2021
DOI: 10.1002/asna.20210066
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Characterizing X‐ray activity cycles of young solar‐like stars with solar observations

Abstract: Throughout an activity cycle, magnetic structures rise to the stellar surface, evolve, and decay. Tracing their evolution on a stellar corona allows us to characterize the X-ray cycles. However, directly mapping magnetic structures is feasible only for the Sun, while such structures are spatially unresolved with present-day X-ray instruments on stellar coronae. We present here a new method, implemented by us, that indirectly reproduces the stellar X-ray spectrum and its variability with solar magnetic structur… Show more

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Cited by 4 publications
(1 citation statement)
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“…A similar amplitude is indicated by our 3 yr time series of the chromospheric Ca II H&K emission, and by comparison of the Si IV resonant doublet in our HST/COS G130M observation with that in a COS G160M spectrum taken 10 months before. This result is consistent with the trend of decreasing amplitude of magnetic activity cycles with increasing stellar high-energy fluxes (Wargelin et al 2017;Coffaro et al 2022).…”
Section: Discussionsupporting
confidence: 90%
“…A similar amplitude is indicated by our 3 yr time series of the chromospheric Ca II H&K emission, and by comparison of the Si IV resonant doublet in our HST/COS G130M observation with that in a COS G160M spectrum taken 10 months before. This result is consistent with the trend of decreasing amplitude of magnetic activity cycles with increasing stellar high-energy fluxes (Wargelin et al 2017;Coffaro et al 2022).…”
Section: Discussionsupporting
confidence: 90%