Signatures of nonlinear mode interactions in the pulsating hot B subdwarf star KIC 10139564
^{1} Université de Toulouse, UPSOMP, IRAP, 31400 Toulouse, France
email: weikai.zong@irap.omp.eu; stephane.charpinet@irap.omp.eu; gerard.vauclair@irap.omp.eu
^{2} CNRS, IRAP, 14 avenue Edouard Belin, 31400 Toulouse, France
Received: 16 June 2016
Accepted: 18 July 2016
Context. The unprecedented photometric quality and time coverage offered by the Kepler spacecraft has opened up new opportunities to search for signatures of nonlinear effects that affect oscillation modes in pulsating stars.
Aims. The data accumulated on the pulsating hot B subdwarf KIC 10139564 are used to explore in detail the stability of its oscillation modes, focusing in particular on evidences of nonlinear behaviors.
Methods. We analyzed 38 months of contiguous shortcadence data, concentrating on mode multiplets induced by the star rotation and on frequencies forming linear combinations that show intriguing behaviors during the course of the observations.
Results. We find clear signatures that point toward nonlinear effects predicted by resonant mode coupling mechanisms. These couplings can induce various mode behaviors for the components of multiplets and for frequencies related by linear relationships. We find that a triplet at 5760 μHz, a quintuplet at 5287 μHz and a (ℓ > 2) multiplet at 5412 μHz, all induced by rotation, show clear frequency and amplitude modulations which are typical of the socalled intermediate regime of a resonance between the components. One triplet at 316 μHz and a doublet at 394 μHz show modulated amplitude and constant frequency which can be associated with a narrow transitory regime of the resonance. Another triplet at 519 μHz appears to be in a frequencylocked regime where both frequency and amplitude are constant. Additionally, three linear combinations of frequencies near 6076 μHz also show amplitude and frequency modulations, which are likely related to a threemode direct resonance of the type ν_{0} ~ ν_{1} + ν_{2}.
Conclusions. The identified frequency and amplitude modulations are the first clearcut signatures of nonlinear resonant couplings occurring in pulsating hot B subdwarf stars. However, the observed behaviors suggest that the resonances occurring in these stars usually follow more complicated patterns than the simple predictions from current nonlinear theoretical frameworks. These results should therefore motivate further work to develop the theory of nonlinear stellar pulsations, considering that stars such as KIC 10139564 now offer remarkable testbeds to do so.
Key words: techniques: photometric / stars: variables: general / stars: individual: KIC 10139564
© ESO, 2016
1. Introduction
Hot B subdwarf (sdB) stars are helium core burning objects that populate the socalled extreme horizontal branch (EHB). They are expected to have a mass around 0.47 M_{⊙} and are characterized by a very thin hydrogenrich residual envelope containing at most ~ 0.02M_{⊙}. For this reason, they remain hot and compact throughout all their helium core burning evolution, with effective temperatures, T_{eff}, and surface gravities, log g, ranging from 22 000 K to 40 000 K and from 5.2 to 6.2, respectively (Heber 2009; Fontaine et al. 2012).
The presence of pulsations in some sdB stars make them good candidates for probing their interior with the technique of asteroseismology. A first group of nonradial sdB pulsators with periods of a few minutes was theoretically predicted by Charpinet et al. (1996) and effectively discovered by Kilkenny et al. (1997). These pulsators, now referred to as the V361 Hya stars, show loworder, lowdegree pressure (p)modes that are driven by a κmechanism induced by the partial ionization of irongroup elements occurring in the “Zbump” region and poweredup by radiative levitation (Charpinet et al. 1996, 1997). Long period oscillations of ~ 1−4 h were later discovered by Green et al. (2003), forming another group of sdB pulsators known as the V1093 Her stars. The latter show midorder gravity (g)modes driven by the same mechanism (Fontaine et al. 2003). Hybrid pulsators that show both p and gmode oscillations simultaneously have also been reported (e.g., Schuh et al. 2006). Tight seismic constraints have indeed been obtained from the measured frequencies using both types of sdB pulsators, in particular based on highquality photometric data gathered from spaceborne telescopes (e.g., Charpinet et al. 2011; van Grootel et al. 2010). However, the reason behind the apparent variability of some oscillation modes in sdB stars, already noticed from repeated ground based campaigns (e.g., Kilkenny et al. 2007), has remained poorly understood.
The temporal variation of oscillation modes in pulsating sdB stars is beyond the scope of the standard linear nonradial stellar oscillation theory in which eigenmodes have a stable frequency and amplitude (Unno et al. 1989). These behaviors must be studied within a nonlinear framework to interpret the modulations. In particular nonlinear resonant mode coupling effects are expected to affect some oscillation modes, as noted, for example, in the helium dominated atmosphere white dwarf variable (DBV) star GD 358 (Goupil et al. 1998). Different types of resonant coupling have been investigated within the framework of the amplitude equation (AE) formalism since the 1980’s (e.g., Buchler & Goupil 1984), among them the ν_{0} ~ ν_{1} + ν_{2} resonance (Dziembowski 1982; Moskalik 1985) and the 2:1 resonance in Cepheid stars (Buchler & Kovacs 1986). The AE formalism was then extended to nonadiabatic nonradial pulsations in Eulerian and Lagrangian formulations by Goupil & Buchler (1994) and van Hoolst (1994), respectively. A theoretical exploration of specific cases of nonradial resonances was developed in Buchler et al. (1995, 1997), including notably the resonance occurring in a mode triplet that is caused by slow stellar rotation and which satisfies the relationship ν_{+} + ν_{−} ~ 2ν_{0}, where ν_{0} is the frequency of the central m = 0 component. However, these theoretical developments based on AEs have since considerably slowed down, in part due to the lack of clear observational data to rely on.
The launch of instruments for ultra high precision photometry from space has changed the situation, making it now possible to capture amplitude and/or frequency modulations occurring on timescales of months or even years that were difficult to identify from groundbased observatories. It is however from ground based data that Vauclair et al. (2011) proposed for the first time that resonant couplings within triplets could explain the longterm variations, both in amplitude and frequency, seen in several oscillation modes monitored in the GW Virginis pulsator PG 0122+200, through successive campaigns.
The observation of a multitude of pulsating stars, including sdB and white dwarf stars, by the Kepler spacecraft has open up new opportunities to identify and characterize the mechanisms that could modulate the oscillation modes. Kepler monitored a 105 deg^{2} field in the CygnusLyrae region for around four years without interruption, thus obtaining unprecedented high quality photometric data for asteroseismology (Gilliland et al. 2010). These uninterrupted data are particularly suited for searching longterm temporal amplitude and frequency modulations. In the context of white dwarf pulsators, for instance, Zong et al. (2016, hereafter Z16) found that the DBV star KIC 08626021 shows clear signatures of nonlinear effects attributed to resonant mode couplings. In this star, three rotational multiplets show various types of behaviors that can be related to different regimes of the nonlinear resonant mode coupling mechanism. In particular some amplitude and frequency modulation timescales are found to be consistent with theoretical expectations. This finding suggests that the variations of some oscillation modes in sdB stars may also be related to nonlinear resonance effects. It is in this context that we decided to search clues of similar nonlinear phenomena involving mode interactions in pulsating sdB stars.
Eighteen sdB pulsators have been monitored with Kepler (see Østensen et al. 2014 and references therein). In this paper, we focus on one of them, the star KIC 10139564, which was discovered in quarter Q2.1 and then continuously observed from Q5.1 to Q17.2. A preliminary analysis based on one month of short cadence data originally showed that KIC 10139564 is a V361Hya type (rapid, pmode) sdB pulsator featuring also a lowamplitude gmode oscillation (Kawaler et al. 2010). With extended data, Baran et al. (2012) detected up to 57 periodicities including several multiplets attributed to the rotation of the star. These multiplets are characterized by common frequency spacings, both for the p and gmodes, indicating that KIC 10139564 has a rotation period of 25.6 ± 1.8 d. These authors did not find any radialvelocity variations from their dedicated spectroscopy and derived the atmospheric parameter values T_{eff} = 31 859 K and log g = 5.673 for this star. An interesting finding concerning KIC 10139564 is that two of the identified multiplets may have degrees ℓ greater than two, a possibility further investigated by Baran & Østensen (2013). The detection of several multiplets in this star continuously monitored for more than three years makes it a target of choice for studying eventual nonlinear resonant mode couplings in sdB stars.
In this study, we show that several multiplets in KIC 10139564 have indeed amplitude and frequency modulations suggesting nonlinear resonant mode couplings, which constitutes the first clearcut case reported for sdB pulsators, so far. In Sect. 2, we present the thorough analysis of the frequency content of the Kepler photometry available on KIC 10139564, including our analysis of the frequency and amplitude modulations identified in several multiplets and linear combination frequencies. In Sect. 3, we recall some theoretical background related to nonlinear resonant mode couplings, focusing mainly on two types of resonances. The interpretation of the observed modulations which may relate to nonlinear resonant mode couplings is discussed in Sect. 4. The summary and conclusion are then given in Sect. 5.
2. The frequency content of KIC 10139564 revisited
2.1. The Kepler photometry
The pulsating sdB star KIC 10139564 was observed by Kepler in shortcadence (hereafter SC) mode during quarter Q2.1 and from Q5.1 to Q17.2 (i.e., until the spacecraft finally lost its second inertia reaction wheel and stopped its operations). Results based on parts of these data have already been published in the literature (e.g., Baran et al. 2012; Baran & Østensen 2013). we obtained the light curves through the Kepler Asteroseismic Science Consortium (KASC)^{1}. These data were processed through the standard Kepler Science Processing Pipeline (Jenkins et al. 2010). For our purposes, we do not further consider the “short” (one month) light curve of Q2.1 which is well disconnected from the main campaign and would introduce a large and detrimental gap for our upcoming analysis. This leaves us with a nearly contiguous 38month light curve starting from BJD 2 455 276.5 and ending on BJD 2 456 424 (which spans ~1147.5 days), with a duty circle of ~ 89%.
Fig. 1 Top panel: condensed representation of the full Kepler light curve of KIC 10139564 (Amplitude as the residual relative to the mean brightness intensity of the star vs time in Barycentric Julian Date) covering from Q5.1 to Q17.2 (~ 1147.5 days). Bottom panel: closeup view showing 0.8 days of the Kepler light curve by slices of 0.08 days. At this scale the oscillations are clearly apparent. 

