@inproceedings{stan2026-PREX-77FV,
    author = {{Stanislavsky}, A. A. and {Bubnov}, I. N. and {Stanislavsky}, L. A. and {Zarka}, P. and {Loh}, A. and {Viou}, C. and {Konovalenko}, A. A. and {Vashchishyn}, R. V.},
    title = {{NenuFAR Observations of Scintillation During High Solar Activity}},
    booktitle = {Planetary, Solar and Heliospheric Radio Emissions X},
    publisher = {OSU Pyth{\'{e}}as/AMU, Observatoire de Paris}
    year = {2026},
    editor = {{Lamy}, L. and {Louis}, C. K. and {Fischer}, G. and {Morosan}, D. E. and {Zarka}, P.},
    pages = {},
    doi = {10.25935/PREX-77FV},
    abstract = {{We present a reproducible diagnostic framework for detecting interplanetary scintillation (IPS) in low-frequency radio observations of compact sources with the New Extension in Nançay upgrading LOFAR (NenuFAR). Power spectral densities were estimated using Welch's method and partitioned into ionospheric (<0.05 Hz) and interplanetary (0.05–1.0 Hz) bands, with IPS ratios defined as the fraction of power in the latter. Bootstrap resampling provided empirical confidence intervals, while Gaussian fits to autocorrelation functions yielded scintillation timescales via full width at half maximum (FWHM). Applying this chain to multi-channel observations of Cassiopeia A and Cygnus A, we find systematically higher IPS ratios and narrower FWHM for Cas A, with statistically significant separation confirmed by both two-sample t-tests (p = 0.0006) and non-overlapping bootstrap confidence intervals. These results demonstrate that IPS dominates the fast fluctuations in Cas A, while Cyg A serves as a control for ionospheric scintillation. In agreement with Fallows et al. (2020), we acknowledge possible D-region contributions at low frequencies, but our multi-source comparison rules out ionospheric contamination as the sole explanation. The methodology provides a transparent, transferable standard for IPS detection, applicable to other compact sources and coordinated multi-station campaigns.}}
}