[논문]TEMPORAL VARIATIONS OF THE GLOBAL SEISMIC PARAMETERS OF HD 49933 OVER A MAGNETIC CYCLE

Kim, Ki-Beom; Chang, Heon-Young

doi:10.5303/jkas.2021.54.4.129

[국내논문] TEMPORAL VARIATIONS OF THE GLOBAL SEISMIC PARAMETERS OF HD 49933 OVER A MAGNETIC CYCLE 원문보기

Journal of the Korean astronomical society = 천문학회지, v.54 no.4, 2021년, pp.129 - 137

Kim, Ki-Beom (Department of Astronomy and Atmospheric Sciences, Kyungpook National University) , Chang, Heon-Young (Department of Astronomy and Atmospheric Sciences, Kyungpook National University)

Abstract ▼ AI-Helper

It has been established that the acoustic mode parameters of the Sun and Sun-like stars vary over activity cycles. Since the observed variations are not consistent with an activity-related origin, even Sun-like stars showing out-of-phase changes of mode frequencies and amplitudes need to be carefully studied using other observational quantities. In order to test whether the presumed relations between the global seismic parameters are a signature of the stellar activity cycle, we analyze the photometric light curve of HD 49933 for which the first direct detection of an asteroseismic signature for activity-induced variations in a Sun-like star was made, using observations by the CoRoT space telescope. We find that the amplitude of the envelope significantly anti-correlates with both the maximum frequency of the envelope and the width of the envelope unless superflare-like events completely contaminate the light curve. However, even though the photometric proxy for stellar magnetic activity appears to show relations with the global asteroseismic parameters, they are statistically insignificant. Therefore, we conclude that the global asteroseismic parameters can be utilized in cross-checking asteroseismic detections of activity-related variations in Sun-like stars, and that it is probably less secure and effective to construct a photometric magnetic activity proxy to indirectly correlate the global asteroseismic parameters. Finally, we seismically estimate the mass of HD 49933 based on our determination of the large separation of HD 49933 with evolutionary tracks computed by the MESA code and find a value of about 1.2M☉ and a sub-solar metallicity of Z = 0.008, which agrees with the current consensus and with asteroseismic and non-asteroseismic data.

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표/그림 (8)

표 Table 1 Stellar parameters of HD 49933
그림 Figure 2. The power spectral density (PSD) of HD 49933 resulting from the first 40-day-long time series in the second observing run. Note that the PSD is shown after removing the background red noise with the Karoff model with n = 2. Thus, the thick curve represents the sum of the envelope profile of the power excess for the acoustic oscillation and the background white noise.
그림 Figure 1. Light curves of HD 49933 observed by CoRoT for three separate observing runs, which are recorded with a cadence of 32 seconds for 60 days in 2007, 137 days in 2008, and 60 days in 2012 (from top to bottom, respectively). Note two superflare-like peaks from JD 2454480 to JD 2454520 which are suspected to be comparable to the Halloween solar storms in late 2003.
그림 Figure 3. Temporal variations in 𝛿v, A, v_max, and 𝛿v_env (from top to bottom, respectively). Data points result from each power spectrum of a 40-day-long time series shifted every 10 days in the second run of CoRoT observations.
그림 Figure 4. Scatter plots of v_max (top) and 𝛿v_env (bottom) against A. The solid and dashed lines represent the best fits resulting from 10 points and 9 points. See the text for details.
그림 Figure 5. Frequency of the maximum height in the acoustic power spectrum, 𝛿v, together with the photometric proxy for stellar magnetic activity, S_ph, as a function of time. The solid and dashed curves represent 𝛿v and S_ph, respectively.
그림 Figure 6. Scatter plots of A (top), v_max (center), and 𝛿v_env (bottom) against S_ph. The solid and dashed lines represent the best fits resulting from 10 points and 9 points. See the text for details.
그림 Figure 7. Seismic Hertzsprung{Russell diagram showing the large separation, Δv, as a function of the effective temperature, T_eff , with evolutionary tracks. The dotted gray lines connect the positions where the star is ~ 2:25 Gyr old, respectively. The locations of HD 49933 and the Sun are marked with an asterisk and its common sign (⊙), respectively. The solid and dashed curves result from two chemical compositions of Z = 0:008 and Z = 0:014 for a given mass denoted in the bottom of individual curves, respectively.

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