KIC 3749404: a heartbeat star with rapid apsidal advance indicative of a tertiary component

Hambleton, Kelly; Kurtz, D. W.; Prša, Andrej; Quinn, S. N.; Fuller, James; Murphy, Simon J.; Thompson, Susan E.; Latham, David W.; Shporer, Avi

doi:10.1093/mnras/stw1970

Cited by 65 publications

(45 citation statements)

References 68 publications

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“…These binary stars undergo extreme dynamic tides, causing them to become tidally distorted and more oblate in shape as they pass through periastron. The dynamic tidal distortions, along with heating and Doppler boosting, cause their distinctive pulse-like variations (Welsh et al 2011;Hambleton et al 2015Hambleton et al , 2016. Also, these stars show pulsations at frequencies that are harmonics of the orbital frequency, indicating that these pulses are likely tidally driven (Willems & Aerts 2002).…”

Section: Introductionmentioning

confidence: 94%

“…Accurate and unique models of the photometric variations, as that done for KOI-54 (Welsh et al 2011) and KIC3749404 (Hambleton et al 2016), require radial velocity measurements to constrain the possible orbital solutions. From these RV measurements, combined with photometric data, a full orbital solution can be obtained, including the stellar mass, eccentricity, and inclination of the system.…”

Section: Introductionmentioning

confidence: 99%

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The Pseudosynchronization of Binary Stars Undergoing Strong Tidal Interactions

Zimmerman

Thompson

Mullally

et al. 2017

ApJ

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Eccentric binaries known as heartbeat stars experience strong dynamical tides as the stars pass through periastron, providing a laboratory to study tidal interactions. We measure the rotation periods of 24 heartbeat systems, using the Kepler light curves to identify rotation peaks in the Fourier transform. Where possible, we compare the rotation period to the pseudosynchronization period derived by Hut. Few of our heartbeat stars are pseudosynchronized with the orbital period. For four systems, we were able to identify two sets of rotation peaks, which we interpret as the rotation from both stars in the binary. Most stars in our sample have rotation rates larger than the pseudosynchronization period while a single target rotates much faster than this rate. The majority of the systems have a rotation period that is approximately 3 2 times the pseudosynchronization period, suggesting that other physical mechanisms strongly influence the star's evolution.

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Section: Introductionmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

The Pseudosynchronization of Binary Stars Undergoing Strong Tidal Interactions

Zimmerman

Thompson

Mullally

et al. 2017

ApJ

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“…KIC 3749404: (Figure 11, Table 6) This 20-day, eccentric (e = 0.635), and fastly precessing (ω p = 1.2 • yr −1 ) binary has an intermediate inclination of i = 62 • (Hambleton et al 2016). This orientation slightly favours the m = 2 modes but m = 0 modes cannot be excluded.…”

Section: Four Published Heartbeat Stars With Teosmentioning

confidence: 99%

Tidally Excited Oscillations in Heartbeat Binary Stars: Pulsation Phases and Mode Identification

Guo

Shporer

Hambleton

et al. 2020

ApJ

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Tidal forces in eccentric binary stars known as heartbeat stars excite detectable oscillations that shed light on the processes of tidal synchronization and circularization. We examine the pulsation phases of tidally excited oscillations (TEOs) in heartbeat binary systems. The target list includes four published heartbeat binaries and four additional systems observed by Kepler. To the first order, the pulsation phases of TEOs can be explained by the geometric effect of the dominant l = 2, m = 0, or ±2 modes assuming pulsations are adiabatic. We found that this simple theoretical interpretation can account for more than half of the systems on the list, assuming their spin and orbit axes are aligned. We do find significant deviations from the adiabatic predictions for some other systems, especially for the misaligned binary KIC 8164262. The deviations can potentially help to probe the non-adiabaticity of pulsation modes as well as resonances in the tidal forcing.

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“…Also they state that in short-period (P orb < 13 days) detached systems, the tidal effects may play an important role to the pulsation frequency modulation. Although tidal potential excites g-mode pulsations (Zahn 2013;Hambleton et al 2016), there is probably an influence to the p modes and/or to the radial mode of the pulsating member of the system. In oscillating eclipsing systems of algol type stars, this dependence seems to be more complicated because the mass transfer rate may be also a determining parameter additionally to the tidal interaction influence in the pulsations likely in detached systems (Liakos and Niarchos 2017).…”

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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KIC 3749404: a heartbeat star with rapid apsidal advance indicative of a tertiary component

Cited by 65 publications

References 68 publications

The Pseudosynchronization of Binary Stars Undergoing Strong Tidal Interactions

The Pseudosynchronization of Binary Stars Undergoing Strong Tidal Interactions

Tidally Excited Oscillations in Heartbeat Binary Stars: Pulsation Phases and Mode Identification

STEREO observations of hybrid stars V775 Tau and V483 Tau

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