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The full light curve was constructed from each quarter “corrected” light curves, which most notably include a correction of the amplitudes taking into account contamination by nearby objects (this correction estimates that ~ 83.2% of the light comes from KIC 10139564). Each quarter light curve was individually detrended to correct for residual drifts by performing a sixthorder polynomial fit. Then, data points that differ significantly from the local standard deviation of the light curve were removed by applying a running 3σ clipping filter. Note that the latter operation decreases slightly the overall noise level in Fourier space, but has no incidence on the measured frequencies.
The fully assembled light curve of KIC 10139564 is shown in the top panel of Fig. 1 while the bottom panel expands a 0.8day portion of the data. Lowamplitude multiperiodic oscillations dominated by periodicities of a few minutes are clearly visible. Their presence is confirmed in the corresponding LombScargle periodogram (LSP, Fig. 2; Scargle 1982). The LSP shows two distinct regions with significant signal corresponding to pmodes at high frequencies and gmodes at low frequencies. This identifies KIC 10139564 as a hybrid pulsating sdB star (Schuh et al. 2006) whose oscillations are however largely dominated by pmodes. The formal frequency resolution achieved with these data is ~ 0.010μHz.
2.2. Frequency extraction
A dedicated software, Felix (Frequency Extraction for LIghtcurve eXploitation) developed by one of us (S.C.), was used to first extract the frequency content of KIC 10139564 down to a chosen detection threshold. The latter was established following the same method as in Z16 (see their Sect. 2.2), leading also in the present case to a conservative 5.6σ criterion (in practice, we searched down to ~ 5σ if a frequency is suspected to be part of a multiplet; see below).
Fig. 2 LombScargle periodogram (LSP; amplitude in % of the mean brightness vs frequency in μHz) of the Kepler light curve for KIC 10139564. The represented range, up to the Nyquist frequency, covers the longperiod gmode and the shortperiod pmode frequency domains. The region between the two dashed vertical lines at 5200 and 6400 μHz is where peaks have the largest amplitudes. However, weaker peaks outside of this particular region are present and are made visible by scaling up amplitudes by a factor of 20. The dashed horizontal line represents the 5.6σ detection threshold (see text). Some wellknown Kepler instrumental artefacts are present, but can easily be recognized. 

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The extraction method is a standard prewhithening and nonlinear least square fitting technique (Deeming 1975), which works with no difficulty in the present case. The code Felix greatly accelerates and eases the application of this procedure, especially for treating very long timeseries obtained from space such as CoRoT and Kepler (Charpinet et al. 2010, 2011).
List of frequencies detected in KIC 10139564 on which we focus our analysis.
We provide in Table A.1 (see Appendix) a list of all the extracted frequencies with their fitted attributes (frequency in μHz, period in second, amplitude in percent of the mean brightness, phase relative to a reference time t_{0}, and signaltonoise ratio) and their respective error estimates (σ_{f}, σ_{P}, σ_{A}, and σ_{Ph}). For convenience, because in this study we focus on a particular subset of the observed frequencies, we repeat some of these information in Table 1 for the relevant modes. The “Id.” column in both tables uniquely identify a detected frequency with the number indicating the rank by order of decreasing amplitude.
We have detected 60 clear independent frequencies that comes out well above the 5.6σ detection threshold (Table A.1), of which 29 frequencies consist of three triplets, one doublet, one quintuplet and two incomplete multiplets with ℓ> 2 (Table 1). We also detect another three frequencies that appear as significant but are linked to other frequencies through linear combinations. Five additional “forests” of frequencies, each containing many close peaks in a very narrow frequency range, are detected in the 5400−6400 μHz region. We also prewhitened 14 frequencies whose amplitudes are above 5.0σ but below 5.6σ which, we suspect, are real pulsations. Our wellsecured extracted frequencies agree well with the independent analysis of Baran & Østensen (2013), but we detect a few more lowamplitude frequencies because the data that we consider here cover about one more year. We do not investigate further these “forests” of frequencies (G1–G5, see Table A.1) that show very complicated structures. These were discussed in Baran et al. (2012). We point out that our extracted frequencies may differ in amplitude compared with the work of Baran & Østensen (2013) because some of these frequencies have variable amplitudes.
Fig. 3 Left panel: 2D distribution of the frequency and amplitude deviations between the prewhitened and the injected values for 1000 artificial modes of constant amplitude. S/N denotes the signaltonoise ratio of the injected signals and the deviations have been normalized by the 1σ error, σ_{A} and σ_{f}, derived from the prewhitening procedure implemented in the code Felix. The 2D distribution is also projected into 1D histograms (frequency and amplitude) to be compared with the Normal Distribution, plotted as a red solid curve. Right panel: same as above but for 1000 modes with random amplitudes. The injected modes are divided into three groups of S/N in the ranges [5,15], (15,25], and (25,60], respectively (represented by three different colors and symbols). 

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2.3. Error estimates on frequencies and amplitudes
Before proceeding further in our analysis, we briefly discuss our quantitative evaluation of the uncertainties associated with the measured frequencies and amplitudes given in Tables 1 and A.1. The reliability of these error estimates is particularly important when it comes to discuss amplitude and frequency variations with time, in particular to assess if these are significant or not.
With Felix, errors are estimated following the formalism proposed by Montgomery & Odonoghue (1999), with the particularity, however, that σ_{A}, the error on the amplitude of a mode, is measured directly in the LombScargle periodogram. A window around each frequency is chosen and the median value of the amplitudes in that frequency range defines σ_{A}. The relations given in Montgomery & Odonoghue (1999) are then used to compute the other errors, in particular σ_{f}, the error on the measured frequency. In order to test that this procedure is correct and does not largely under or overestimate the true errors, we conduct two Monte Carlo experiments.
We first construct an artificial light curve covering about 200 days (similar to the time baseline of each light curve pieces considered in the next subsection) with the same SCmode sampling provided by Kepler in which we add white random gaussian noise. We further inject in this light curve 1000 sinusoidal signals with the same amplitude (S/N ~ 160) but of frequency increasing by steps of ~ 8.2 μHz per signal. In practice, a random frequency shift of a few tenth μHz is performed on each injected frequency in order to reduce the number of harmonics and linear combinations. The generated time series is then analyzed with our code Felix that extracts and measures each signal and evaluates the uncertainties associated to the measured frequencies and amplitudes (σ_{A} and σ_{f}). Since the true values of these quantities are perfectly known from the signals we injected, the real distribution of the deviations between measured (prewhitenned) values and true values can be evaluated. For that purpose, we define the frequency and amplitude deviations normalized by their 1σ errors (as estimated with the code Felix from the procedure described above), Δf = (f_{pre}−f_{inj}) /σ_{f} and ΔA = (A_{pre}−A_{inj}) /σ_{A}, where the subscripts indicate the prewhitened value and the injected one, respectively. A variant of this test is also performed by again injecting 1000 sinusoidal signals, but this time with random amplitudes (instead of constant ones) chosen in the S/N ∈ (5,60) range. This second test allows us to check also the reliability of our error estimates as a function of amplitude, considering that σ_{f} in particular depends on the mode S/N (σ_{f} increases when S/N decreases).
Figure 3 shows the results obtained in both cases. The 2D distributions of the frequency and amplitude deviations are well confined within 3σ. Moreover, the associated 1D histograms show that for both quantities, the measured deviations closely follow the Normal Distribution, , plotted as a red solid curve. Only a few data points fall outside the [− 3σ, + 3σ] range (within which 99.73% of the measurements should be for the normal distribution, ). This is the behavior we expect for an accurate determination of the error estimates, σ_{A} and σ_{f}, with the code Felix. Hence, these tests demonstrate that error values derived in our frequency analysis are robust.
2.4. Amplitude and frequency modulations
From now on, we concentrate our discussion on the six multiplets, which include three triplets T_{1}, T_{2} and T_{3}, one doublet D_{1}, one quintuplet Q_{1} and a likely ℓ = 4 multiplet M_{1} (see again Table A.1). Interestingly, three of these multiplets (T_{2}, D_{1}, and T_{3}) involve gmodes, while the others (Q_{1}, M_{1}, and T_{1}) are pmodes. We also examine three linear combination frequencies (C_{1}). The fine structures of the multiplets are shown in the left top panels of Figs. 4, 6, 7 and 9−11. The average frequency spacing between the components of these welldefined, nearly symmetric multiplets is ~ 0.25 μHz for the gmodes and 0.423 μHz for the pmodes, thus suggesting that the gmodes are dipoles (ℓ = 1) in a star rotating rigidly with a period of ~ 26 days.
In order to investigate the time variability of these oscillation modes and their relationships, we used our software Felix to compute sliding LombScargle periodograms (sLSP) of the data set. This method constructs timefrequency diagrams by filtering in only parts of the data set as a function of time. We chose a filter window of 200day width moved along the entire light curve by time steps of 20 days. This ensures a good compromise, for our purposes, between the frequency resolution (to resolve close structures of peaks in each LSP), time resolution, and signaltonoise. The sLSP offers an overall view of the amplitude and frequency variations that may occur for a given mode (see, e.g., the middle left panel of Fig. 4). As a complementary (and more precise) technique, we also extracted the frequencies (through prewhitening and nonlinear least square fitting) in various parts of the light curve. The 38month light curve of KIC 10139564 was divided into 32 time intervals, each containing nine months of Kepler data (for the purposes of precision in the measurements) except for the last three intervals at the end of the observations. This second approach provides a measure of the (averaged) frequencies and amplitudes at a given time, along with the associated errors (see, e.g., the right and bottom left panels of Fig. 4).
Fig. 4 Frequency and amplitude modulations in the T_{1}pmode triplet near 5760 μHz. Topleft panel presents the fine structures of the well defined triplet with near symmetric frequency spacings. The dashed horizontal line in red represents the 5.6 σ detection threshold. Middleleft panel shows the sliding LombScargle periodogram (sLSP giving the amplitude in % as a function of frequency in μHz and time in days) of the triplet as a whole. Bottomleft panel shows expanded views around the average frequency (the solid vertical lines, also in the middle left panel) of each component, obtained from prewhitening subsets of the data, thus measuring precisely the frequencies, as a function of time. Right panel provides the measured amplitudes as a function of time obtained for each subset of data (see text for details). Note that the errors for each measurement is smaller than the symbol itself. 

