combining results from analysis of spectroscopic data and Kepler photometry, we calculate masses and radii of the primary and the secondary components as M1 = 1.71 ± 0.08 M , M2 = 0.37 ± 0.04 M and R1 = 1.59 ± 0.03R , R2 = 1.90 ± 0.03R , respectively. Position of the primary component in HR diagram is in the region of γ Doradus type pulsators and residuals from light curve modeling exhibit additional light variation with a dominant period of ∼0.5 day. These are clear evidences of the γ Doradus type pulsations on the primary component. We also observe occasional increase in amplitude of the residuals, where the orbital period becomes the most dominant period. These may be attributed to the cool star activity originating from the secondary component.

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V2653 Ophiuchii with a pulsating component and Ppuls – Porb, Ppuls – g correlations for γ Dor type pulsators

Abstract: V2653Ophiuchii with a pulsating component and P puls -P orb , P puls -g correlations for γ-Dor type pulsators

Cited by 11 publications

References 51 publications

Catalogue and properties of δ Scuti stars in binaries

Catalogue and properties of δ Scuti stars in binaries

STEREO observations of hybrid stars V775 Tau and V483 Tau

KIC 7385478: An Eclipsing Binary with a γ Doradus Component

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