Asteroseismology of KIC 11754974: a high-amplitude SX Phe pulsator in a 343-d binary system

Murphy, Simon J.; Pigulski, A.; Kurtz, D. W.; Suárez, J. C.; Handler, G.; Balona, L. A.; Smalley, B.; Uytterhoeven, K.; Szabo, Robert M.; Thygesen, A. O.; Elkin, V. G.; Breger, M.; Grigahcène, A.; Guzik, J. A.; Nemec, J. M.; Southworth, J.

doi:10.1093/mnras/stt587

Cited by 47 publications

(40 citation statements)

References 51 publications

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“…Unlike the traditional O-C (observed minus calculated) method, PM uses all of the data -not just the pulsation maxima -and is particularly suited to multimode pulsators. The validity of FM and PM has been confirmed with known binaries ( [15], [16]). …”

Section: Introductionsupporting

confidence: 53%

Finding non-eclipsing binaries through pulsational phase modulation

Murphy

Bedding

Shibahashi

et al. 2015

EPJ Web of Conferences

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Abstract. We present a method for finding binaries among pulsating stars that were observed by the Kepler Mission. We use entire four-year light curves to accurately measure the frequencies of the strongest pulsation modes, then track the pulsation phases at those frequencies in 10-d segments. This produces a series of time-delay measurements in which binarity is apparent as a periodic modulation whose amplitude gives the projected light travel time across the orbit. Fourier analysis of this time-delay curve provides the parameters of the orbit, including the period, eccentricity, angle of ascending node and time of periastron passage. Differentiating the time-delay curve yields the full radial-velocity curve directly from the Kepler photometry, without the need for spectroscopy. We show examples with delta Scuti stars having large numbers of pulsation modes, including one system in which both components of the binary are pulsating. The method is straightforward to automate, thus radial velocity curves can be derived for hundreds of non-eclipsing binary stars from Kepler photometry alone. This contribution is based largely upon the work by Murphy et al. [1], describing the phase-modulation method in detail.

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Section: Introductionsupporting

confidence: 53%

Finding non-eclipsing binaries through pulsational phase modulation

Murphy

Bedding

Shibahashi

et al. 2015

EPJ Web of Conferences

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“…Wu 2001 andMontgomery 2005). Combination frequencies dominate the amplitude spectra of some δ Sct stars, for example KIC 11754974 (Murphy et al 2013) and KIC 8054146 (Breger et al 2012;Breger & Montgomery 2014), where the astrophysical implications and uses of the combination frequencies are more uncertain than for white dwarf stars.…”

Section: Introductionmentioning

confidence: 99%

A unifying explanation of complex frequency spectra of γ Dor, SPB and Be stars: combination frequencies and highly non-sinusoidal light curves

Kurtz¹,

Shibahashi²,

Murphy³

et al. 2015

Monthly Notices of the Royal Astronomical Society

152

199

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There are many Slowly Pulsating B (SPB) stars and γ Dor stars in the Kepler Mission data set. The light curves of these pulsating stars have been classified phenomenologically into stars with symmetric light curves and with asymmetric light curves. In the same effective temperature ranges as the γ Dor and SPB stars, there are variable stars with downward light curves that have been conjectured to be caused by spots. Among these phenomenological classes of stars, some show 'frequency groups' in their amplitude spectra that have not previously been understood. While it has been recognised that nonlinear pulsation gives rise to combination frequencies in a Fourier description of the light curves of these stars, such combination frequencies have been considered to be a only a minor constituent of the amplitude spectra. In this paper we unify the Fourier description of the light curves of these groups of stars, showing that many of them can be understood in terms of only a few base frequencies, which we attribute to g mode pulsations, and combination frequencies, where sometimes a very large number of combination frequencies dominate the amplitude spectra. The frequency groups seen in these stars are thus tremendously simplified. We show observationally that the combination frequencies can have amplitudes greater than the base frequency amplitudes, and we show theoretically how this arises. Thus for some γ Dor and SPB stars combination frequencies can have the highest observed amplitudes. Among the B stars are pulsating Be stars that show emission lines in their spectra from occasional ejection of material into a circumstellar disk. Our analysis gives strong support to the understanding of these pulsating Be stars as rapidly rotating SPB stars, explained entirely by g mode pulsations.

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“…Murphy et al 2013), (b) the continuous monitoring of the targets, that eliminates the effect of alias in frequencies detections (Breger 2000), and (c) the relatively high time resolution of the short-cadence data (∼ 1 min). It should to be noted that the long-cadence data (i.e.…”

Section: Introductionmentioning

confidence: 99%

Asteroseismology ofKeplerAlgol-type oscillating eclipsing binaries

Liakos

2017

A&A

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Context. This research paper contains light curve modelling, spectroscopy and detailed asteroseismic studies for four out of five in total semidetached eclipsing binaries with a δ Scuti component, that have been detected to date through Kepler mission, namely KIC 06669809, KIC 10581918, KIC 10619109 and KIC 11175495. Aims. The goal is to study the pulsational characteristics of the oscillating stars of the systems as well as to estimate their absolute parameters and enrich the so far poor sample of this kind of systems. Methods. Ground based spectroscopic observations provide the means to estimate the spectral types of the primary components and to model the light curves with higher certainty. The photometric data are analysed using eclipsing binary modeling techniques, while Fourier analysis is applied on their residuals in order to reveal the pulsation frequency modes. Results. The results of analyses show that the primaries are pulsating stars of δ Scuti type and that all systems belong to the group of Algol type binaries with an oscillating star, namely oEA stars. The primaries of KIC 06669809, KIC 10581918, and KIC 10619109 pulsate in three, two, and five frequencies, respectively and in more than 200 other detected as combinations. The δ Scuti star of KIC 11175495 is the youngest and the fastest pulsator in binary systems that has ever been found and it oscillates in three main nonradial frequencies, while other 153 are also found as depended ones. Moreover, a comparison of their properties with other systems of the same type as well as with theoretical models of pulsating stars are also presented and discussed.

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Asteroseismology of KIC 11754974: a high-amplitude SX Phe pulsator in a 343-d binary system

Cited by 47 publications

References 51 publications

Finding non-eclipsing binaries through pulsational phase modulation

Finding non-eclipsing binaries through pulsational phase modulation

A unifying explanation of complex frequency spectra of γ Dor, SPB and Be stars: combination frequencies and highly non-sinusoidal light curves

Asteroseismology ofKeplerAlgol-type oscillating eclipsing binaries

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