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Figure 4 shows the amplitude and frequency modulations for the three components forming the triplet T_{1} near 5760 μHz. As mentioned already, the topleft panel shows the triplet as revealed by the full data set with components nearly equally spaced in frequency. We note, however, that this spacing is not strictly symmetric, with a difference (or “frequency mismatch”) of 0.0026 μHz. Frequency variations with time are illustrated by the sLSP diagram in the middleleft panel where the color scale represents the amplitude of the modes. An expanded view centered on the average frequency of each component is then provided in the bottomleft panel while the amplitude behavior with time for each component is shown in the right panel. The latter two are obtained from prewhitening parts of the light curve as described above.
From the sLSP diagram, we find that both the amplitudes and frequencies have varied during the Kepler observations. These variations are more clearly seen in the bottomleft and right panels. The side components both show suggestions of a quasiperiodic modulation in frequency and evolve in antiphase. We also note a long timescale trend as the frequencies of the two side components gradually approach toward each other, as well as toward the central component. In order to filter out these trends, we applied a parabolic fit to each component, leaving the remaining signature of the quasiperiodic modulation of the frequencies (see Fig. 5). In the process, we find that the two side components had frequencies about 0.06 μHz closer to each other at the end of the run compared to the beginning of the observations. Figure 5 shows that the data almost cover two cycles of the quasiperiodic frequency variations. While clearly not strictly sinusoidal, although not very far from it, if we fit the closest pure sine wave to each curve, we find that all have a very similar (quasi)period of ~ 570 days. The variations for the side components (retrograde and prograde modes) are clearly in antiphase. For the amplitude variations, we also find suggestions of a quasiperiodic modulation for the central and prograde components. The retrograde mode for its part has a more regular amplitude evolution (increase) during the course of the observations.
Fig. 5 Frequency modulations after removing the longterm trend in the T_{1} triplet by applying a secondorder polynomial fit. The solid curves represent the best fits of one pure sine wave to the frequency modulations. The associated formal errors for the periods and phases are also estimated. 

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Figure 6 illustrates the amplitude and frequency modulations for the gmode triplet T_{2} near 316 μHz using the same presentation as in Fig. 4. In this case, the triplet shows a very small (but significant) asymmetry of 0.0036 μHz. The frequencies appear to be stable over the 38month Kepler observations. The amplitude is essentially constant for the retrograde (m = −1) mode while the other two components display some variations. The central one may show a small oscillatory behavior, but more precise measurements would be needed to really confirm that trend. The prograde (m = 1) mode has its amplitude rising continuously throughout the observations, from 400 ppm up to about 600 ppm.
Fig. 6 Same as Fig. 4 but for the T_{2}gmode triplet near 316 μHz. 

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The amplitude and frequency variations of the gmode triplet T_{3} near 519 μHz are shown in Fig. 7. In this triplet, which is almost perfectly symmetric, the three components have stable frequencies and amplitudes within the quoted uncertainties. This stability is further illustrated with Fig. 8 that shows the scattering of the measured frequencies and amplitudes for these modes from all the data chunks considered throughout the entire light curve. Almost all measurements are indeed confined within 2σ around their average values (and all are within 3σ). It is interesting to note that the triplet T_{3} therefore has different characteristics compared to the two triplets T_{1} and T_{2}.
Figure 9 shows the amplitude and frequency modulations for the gmode doublet D_{1} near 394 μHz. The frequencies of each component forming the doublet appear to be stable over the 38month Kepler observations, while the amplitudes show very suggestive indications of quasiperiodic variations. We find that the amplitude modulations of the two components have very similar periods, about 1100 days, as illustrated by the bestfit sine waves to the data (the red solid curves in right panel of Fig. 9). Hence the available Kepler data just cover about one cycle of this variation, but it is remarkable that almost all the amplitude measurements match very closely the fitted sine curves. This estimated period is almost twice the period of modulations occurring in the main triplet T_{1}. Moreover, we clearly see that the amplitudes of the two components evolve almost in antiphase during the observing run.
Fig. 7 Same as Fig. 4 but for the T_{3}gmode triplet near 519 μHz. 

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Fig. 8 Frequency and amplitude scattering for the three components forming the gmode triplet T_{3} around their averaged values. The red and blue dashed rectangles indicate the 2σ and 3σ error boxes, respectively. All the data points are within 3σ. 

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Fig. 9 Same as Fig. 4 but for the D_{1}gmode doublet near 394 μHz. The solid curves in right panel show the best fit of a pure sine wave to the amplitude modulations. 

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Figure 10 shows the amplitude and frequency modulations for the pmode quintuplet Q_{1} near 5287 μHz. In this complete quintuplet, the m = ± 2 modes and possibly the m = 0 central component show significant frequency variations. The other modes, with m = ± 1, have frequencies which are rather stable (with only marginal fluctuations) over the entire observation run. In contrast, the amplitudes for all the modes in the quintuplet vary with patterns that cannot clearly be connected to periodic modulations, based on the available data. Of course, quasi periodic modulations with a timescale longer than twice the present Kepler observation cannot be ruled out. We also note that the frequency variations of the m = −2 and m = + 2 components and the amplitude modulations of the m = −2 and m = −1 components are roughly in antiphase during the observation.
Fig. 10 Same as Fig. 4 but for the Q_{1}pmode quintuplet near 5287 μHz. 

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Figure 11 shows the amplitude and frequency modulations for the ℓ> 2pmode multiplet M_{1} near 5413 μHz. The ℓvalue for this group of modes is not clearly assessed yet, but a plausible interpretation is that it corresponds to an ℓ = 4 nonuplet (Baran et al. 2012) with three undetected components and one component barely visible in the LSP of the full data set (see topleft panel of Fig. 11) but which is too low in amplitude to be studied in subsets of the light curve. Some of the frequencies and amplitudes of the five clearly visible modes in this multiplet show significant variations during the 38 months of Kepler observation. In particular, the frequencies of the side components drifted toward each other by ~ 0.032 μHz from the beginning to the end of the run. This trend may be comparable to that observed in the side components of the T_{1} triplet (see Fig. 4). Moreover, the same phenomenon also occurs for some modes observed in the longperioddominated sdB pulsator KIC 2697388 (M.D. Reed, priv. comm.).
In addition to the six multiplets discussed above, we identified other possible multiplets in the data, such as six modes near 5571 μHz (see Table A.1), in which however most of the components have amplitudes too low to be well studied in a timefrequency analysis or by prewhitening shorter parts of the light curve. We therefore do not consider them further in this work.
Beyond the multiplets generated by the rotation of the star, we also focus on the interesting narrow frequency region near 6076 μHz where three structures (f_{23}, f_{35} and f_{74}) show amplitude and frequency modulations as illustrated in Fig. 12. These frequencies are in fact related to components of the T_{1} and T_{2} triplets through linear combinations. We find that f_{23} ~ f_{1} + f_{11}, f_{35} ~ f_{3} + f_{21}, and f_{74} ~ f_{3} + f_{11}. Interestingly, we note that the frequency and amplitude variation pattern of f_{23} is similar to the variations observed for the mode f_{1}. Similarities also exist between the variations observed in f_{35} and f_{2}. The peak f_{74}, for its part, shows a rather large frequency variation covering up to ~ 0.1 μHz (the scales of these frequency variations are indicated by the green shadowed region in the top panel of Fig. 12).
After this description of the various behaviors encountered, we concentrate, in the following sections, on plausible theoretical interpretations for the observed amplitude and frequency modulations.
Fig. 11 Same as Fig. 4 but for the ℓ> 2pmode multiplet M_{1} near 5413 μHz. Note that at least three components are missing in this multiplet and the red vertical dashed lines indicate the expected position for two of them. 

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Fig. 12 Frequency and amplitude modulations of a group of linear combination frequencies C_{1} near 6076 μHz. The red dashed line indicates the 5.6σ detection threshold. The green shadowed areas in top panel represent the scales of variation of these frequencies (see text for details). 

