Abstract:
We study intensity oscillations near the apex of a coronal loop to find the signature of MHD oscillations.
We analyse the time series of the strongest Fe XII 195.12 Å image data, observed by 40" SLOT of the EUV
Imaging Spectrometer (EIS) onboard the Hinode spacecraft. Using a standard wavelet tool, we produce
power spectra of intensity oscillations at location ‘Lз ’ near the apex of a clearly visible coronal loop.
We detect intensity oscillations of a period of ≈322 s with a probability of 96%. This oscillation period
of ≈322 s is found to be in good agreement with theory of the multiple (first and second) harmonics
of standing slow acoustic oscillations of P₂and slow ≈ 313 ± 31 s. We detect, for the first time, the observational signature of multiple (first and second) harmonics of slow acoustic oscillations in the non-flaring
coronal loop. Such oscillations have been observed in the past in hot and flaring coronal loops only, but have been predicted recently to exist in comparatively cooler and non-flaring coronal loops as well. We
find the periodicities ~497 s and ~592 s with the probability 99–100% at the ‘L ₁’ and ‘L₂’ locations,
respectively, near the clearly visible western footpoint of the loop. We interpret these Oscillations be likely associated with the first harmonics (fundamental mode) of slow acoustic oscillations. Using
the period ratios P ₁ /P₂= 1:54 and 1:84, we estimate the density scale heights in the EUV loop as ~10 Mm and 21 Mm, respectively, in which the latter value (~21 Mm) is compared well with the loop
half length. We also find an evidence of propagating bright blob at its lower bound sub-sonic speed of
≈6.4 km/s, suggesting that they are caused by the mass flow from one end to the other in the coronal
loop. We also suggest that standing oscillations, and propagating bright blobs caused probably by the
pulse of plasma flow, co-exist in comparatively cooler and non-flaring coronal loop.
