000007758 001__ 7758
000007758 005__ 20260108090157.0
000007758 037__ $$aOUTRART-2026-0005
000007758 100__ $$aShrivastav, A. K.  
000007758 245__ $$aCross-scale nature of decayless waves in the solar corona
000007758 260__ $$c2025
000007758 520__ $$aThe long-standing problem of coronal heating focuses on probing sources that can continuously supply energy to sustain million-degree temperatures. Magnetohydrodynamic (MHD) waves play a crucial role because their dissipation in the solar corona can supply the necessary energy to compensate for radiative losses. Moreover, MHD waves offer an effective tool for diagnosing local physical conditions through coronal seismology. Elucidating the characteristics of MHD waves across various coronal regions and at different spatial scales is crucial in the context of coronal heating and its driving mechanisms. Decayless transverse kink waves are a type of MHD wave mode in coronal loops with no significant decay in the wave amplitude over multiple cycles. These are omnipresent in active regions [1] which makes them a viable candidate for coronal heating [2]. Additionally, they  provide an essential tool to diagnose coronal magnetic fields in the quiet active region corona [3] .
000007758 594__ $$aSTCE
000007758 6531_ $$aSolar Orbiter
000007758 6531_ $$aEUI
000007758 6531_ $$awaves
000007758 700__ $$aPant, V.  
000007758 700__ $$aBerghmans, D.  
000007758 700__ $$aKumar, R. 
000007758 700__ $$aZhukov, A. N.  
000007758 700__ $$aVan Doorsselaere, T.  
000007758 700__ $$aPetrova, E. 
000007758 700__ $$aBanerjee, D.
000007758 700__ $$aLim, D. 
000007758 700__ $$aVerbeeck, C.
000007758 773__ $$n#66$$pSolar Orbiter Science Nuggets$$v30/07/2025$$y2025
000007758 8560_ $$fdavid.berghmans@ksb-orb.be
000007758 85642 $$ahttps://www.cosmos.esa.int/web/solar-orbiter/-/cross-scale-nature-of-decayless-waves-in-the-solar-corona
000007758 980__ $$aOUTRART