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3. Resonant mode coupling and amplitude equations
In this section, we recall the most natural theoretical background to understand the behavior of the modes forming the six multiplets induced by stellar rotation. These are indeed prone to develop nonlinear interactions through resonant mode couplings, which is the mechanism that we ultimately support from our present analysis. But before moving forward in discussing details on the nonlinear resonant coupling mechanism, we first rule out several other possibilities as the cause of the observed modulations, such as instrumental effects, binarity, stochastically driven pulsations, or stellar “weather”.
Instrumental modulations can possibly occur, for example, on a per quarter basis, such as a slightly varying contamination from nearby stars that could affect the amplitude of the modes. Such effects would however affect all frequencies similarly, which is not what is observed with KIC 10139564 where the modes show different types of behavior. Another effect related to the instrument that could induce frequency and amplitude modulations is the slight shift of the Nyquist frequency associated with the movement of the Kepler spacecraft in the Solar System barycentric reference frame. Fortunately, the multiplets that we consider (with frequencies below 5761 μHz), are far away from the Nyquist frequency limit (~ 8496 μHz). Moreover, such wellstructured nearly equally spaced multiplets can obviously not be the mirror reflected frequencies of signals occurring above the Nyquist limit (Baran et al. 2012).
The presence of orbiting companions around compact stars could also induce frequency variations. However, these should occur in all frequencies and be correlated in phase, such as in the sdB pulsator V391 Peg (Silvotti et al. 2007). The variations that we find in several frequencies of KIC 10139564 are clearly not correlated in phase. In addition, radial velocity measurements from spectroscopy do not show any significant variation, thus ruling out the presence of a stellar companion (Baran et al. 2012, but for substellar objects, a higher precision would be needed to exclude this possibility).
Stochastically driven pulsations by envelope convection have long been observed in the Sun and solarlike stars. It has been claimed in the past that stochastic oscillations could also occur in some sdB pulsators, based on the observation that mode amplitudes could vary from season to season (Kilkenny et al. 2010; Reed et al. 2007). Østensen et al. (2014) recently announced that stochastic pulsations were found in the sdB star KIC 2991276, in which the amplitude and phase of the modes vary substantially and irregularly on a timescale of a month. However, the mechanism responsible for the oscillations in sdB stars, a well identified κeffect involving irongroup elements (Charpinet et al. 1997; Fontaine et al. 2003), is very different in nature from the stochastic driving occurring in the convective envelope of solarlike stars. Such a mechanism would indeed hardly be efficient in sdB stars that have radiative envelopes, except may be for a very narrow convective layer generated by the accumulation of iron in the Zbump region (the latter being however extremely weak). Beyond these theoretical considerations, we find in the case of KIC 10139564 that several mode behaviors, for example, the frequencies in the triplet T_{1} and the amplitudes in the doublet D_{1}, show correlations that would be difficult to account for with a stochastic driving mechanism and that essentially rule out this interpretation.
Changes in the background physical state of the star such as possibly induced by magnetic cycles could also be invoked for explaining amplitude and frequency modulations. Magnetic cycles indeed have an impact on the frequencies of pmodes observed in the Sun and lead to small frequency drifts that correlate in time with tracers of the solar surface activity (see, e.g., Salabert et al. 2015, and references therein). However, there is no clear observational evidence of stellar activity on the surface of sdB stars which, again, have very stable radiative envelopes and are not known to be magnetic. Cycles comparable to those observed in solarlike stars are therefore unlikely to be found in sdB stars. Moreover, such a mechanism, or more generally a phenomenon modifying the physical state of the star on a timescale of months could hardly account for the observed modulations in KIC 10139564 that show very different modulation behaviors from mode to mode, while a global change in the star would affect all modes similarly. Consequently, we also rule out this possibility in the present case.
3.1. Triplet resonance induced by slow stellar rotation
We hereafter propose that nonlinear resonant coupling mechanisms could be a natural explanation for the observed modulations in KIC 10139564. Resonant interactions between modes may indeed result in amplitude and frequency variations occurring on timescales of weeks, months, and even years.
In the present context, we limit ourselves to the type of resonances described in Buchler et al. (1995, 1997) involving linear frequency combinations ν_{1} + ν_{2} ~ 2 ν_{0}. More specifically, we focus on a particular case where dipole (ℓ = 1) modes are split by slow rotation and form a nearly symmetric triplet (thus following the above relationship between the frequencies of the components). We also consider the threemode couplings of the form ν_{1} + ν_{2} ~ ν_{0}, which corresponds to the socalled direct resonances or parametric instabilities (Dziembowski 1982; Wu & Goldreich 2001).
We first recall some basic theoretical background relative to resonances in mode triplets created by stellar rotation. We emphasize that our focus on this particular mechanism is obviously motivated by the specific configuration of the modes observed in KIC 10139564, most of which are identified as ℓ = 1 rotationally split triplets. We also point out that this type of nonlinear resonance has recently been strongly suggested to explain the modulations of the gmodes triplets in the DB white dwarf KIC 08626021 (Z16). It is therefore the most natural effect that one could think of in the present case. The AEs formalism could also, in principle, be extended to multiplets of degree ℓ> 1 at the expense of solving a larger set of coupled amplitude equations (Buchler et al. 1995). However, such development has yet to be done, which is beyond the scope of our present paper. The latter would be needed for KIC 10139564 in order to fully interpret the several multiplets with ℓ> 1 that show variations. The behavior for more complex ℓ> 1 multiplets may indeed differ from the simpler (better documented) ℓ = 1 triplet case, although we expect some similarities in general.
Details on the theory of nonlinear resonant couplings for threemode interactions, such as in ℓ = 1 triplet, can be found in (Buchler et al. 1995, 1997, Z16). We summarize below the most relevant aspects (for our purposes) of the theory. In particular, The quantity δν (which we thereafter call the frequency asymmetry), measuring the departure from exact resonance (that would occur if, e.g., triplets were perfectly symmetric), is in fact essential for driving the various resonant mode coupling behaviors. Contributions to the frequency asymmetry in a given triplet generally involves higher order effects of stellar rotation on the pulsation frequencies (Dziembowski & Goode 1992; Jones et al. 1989), but could also have additional origins, such as the presence of a weak magnetic field^{2}. We do not however consider further that possibility since no evidence of significant magnetism exists for sdB stars (Petit et al. 2012; Landstreet et al. 2012).
The rotationally split frequencies up to the second order, which should be the main contribution to the frequency asymmetry, are given by the formula (1)where the C_{kℓ} coefficient is the wellknown first order Ledoux constant, D_{kℓ} involves a complex integration of the eigenfunctions of the modes, and Ω = 1 /P_{rot} is the rotation frequency of the star (expressed in Hertz). The value of C_{kℓ} is typically ~ 0.5 for dipole gmodes when approaching the asymptotic regime, while it is usually very small (C_{kℓ} ≪ 1) for pmodes. The second order coefficient D_{kℓ} is roughly 4C_{kℓ} for dipole gmodes (Dziembowski & Goode 1992; Goupil et al. 1998) but can vary significantly from one pmode to another (Dziembowski & Goode 1992; Saio 1981). The rotation period of KIC 10139564, P_{rot}, can be estimated from the average of the frequency separations between the components of the multiplets using the first order approximation Δν = (1−C_{kℓ})Ω. We find P_{rot} ~ 26 days for KIC 10139564 (see Sect. 2). An “observed” frequency asymmetry can also be evaluated directly from the measured frequency of each triplet component, simply from the relation (2)We note at this stage that δν_{o} may actually differ from asymmetries expected from linear developments (such as discussed above) because nonlinear effects can modify the frequencies of the modes.
The numerical solutions of the AEs for mode interactions in triplets mainly reveal three distinct regimes of resonances (see, e.g., Buchler et al. 1997, and in Z16). The first state is the “frequency lock” regime where all the components in the triplet have constant frequencies and amplitudes and the asymmetry tend to be zero (triplets become perfectly symmetric). The opposite configuration is the nonresonant regime where the triplet configuration is likely predicted by the linear theory of stellar oscillations. Between the two, there is an intermediate regime in which all the modes in the triplet show modulated frequencies and amplitudes which can be periodic, irregular, or even chaotic.
In order of magnitude, the occurrence of these three regimes is roughly linked to a parameter D defined as (see Goupil et al. 1998) (3)where κ_{0} is the linear growth rate of the m = 0 mode in the triplet (a nonadiabatic quantity). However, the ranges of values for this parameter which define the different regimes depend somewhat on the values of the nonlinear coefficients in the real star. D is also a quantitative indicator that measures how far the triplet modes are away from the exact resonance center (D = 0). We nonetheless summarize some of the properties encountered in previous studies as a function of D:

In the frequencylocked regime(δν → 0), the Dparameter roughly corresponds to values in the range ~ 0−1 according to the AEs formalism. However, in the case of the white dwarf star GD 358, Goupil et al. (1998) found that D could be up to 20 and still correspond to a frequencylocked situation. These ranges, therefore, are somewhat dependent on the specific properties of the mode being considered, in particular on the scale of their linear growth rate, κ_{0}.

The intermediate regime occurs when the triplet components move away from the resonance center (δν ≠ 0). In this situation, if periodic variations indeed affect the considered modes, these can be expected to have a modulation timescale of (4)that is, roughly the timescale derived from the inverse of the linear (i.e., unperturbed) frequency asymmetry of the triplet dominated by the second order effect of stellar rotation (following Eq. (2)). This timescale is also connected to the inverse of the growth rate of the oscillation mode through the D parameter (Goupil et al. 1998).

The modes recover a configuration of steady pulsations with the nonresonant regime when the involved frequencies are such that the modes are now far from the resonance condition (D ≫ 1). In this regime, the nonlinear interaction between modes is very weak and nonlinear frequency shifts become very small. Consequently, the mode frequencies are close to the linear ones.
We finally point out that in addition to the above mentioned three main regimes, a narrow hysteresis (transitory) regime exists between the frequencylocked and intermediate regimes in which the frequencies can be locked (i.e., constant), while the amplitudes still have a modulated behavior (Buchler et al. 1997).
3.2. Three mode resonance of the type ν_{0} ~ ν_{1} + ν_{2}
In this section, we recall some properties of nonlinear interactions between oscillations modes not within triplets but whose frequencies are close to a resonance condition such that ν_{0} ~ ν_{1} + ν_{2}. Frequencies with such a relationship could also result from simple linear combination frequencies, that is, exact sum or difference of frequencies (where the “child” frequency is not a true eigenmode), which may be related to nonlinearities in the mixing process affecting the depth of a convective zone in the outer layer of a pulsating star (Wu 2001), or to nonlinearities in the flux response induced by the surface geometrical and temperature distortions triggered by the propagating waves (Brassard et al. 1995).
A useful quantity, R, connecting the observed amplitude of the combination frequency and the amplitudes of its “parent” modes, has been defined as (van Kerkwijk et al. 2000; Wu 2001) (5)where the A_{0}, A_{1}, and A_{2} are the amplitudes of the frequencies ν_{0}, ν_{1}, and ν_{2}, respectively. This ratio R is typically less than ten for simple linear combinations related, such as, to nonlinearities in the flux response. Consequently, in pulsating sdB stars, the “child” frequency resulting from this effect usually has a very low amplitude compared to its “parent” frequencies. In the large amplitude and brightest known pulsating sdB star, Balloon 090100001, where such linear combination frequencies have been unambiguously observed, the amplitude ratios are 3.9, 3.7, 3.0 and 5.5 for the linear combination frequencies of four pmodes and one gmode f_{1} + f_{2}, f_{1} + f_{3}, f_{1} + f_{4} and f_{1}−f_{B} in Bband photometry (Baran et al. 2008), respectively. In the present work, we however find that the identified linear combination frequencies C_{1} have amplitude ratios in the 10−100 range, that is, one order of magnitude larger than typical linear combination frequencies observed so far. One possible interpretation for the high amplitude ratios is that the frequency sum/difference is near the resonance condition of ν_{0} ~ ν_{1} + ν_{2} and its amplitude is boosted significantly by the resonance (e.g., Dziembowski 1982; Breger & Montgomery 2014).
The AEs formalism treating the ν_{0} ~ ν_{1} + ν_{2} type of resonance, including the parametric instability and the direct resonance (see below), is similar to the case of a triplet resonance (e.g., see the amplitude equations in Buchler et al. 1997, Z16). According to Dziembowski (1982), the threemode interactions can be described by the following coupled system Where is the complex conjugate of the amplitude A_{j} (A_{j} = A_{j}e^{iφj}), I_{j} is the mode inertia, and κ_{j} is the linear growth rate for the three involved frequencies. The quantity q is a nonlinear coupling coefficient, and δν is the frequency mismatch relative to pure resonance defined by the relationship δν = ν_{0}−ν_{1}−ν_{2}.
The nonlinear Eqs. (6a), (6b) and (6c) cannot be solved by analytical methods, but solutions for the equilibrium state (all time derivatives set to zero) can be obtained. In particular, the equilibrium solution leads to an amplitude ratio (7)The stability of the equilibriumstate depends on the growth (damping) rates and the frequency mismatch (e.g., Dziembowski 1982).
In a threemode direct resonance, the child mode is damped and has a frequency very close to the sum of frequencies of its two parent modes which are linearly driven (unstable). The child mode amplitude is very sensitive to its mode inertia, linear growth rate, and to the nonlinear coupling coefficient (see Eq. (7)). This near resonance mode can grow up to a very large amplitude if the quantity q/κ_{0}I_{0} is sufficiently large. The coupling coefficient q follows from a complex integration of the coupled mode eigenvectors and its explicit form can be found in Dziembowski (1982). It may be possible, in principle, to calculate this coefficient provided that the mode eigenfunctions are known. However, this would require that a precise seismic solution is found for KIC 10139564, which still has to be obtained. To test the theory of a threemode direct resonance, we would also need to know the linear damping (growth) rate and the inertia of the damped mode, eventually corrected by the effect of slow stellar rotation (e.g, see Carroll & Hansen 1982). However, the situation could be simplified in the case of unstable equilibrium state where the amplitude and frequency of the child mode should exactly follow those of its parent modes, even if the growth rates and coupling coefficients are unknown. Fortunately, the equilibrium state of threemode direct resonances seems always unstable because the growth (damping) rates cannot satisfy the stability criteria of the Hurwitz theorem (Dziembowski 1982). Therefore, each frequency and amplitude measurement could be used as one independent test of these particular nonlinear couplings. Furthermore, this also provides a method to separate the child mode from their parent modes according to the amplitude and frequency relationships (e.g., Breger & Montgomery 2014).
The parametric instability is another form of threemode resonant coupling that could destabilize a pair of stable daughter modes from an overstable (driven) parent mode (Wu & Goldreich 2001). In this mechanism, the overstable parent mode gains energy through the driving engine (a κmechanism in our case) and the two independent damped child modes dissipate energy. This configuration would lead the system to reach limit cycles under certain conditions (e.g., if δν<κ_{1} or κ_{2}, Wu & Goldreich 2001; Moskalik 1985). During such limit cycles, the amplitude of the parent mode first increases slowly on a timescale of , then decreases rapidly on a timescale of . A the same time, the amplitude of the daughter modes follow the opposite behavior. In sdB stars, we point out that the linear growth rate of the parent mode κ_{0} would be usually far smaller than the damping rate of the daughter modes κ_{1,2}. We further mention that the nonlinear interactions between the parent/child modes would also affect their periods as a result of phase variations. The nonlinear frequency shift could be of the order of a few μHz in some extreme conditions (Wu & Goldreich 2001; Moskalik 1985). We point out that a parametric instability can also occur in multiplets. In such circumstances, different m components that forms the multiplet may share some common damped daughter modes. Having common daughter modes involved in different parametric resonances, that is, involving different parent overstable components, will obviously induce more complex dynamic modulations than simple periodic variations that could be expected from pure threemode only interactions. We indeed point out that both the triplet resonance that was explored by Buchler et al. (1995, 1997) and the threemode ν_{0} ~ ν_{1} + ν_{2} resonances that were investigated by Dziembowski (1982), Moskalik (1985) and Wu & Goldreich (2001) are treated as isolated systems, i.e., assuming only interactions between the three involved modes and ignoring the possible influence of other modes. Modes with the highest amplitudes are more likely to efficiently couple with different resonances, such as in a multiplet resonance and in a ν_{0} ~ ν_{1} + ν_{2} resonance.
4. Connections with mode behaviors seen in KIC10139564
In light of the theoretical background summarized in the last section, we tentatively interpret some of the behaviors described in Sect. 2 for the frequencies listed in Table 1. These indeed show striking similarities with patterns expected for nonlinear resonant mode interactions that occur in various regimes.
4.1. Multiplets in the intermediate regime
The first connection is for the modes belonging to multiplets that show quasiperiodic amplitude and frequency modulations. In particular, the pmode triplet near 5760 μHz (T_{1}) shows indication that it could be evolving within the socalled intermediate regime of a triplet resonance. We recall (see Sect. 2; Fig.5) that the frequencies of the two side components in this triplet, besides showing a long term drift, vary quasiperiodically in antiphase with a timescale of ~ 550 days. The central component of T_{1}, for its part, has a frequency modulation which also vary, possibly with a slightly longer period of ~ 600 days. For comparison purposes, the modulation timescale is expected to be related to the inverse of the linear (i.e., unperturbed) frequency asymmetry in the triplet (see Eq. (4)), which therefore should be δν ~ 0.02μHz. Assuming that this frequency asymmetry originally comes from the second order effect of slow rotation, and given the average rotation frequency of the star (~ 0.42μHz, corresponding to ~ 26 days), the D_{kℓ} coefficient in Eq. (1) can be estimated to ~ 200 for that mode. This value is plausible because the D_{kℓ} coefficient is found to vary over a large range for dipole pmodes (Dziembowski & Goode 1992; Saio 1981). However, to compute D_{kl} in this specific case and compare with this value, a precise seismic solution for KIC 1013956 has to be worked out, but is not available yet. It has to be noted that the frequency asymmetry measured from the averaged frequencies given in Table 1 is only 0.0026 μHz that is one order of magnitude lower than the value derived from the modulation frequency (~ 0.02 μHz). We note, however, since the frequencies are varying with time, that the maximum extent of the observed frequency asymmetry is ~ 0.02 μHz when considering the 33 measurements independently (see Fig. 4). We point out that these observed values (0.0026 μHz on average and ~ 0.02 μHz for the maximum asymmetry) are similar to those observed in the main triplet of the DBV star KIC 08626021, which is also in the intermediate regime (Z16). Nonlinear resonant interactions are bound to perturb the linear frequencies of the modes, forcing them in some cases to shift toward the exact resonance (obtained when the system is locked). It is therefore not surprising to observe a frequency asymmetry that can be significantly smaller than the theoretical shift expected in the linear theory context.
In terms of amplitude modulations, the situation is bit less clear as only the prograde component in T_{1} shows a quasiperiodic modulation, with a timescale of ~ 800 days, while, for the other two components, particularly for the retrograde mode, their amplitude variations appear somewhat irregular.
In addition to the frequency variations of T_{1} discussed above, we note that the three components that form this triplet feature a regular drift toward each other which, if nothing change, would lead them to merge into one frequency on a timescale of ~ 10 yr. Such a merging is of course not conceivable and what we observe is more likely a small fraction of a variation cycle occurring on a timescale much longer than the duration of the Kepler observations. This suggests that the triplet resonance is probably not the only mechanism that affects the stability of T_{1}. This added complexity may also explain the more erratic behavior of the amplitude variations in this triplet. Quite notably, we indeed find that all the components of T_{1} can be linked to other frequencies forming linear combinations satisfying the conditions for a threemode resonance ν_{0} ~ ν_{1} + ν_{2}. This will be further discussed in Sect. 4.4.
The quintuplet Q_{1} also shows components with amplitude and frequency variations (see Fig. 10) that may be associated to the intermediate regime. In this case, however, we cannot estimate timescales for the modulations which appear to have a more complex behavior than the modulations detected in the T_{1} triplet or, if we compare to other cases, in the triplets of the pulsating DB star KIC 08626021 (Z16). The averaged frequency mismatch, δν_{o}, for Q_{1} is about 0.0018 μHz. This could either be the result of the nonlinear coupling mechanism locking the modulated components close to the exact resonance, even if they are in the intermediate regime (see the case of T_{1}, as well as the triplets in the DBV star KIC 08626021), or it could indicate that the modulation timescale for Q_{1} is ~ 17.6 yr (the inverse to δν_{o}, if their amplitudes have a periodic behavior). As there has been no theoretical exploration of the nonlinear fivemode interaction yet, the connection of Q_{1} with the intermediate regime is based on the assumption that nonlinear fivemode interactions has also mainly three distinct regimes. The coupled amplitude equations for the fivemode resonance involve more terms in each AE and the numerical solutions are more difficult to search for.
Another case may be connected with the intermediate regime: the multiplet M_{1} which shows amplitude and frequency variations (see Fig. 11). But, again, we cannot determine any timescale for the complex modulations occurring in this multiplet. In that case, there is also a slow trend leading frequencies, particularly for the most side components, to seemingly converge. This trend is very similar to the slow variation observed in the T_{1} triplet. It could possibly be a fraction of a variation cycle with a much longer timescale than the duration of the observations, but more observations would be needed to confirm this hypothesis. This multiplet M_{1} should be the siege of even more complex resonant coupling interactions than the quintuplet Q_{1}, since there are six detected components, with at least three components missing.
4.2. Triplets in the transitory regime
Another type of behavior encountered in our data can be linked to the narrow transitory hysteresis regime which is between the frequency lock and intermediate regimes. This state is characterized by stable frequencies but varying amplitudes. This is notably observed in the gmode triplet T_{2} (see Fig. 6). For this triplet, the observed frequency mismatch is about 0.0036 μHz, that is, very similar to the value measured for the T_{1} triplet (see lefttop panel of Figs. 4 and 6). We also point out that T_{2} may couple with the pmode triplet T_{1} through a threemode resonance ν_{0} ~ ν_{1} + ν_{2}, as discussed in Sect. 4.4.
The incomplete triplet D_{1} may also be associated to this transitory regime as it shows quasiperiodic amplitude modulations and stable frequencies. Due to the missing component, we cannot measure the frequency mismatch for this doublet. We note that the AEs for the triplet resonance indicate that the modes cannot be stable, i.e, there is no fixedpoint solution, if one of the visible modes forming the incomplete triplet is the central (m = 0) component (Buchler et al. 1995). Thus, at this stage, we may just fail to detect either the third component of the triplet whose amplitude may be lower than the detection threshold (meaning that the triplet is indeed in the narrow transitory regime), or the nonlinear modulation of the frequencies, which may be smaller in amplitude than our current precision (meaning a doublet in the intermediate regime, as predicted by the AEs).
4.3. A triplet in the frequencylocked regime
The last case occurring in a different regime is the gmode triplet T_{3}, which shows stable amplitudes and frequencies (see Figs. 7 and 8). This suggests that T_{3} is in the configuration of the frequencylocked regime where the triplet approaches the resonance center, i.e., δν → 0 and both the frequencies and amplitudes are constant. Indeed, we find that the observed frequency asymmetry, δν_{o}, is 0.0008 μHz (Fig. 7) for T_{3}, which is less than the measured error 0.0011 μHz. The triplet T_{3} is therefore exactly (within measurement errors) at the resonance center, contrary to T_{1} and also T_{2} which has constant frequencies but a small nonzero frequency mismatch.
In summary, the various behaviors encountered in the multiplets detected in KIC 10139564 seem to cover all the different regimes expected in a context of resonant mode coupling in multiplets. This mechanism is therefore quite likely responsible, at least in part, for the observed phenomena. In the following section, we discuss another type of resonance, the ν_{0} ~ ν_{1} + ν_{2} nonlinear interaction.
4.4. Threemode resonance
In this section, we discuss the variations of a group of frequencies C_{1}, including f_{23}, f_{35} and f_{74}, that are involved in a relationship ν_{0} ~ ν_{1} + ν_{2}. We find that the variations of these frequencies have strong correlations with the variations of the components in the triplet T_{1} (see Figs. 4 and 12). The large frequency variations first suggest that the C_{1} frequencies correspond to threemode resonances rather than simple linear combination frequencies. The result of prewhitening the frequencies f_{23} and f_{35} (using the same method as for the multiplets) is shown in Figs. 13 and 14, respectively. Most of the amplitude and frequency measurements for f_{23} and f_{35} are exactly following the variation of amplitude and frequency of the sums f_{1} + f_{11} and f_{3} + f_{21} within 1σ, respectively (see in particular the middle and bottom panels of Figs. 13 and 14).
The amplitude ratio R is 37 and 85 for f_{23} ~ f_{1} + f_{11} and f_{35} ~ f_{3} + f_{21}, respectively. These values are significantly higher than those observed for normal linear combination frequencies in sdB stars (see the example given in Sect. 3.2). There is also a possible true linear combination frequency in KIC 10139564 with the frequency f_{79} ~ f_{1}−f_{4} (see Table 2) which indeed has a very low amplitude (signaltonoise ratio of 5.1) and an amplitude ratio R less than one. Thus, we propose that there should be real pulsation modes near the position of the linear combination frequencies f_{1} + f_{11} and f_{3} + f_{21} and these modes had their amplitudes boosted through a resonance. In the ν_{0} ~ ν_{1} + ν_{2} resonance, the child mode indeed follows the behavior of its parent modes (see, again, Figs. 13 and 14 and examples provided by Breger & Montgomery 2014).
Fig. 13 Amplitude and frequency variations of the linear combination frequency f_{23} = f_{1} + f_{11}. Top panel: measured amplitudes as a function of time obtained from each data subset (using the same method as for multiplets). Middle panel: measured frequencies from each data subset compared with the frequency sum f_{1} + f_{11}, both as a function of time. Bottom panel: observed amplitudes of f_{23} vs predicted amplitudes of R × the product of f_{1} and f_{11} amplitudes (see Eq. (6) for the definition of R). In both cases (frequency and amplitude comparisons), the measurements are found to be within 1σ. 

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Fig. 14 Same as Fig. 13 but for the linear combination frequency f_{35} = f_{3} + f_{21}. Note that there are ten missing measurements for f_{21}, including the first nine data points, because the amplitudes were lower than 4σ. The last data point is also not shown because of a large associated error, this measurement being at the end of the data set. 

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We note that another frequency, f_{74}, is also in the region near 6076 μHz, but has an amplitude too low to be monitored over time using the prewhitening technique on subsets of the data. However, Fig. 12 still clearly shows that this frequency is varying smoothly during the observation, from ~ 6076.58 μHz (the first half part of the run) to ~ 6076.68 μHz (the second half part). We speculate that there is possibly a real mode, with a frequency around 6076.58−6076.69 μHz, which first interacts with the frequency sum f_{2} + f_{39} ~ 6076.59 μHz, then with the frequency sum f_{3} + f_{11} ~ 6076.66 μHz, because the influence from the latter modes become stronger than the former ones during the last half of the observation run, due to the amplitude of f_{3} increasing significantly in the second half of the Kepler time series. This, again, suggests that the C_{1} frequencies are really part of ν_{0} ~ ν_{1} + ν_{2} resonances instead of being simple linear combination frequencies.
All of the involved frequencies, f_{1,2,3,11,21,39}, are the components of the triplets T_{1} and T_{2}. They are expected to be overstable (driven) modes, thus meaning that they are involved in a threemode direct resonance and not a parametric resonance which involves one overstable parent mode and two damped unstable daughter modes.
At this stage, it becomes natural to interpret the complex variations observed in the components of T_{1} and T_{2} to be linked with the fact that these modes are simultaneously involved in two different types of resonances, that is, a triplet resonance and ν_{0} ~ ν_{1} + ν_{2} direct resonances. In this situation, the triplet resonance may be the dominating nonlinear interaction occurring in the triplet, while the nonlinear coupling with the modes outside the triplet could strongly perturb the periodic amplitude and frequency modulations expected if the triplets were pure isolated systems. This shows that nonlinear mode interactions in real stars are certainly more complex configurations than those treated by current simplified theoretical approaches. Moreover, since the T_{2} triplet is in the transitory regime, with frequencies locked by the nonlinear coupling within the triplet, the nonlinear interactions outside this triplet are therefore unable to destroy this frequency locking, resulting in no longterm frequency variation as can be seen in the T_{1} triplet. Interestingly, the resonant mode coupling theory predicts that a limit cycle (steady equilibrium state) may not be reached in the case of threemode direct resonance (which is likely at work here as discussed above). The evolution of this longterm frequency variation in T_{1}, whether the mode frequencies will further converge or eventually diverge, and the evolution of T_{2}, whether frequencies will remain constant or the locked regime will eventually be broken, will need further observation either from ground or by future space instruments currently in preparation such as TESS and PLATO (Rauer et al. 2014; Ricker et al. 2014).
4.5. The Dparameter and further insight on the modulations
The value of the Dparameter, that defines how far the modes are from the resonance center, is usually connected to the kind of regime a multiplet is in when undergoing resonant mode interactions. This Dvalue is in particular sensitive to the linear growth rate of the oscillation modes (see again Sect. 3).
For the frequencylocked regime that is observed in KIC 10139564 with the T_{3} triplet, D is near or exactly zero, as predicted by the AEs (Buchler et al. 1995; Goupil et al. 1998). The Dvalue for the other triplets T_{1} (δν_{o} ~ 0.0026 μHz) and T_{2} (δν_{o} ~ 0.0036 μHz) may reflects more their linear growth rates since, with very similar frequency mismatches, the two triplets are found to be in different regimes. The growth rate values are indeed substantially different between p and gmodes (Charpinet 1999; Fontaine et al. 2003). Assuming the growth rate for pmodes is of the order of 10^{6} s^{1} (Charpinet 1999), the corresponding D value for the T_{1} triplet would be far less than one, indicating that T_{1} should be in the frequencylocked regime (Buchler et al. 1997; Goupil et al. 1998), but we find it to be in the intermediate regime. We note however that this estimate for the value of D is based on the measured frequency mismatch which may not be representative of the unperturbed frequency asymmetry that enters in the definition of D. The latter is likely much larger (see Sect. 4.1), leading to a somewhat larger Dvalue more in line with the observed regime of the resonance for T_{1}. The Dvalue for the gmode triplet T_{2}, for its part, could be much larger than that of T_{1}, considering the much smaller growth rates of the ℓ = 1gmodes (Fontaine et al. 2003). Extended ranges for D were also found in the DBV star KIC 08626021 (Z16), where the Dvalues for the triplets are at least two orders of magnitude larger than those suggested in Goupil et al. (1998). This suggests that the nonlinear behaviors not only depend on the magnitude of D, but also on the specific coupling coefficients for each specific mode (Buchler et al. 1995).
Further quantitative comparisons between the observed modulations and the theoretical framework would require to solve the amplitude equations for the specific case of KIC 10139564. This would require to calculate the coupling coefficients in the AEs, which, in principle, could be extracted from the observed amplitude and frequency modulations (Buchler et al. 1995). With these known coupling coefficients, one could then determine the ranges of Dvalues related to each different regime of the nonlinear resonance. A measurement of the growth rates of the oscillation modes would then possibly follow with the determination of this parameter, which may lead for the first time to an independent estimation of the linear nonadiabatic growth rates of the modes and a direct test of nonadiabatic pulsation calculations in sdB stars.
5. Summary and conclusion
While studying the highquality and longduration photometric data provided by the Kepler spacecraft on the pulsating sdB star KIC 10139564, we have identified different patterns in the frequency and amplitude modulations of the oscillation modes belonging to several rotationally split multiplets or linear combination frequencies. These modulations show signatures that can be associated to nonlinear resonant mode coupling mechanisms that could occur between the multiplet components themselves and with other modes under certain conditions, that is, satisfying a ν_{0} ~ ν_{1} + ν_{2} resonance relationship. This is the first time that such signatures are quite clearly identified in pulsating hot B subdwarf stars, and the second case reported so far for a compact pulsator monitored with Kepler photometry (see Z16).
We first reanalyzed the 38month of Kepler photometry obtained for KIC 10139564, leading to the detection of 60 independent frequencies above a secured detection threshold (5.6σ; see Table A.1). Among these, 29 frequencies consist of three triplets, one doublet, one quintuplet and two incomplete multiplets with ℓ> 2 (see Table 1). Another three detected frequencies are linked to other frequencies through linear combinations. Five additional groups of frequencies are found in the region between 5400 and 6400 μHz, which have very complicated structures. Finaly, we also find 14 independent frequencies and two frequencies satisfying linear combination relationships that could be real as their amplitudes are between 5σ and 5.6σ above the noise. In general, our well secured frequencies are in good agreement with the former analysis from Baran et al. (2012). In this paper, we particularly concentrated our study on six multiplets and three linear combination frequencies observed near 6076 μHz.
We found different types of mode behaviors occurring in the above mentioned frequencies. A “short timescale” quasiperiodic amplitude and frequency modulations along with a slow trend of the frequencies to convergence toward each other occur in the dominant pmode triplet near 5760 μHz (T_{1}). The ~ 570day quasiperiodic frequency modulation evolve in antiphase between the two side components in this triplet. Modulated frequencies and amplitudes are also found in a quintuplet near 5287 μHz (Q_{1}) and a (ℓ> 2) multiplet near 5412 μHz (M_{1}), but the modulations do not show a clear periodicity. One triplet near 316 μHz (T_{2}) has a distinct behavior from the above mentioned multiplets, as it shows stable frequencies but varying amplitudes. A similar phenomenon occurs in a doublet near 394 μHz (D_{1}) which shows constant frequencies and an ~ 1100 days periodic amplitude modulations. Another triplet at 518 μHz (T_{3}) completely differs from all the above multiplets, with constant amplitudes and frequencies throughout the whole observation run. In addition, we also discovered amplitude and frequency variations in three frequencies near 6076 μHz (C_{1}) that are linked to other independent frequencies through linear combinations.
After ruling out various possible causes for the modulations, we showed that these mode behaviors could be related to the different types of nonlinear resonances that should occur according to the amplitude equation formalism. In particular, nonlinear resonant couplings within a multiplet can lead to three main regimes, all of which are possibly occurring in KIC 10139564. The multiplets T_{1}, Q_{1} and M_{1} can be associated with the intermediate regime of the resonance where the involved modes have modulated amplitudes and frequencies. The triplet T_{2} and doublet D_{1} have a different behavior that could be associated to a narrow transitory regime in which the frequencies of the modes can be locked (constant) while the amplitudes experience modulations. The behavior of the triplet T_{3} is the unique case found in this star that can be associated to the frequency lock regime of the resonance, where both amplitudes and frequencies are stable. In addition, the large amplitude ratios between the C_{1} frequencies and their main parent modes, together with the large variation of amplitude and frequency observed for these peaks, suggest that C_{1} correspond to threemode direct resonances. We indeed found that the frequencies of C_{1} exactly follow the evolution of their main parent modes. Moreover, as the parent modes of C_{1} are also the components of T_{1} and T_{2}, we suggest part of the complexity of the mode behaviors could be related to these cross interactions between the various modes. In particular, the slow variations occurring in T_{1} may be related to the ν_{0} ~ ν_{1} + ν_{2} resonance superimposed to the triplet resonance occurring between the components.
We emphasize that the observed frequency modulations likely induced by nonlinear mode interactions could challenge future attempts to measure the evolutionary effects on the oscillation mode periods in pulsating sdB stars. Compared to the resonant variations taking place on timescales of years, the rate of period change of the pulsations due to stellar evolution in sdB stars is much longer, typically occurring on a timescale of ~ 10^{6} yr (Charpinet et al. 2002). Nonlinear modulations of the frequencies can potentially jeopardize any attempt to measure reliably such rates, unless they can be corrected beforehand. These nonlinear modulations could also complicate the detection of exoplanets or stellar companions around sdB stars using the technique of measuring phase changes in the pulsations (Silvotti et al. 2007). It should be possible however to distinguish between the two effects, considering that nonlinear couplings may induce different behaviors on different modes, while external causes such as an orbiting body should affect all modes similarly.
Finally, we note that our analysis suggests that resonances occurring in real stars, in which modes could be involved in two or more types of different couplings, lead to more complicated patterns than those predicted by current theoretical frameworks which treat the modes only as isolated systems within one type of resonance and ignore the nonlinear interactions that could occur simultaneously outside of the system. This should motivate further theoretical work to develop nonlinear stellar pulsation theory for more precise predictions of the mode behaviors in pulsating stars in general.
6. Additional table
List of frequencies detected in KIC 10139564.
The asymmetry would be proportional to the strength of magnetic field and the frequency of each component of the triplet (except the central, m = 0, one) would be shifted in the same direction (Jones et al. 1989).
Acknowledgments
Funding for the Kepler mission is provided by NASA’s Science Mission Directorate. We greatfully acknowledge the Kepler Science Team and all those who have contributed to making the Kepler mission possible. WKZ acknowledges the financial support from the China Scholarship Council. This work was supported in part by the Programme National de Physique Stellaire (PNPS, CNRS/INSU, France) and the Centre National d’Études Spatiales (CNES, France).
References
 Baran, A. S., & Østensen, R. H. 2013, Acta Astron., 63, 79 [NASA ADS] [Google Scholar]
 Baran, A., Pigulski, A., O’Toole, S. J. 2008, MNRAS, 385, 255 [NASA ADS] [CrossRef] [Google Scholar]
 Baran, A. S., Reed, M. D., Stello, D., et al. 2012, MNRAS, 424, 2686 [NASA ADS] [CrossRef] [Google Scholar]
 Brassard, P., Fontaine, G., & Wesemael, F. 1995, ApJS, 96, 545 [NASA ADS] [CrossRef] [Google Scholar]
 Breger, M., & Montgomery, M. H. 2014, ApJ, 783, 89 [NASA ADS] [CrossRef] [Google Scholar]
 Buchler, J. R., & Goupil, M. J. 1984, ApJ, 279, 384 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Buchler, J. R., & Kovacs, G. 1986, ApJ, 303, 794 [NASA ADS] [CrossRef] [Google Scholar]
 Buchler, J. R., Goupil, M.J., & Serre, T. 1995, A&A, 296, 405 [NASA ADS] [Google Scholar]
 Buchler, J. R., Goupil, M.J., & Hansen, C. J. 1997, A&A, 321, 159 [NASA ADS] [Google Scholar]
 Carroll, B. W., & Hansen, C. J. 1982, ApJ, 279, 394 [Google Scholar]
 Charpinet, S. 1999, Ph.D. Thesis, Univ. Montréal [Google Scholar]
 Charpinet, S., Fontaine, G., Brassard, P., & Dorman, B. 1996, ApJ, 471, L103 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Charpinet, S., Fontaine, G., Brassard, P., et al. 1997, ApJ, 483, L123 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Charpinet, S., Fontaine, G., Brassard, P., & Dorman, B. 2002, ApJS, 140, 469 [NASA ADS] [CrossRef] [Google Scholar]
 Charpinet, S., Green, E. M., Baglin, A., et al. 2010, A&A, 516, L6 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Charpinet, S., Van Grootel, V., Fontaine, G., et al. 2011, A&A, 530, A3 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Deeming, T. J. 1975, Ap&SS, 36, 137 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Dziembowski, W. A. 1982, Acta Astron., 32, 147 [NASA ADS] [Google Scholar]
 Dziembowski, W. A., & Goode, P. R. 1992, ApJ, 394, 670 [NASA ADS] [CrossRef] [Google Scholar]
 Fontaine, G., Brassard, P., Charpinet, S., et al. 2003, ApJ, 597, 518 [NASA ADS] [CrossRef] [Google Scholar]
 Fontaine, G., Brassard, P., Charpinet, S., et al. 2012, A&A, 539, A12 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Gilliland, R. L., Timothy, M., ChristensenDalsgaard, J., et al. 2010, PASP, 122, 131 [NASA ADS] [CrossRef] [Google Scholar]
 Green, E. M., Fontaine, G., Reed, M. D., et al. 2003, ApJ, 583, L31 [NASA ADS] [CrossRef] [Google Scholar]
 Goupil, M. J., & Buchler, J. R. 1994, A&A, 291, 484 [NASA ADS] [Google Scholar]
 Goupil, M. J., Dziembowski, W. A., & Fontaine, G. 1998, Balt. Astron., 7, 21 [NASA ADS] [Google Scholar]
 Heber, U. 2009, ARA&A, 47, 211 [NASA ADS] [CrossRef] [Google Scholar]
 Jenkins, J. M., Caldwell, D. A., Chandrasekaran, H., et al. 2010, ApJ, 713, L87 [NASA ADS] [CrossRef] [Google Scholar]
 Jones, P. W., Hansen, C. J., Pesnell, W. D., & Kawaler, S. D. 1989, ApJ, 336, 403 [NASA ADS] [CrossRef] [Google Scholar]
 Kawaler, S. D., Reed, M. D., Quint, A. C., et al. 2010, MNRAS, 409, 1487 [NASA ADS] [CrossRef] [Google Scholar]
 Kilkenny, D. 2007, Commun. Asteroseismol., 150, 234 [NASA ADS] [CrossRef] [Google Scholar]
 Kilkenny, D. 2010, Ap&SS, 329, 175 [NASA ADS] [CrossRef] [Google Scholar]
 Kilkenny, D., Koen, C., O’Donoghue, D., & Stobie, R. S. 1997, MNRAS, 285, 640 [NASA ADS] [CrossRef] [Google Scholar]
 Landstreet, J. D., Bagnulo, S., Fossati, L., Jordan, S., & O’Toole, S. J. 2012, A&A, 541, A100 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Montgomery, M. H., & Odonoghue, D. 1999, Delta Scuti Star Newsletter, 13, 28 [NASA ADS] [Google Scholar]
 Moskalik, P. 1985, Acta Astron., 35, 229 [NASA ADS] [Google Scholar]
 Østensen, R. H., Reed, M. D., Baran, A. S., & Telting, J. H. 2014, A&A, 564, L14 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Petit, P., Van Grootel, V., Bagnulo, S., et al. 2012, in Fifth Meeting on Hot Subdwarf Stars and Related Objects, ASP Conf. Ser., 452, 87 [NASA ADS] [Google Scholar]
 Rauer, H., Catala, C., Aerts, C., et al. 2014, Exp. Astron., 38, 249 [NASA ADS] [CrossRef] [Google Scholar]
 Reed, M. D., O’Toole, S. J., Terndrup, D. M., et al. 2007, ApJ, 664, 518 [NASA ADS] [CrossRef] [Google Scholar]
 Ricker, G. R., Winn, J. N., Vanderspek, R., et al. 2014, SPIE, 9143E, 20 [NASA ADS] [Google Scholar]
 Saio, H. 1981, ApJ, 244, 299 [NASA ADS] [CrossRef] [Google Scholar]
 Salabert, D., García, R. A., & TurckChièze, S. 2015, A&A, 578, A137 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Scargle, J. D. 1982, ApJ, 263, 835 [NASA ADS] [CrossRef] [Google Scholar]
 Schuh, S., Hubber, J., Dreizler, S., et al. 2006, A&A, 445, 131 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Silvotti, R., Schuh, S., Janulis, R., et al. 2007, Nature, 449, 189 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Unno, W., Osaki, Y., Ando, H., Saio, H., & Shibahashi, H. 1989, Nonradial oscillations of stars, 2nd edn. (Tokyo: University of Tokyo Press) [Google Scholar]
 van Grootel, V., Charpinet, S., Fontaine, G., et al. 2010, ApJ, 718, L97 [NASA ADS] [CrossRef] [Google Scholar]
 Van Hoolst, T. 1994, A&A, 292, 183 [Google Scholar]
 van Kerkwijk, M. H., Clemens, J. C., & Wu, Y. 2000, MNRAS, 314, 209 [NASA ADS] [CrossRef] [Google Scholar]
 Vauclair, G., Fu, J.N., Solheim, J. E., et al. 2011, A&A, 528, A5 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Wu, Y. 2001, MNRAS, 323, 248 [NASA ADS] [CrossRef] [Google Scholar]
 Wu, Y., & Goldreich, P. 2001, ApJ, 546, 469 [NASA ADS] [CrossRef] [Google Scholar]
 Zong, W., Charpinet, S., Vauclair, G., et al. 2016, A&A, 585, A22 (Z16) [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
All Tables
All Figures
Fig. 1 Top panel: condensed representation of the full Kepler light curve of KIC 10139564 (Amplitude as the residual relative to the mean brightness intensity of the star vs time in Barycentric Julian Date) covering from Q5.1 to Q17.2 (~ 1147.5 days). Bottom panel: closeup view showing 0.8 days of the Kepler light curve by slices of 0.08 days. At this scale the oscillations are clearly apparent. 

Open with DEXTER  
In the text 
Fig. 2 LombScargle periodogram (LSP; amplitude in % of the mean brightness vs frequency in μHz) of the Kepler light curve for KIC 10139564. The represented range, up to the Nyquist frequency, covers the longperiod gmode and the shortperiod pmode frequency domains. The region between the two dashed vertical lines at 5200 and 6400 μHz is where peaks have the largest amplitudes. However, weaker peaks outside of this particular region are present and are made visible by scaling up amplitudes by a factor of 20. The dashed horizontal line represents the 5.6σ detection threshold (see text). Some wellknown Kepler instrumental artefacts are present, but can easily be recognized. 

Open with DEXTER  
In the text 
Fig. 3 Left panel: 2D distribution of the frequency and amplitude deviations between the prewhitened and the injected values for 1000 artificial modes of constant amplitude. S/N denotes the signaltonoise ratio of the injected signals and the deviations have been normalized by the 1σ error, σ_{A} and σ_{f}, derived from the prewhitening procedure implemented in the code Felix. The 2D distribution is also projected into 1D histograms (frequency and amplitude) to be compared with the Normal Distribution, plotted as a red solid curve. Right panel: same as above but for 1000 modes with random amplitudes. The injected modes are divided into three groups of S/N in the ranges [5,15], (15,25], and (25,60], respectively (represented by three different colors and symbols). 

Open with DEXTER  
In the text 
Fig. 4 Frequency and amplitude modulations in the T_{1}pmode triplet near 5760 μHz. Topleft panel presents the fine structures of the well defined triplet with near symmetric frequency spacings. The dashed horizontal line in red represents the 5.6 σ detection threshold. Middleleft panel shows the sliding LombScargle periodogram (sLSP giving the amplitude in % as a function of frequency in μHz and time in days) of the triplet as a whole. Bottomleft panel shows expanded views around the average frequency (the solid vertical lines, also in the middle left panel) of each component, obtained from prewhitening subsets of the data, thus measuring precisely the frequencies, as a function of time. Right panel provides the measured amplitudes as a function of time obtained for each subset of data (see text for details). Note that the errors for each measurement is smaller than the symbol itself. 

Open with DEXTER  
In the text 
Fig. 5 Frequency modulations after removing the longterm trend in the T_{1} triplet by applying a secondorder polynomial fit. The solid curves represent the best fits of one pure sine wave to the frequency modulations. The associated formal errors for the periods and phases are also estimated. 

Open with DEXTER  
In the text 
Fig. 6 Same as Fig. 4 but for the T_{2}gmode triplet near 316 μHz. 

Open with DEXTER  
In the text 
Fig. 7 Same as Fig. 4 but for the T_{3}gmode triplet near 519 μHz. 

Open with DEXTER  
In the text 
Fig. 8 Frequency and amplitude scattering for the three components forming the gmode triplet T_{3} around their averaged values. The red and blue dashed rectangles indicate the 2σ and 3σ error boxes, respectively. All the data points are within 3σ. 

Open with DEXTER  
In the text 
Fig. 9 Same as Fig. 4 but for the D_{1}gmode doublet near 394 μHz. The solid curves in right panel show the best fit of a pure sine wave to the amplitude modulations. 

Open with DEXTER  
In the text 
Fig. 10 Same as Fig. 4 but for the Q_{1}pmode quintuplet near 5287 μHz. 

Open with DEXTER  
In the text 
Fig. 11 Same as Fig. 4 but for the ℓ> 2pmode multiplet M_{1} near 5413 μHz. Note that at least three components are missing in this multiplet and the red vertical dashed lines indicate the expected position for two of them. 

Open with DEXTER  
In the text 
Fig. 12 Frequency and amplitude modulations of a group of linear combination frequencies C_{1} near 6076 μHz. The red dashed line indicates the 5.6σ detection threshold. The green shadowed areas in top panel represent the scales of variation of these frequencies (see text for details). 

Open with DEXTER  
In the text 
Fig. 13 Amplitude and frequency variations of the linear combination frequency f_{23} = f_{1} + f_{11}. Top panel: measured amplitudes as a function of time obtained from each data subset (using the same method as for multiplets). Middle panel: measured frequencies from each data subset compared with the frequency sum f_{1} + f_{11}, both as a function of time. Bottom panel: observed amplitudes of f_{23} vs predicted amplitudes of R × the product of f_{1} and f_{11} amplitudes (see Eq. (6) for the definition of R). In both cases (frequency and amplitude comparisons), the measurements are found to be within 1σ. 

Open with DEXTER  
In the text 
Fig. 14 Same as Fig. 13 but for the linear combination frequency f_{35} = f_{3} + f_{21}. Note that there are ten missing measurements for f_{21}, including the first nine data points, because the amplitudes were lower than 4σ. The last data point is also not shown because of a large associated error, this measurement being at the end of the data set. 

Open with DEXTER  
In the text 