Nalazite se na CroRIS probnoj okolini. Ovdje evidentirani podaci neće biti pohranjeni u Informacijskom sustavu znanosti RH. Ako je ovo greška, CroRIS produkcijskoj okolini moguće je pristupi putem poveznice www.croris.hr
izvor podataka: crosbi

Formation of Coronal Large-Amplitude Waves and the Chromospheric Response (CROSBI ID 225605)

Prilog u časopisu | izvorni znanstveni rad | međunarodna recenzija

Vršnak, Bojan ; Žic, Tomislav ; Lulić, Slaven ; Temmer, Manuela ; Veronig, Astrid Formation of Coronal Large-Amplitude Waves and the Chromospheric Response // Solar physics, 291 (2016), 1; 88-115. doi: 10.1007/s11207-015-0822-9

Podaci o odgovornosti

Vršnak, Bojan ; Žic, Tomislav ; Lulić, Slaven ; Temmer, Manuela ; Veronig, Astrid

engleski

Formation of Coronal Large-Amplitude Waves and the Chromospheric Response

An in-depth analysis of numerical simulations is performed to obtain a deeper insight into the nature of various phenomena occurring in the solar atmosphere as a consequence of the eruption of unstable coronal structures. Although the simulations take into account only the most basic characteristics of a flux-rope eruption, the simulation analysis reveals important information on various eruption-related effects. It quantifies the relation between the eruption dynamics and the evolution of the large-amplitude coronal magnetohydrodynamic wave and the associated chromospheric downward-propagating perturbation. We show that the downward propagation of the chromospheric Moreton-wave disturbance can be approximated by a constant-amplitude switch-on shock that moves through a medium of rapidly decreasing Alfvén velocity. The presented analysis reveals the nature of secondary effects that are observed as coronal upflows, secondary shocks, various forms of wave-trains, delayed large- amplitude slow disturbances, transient coronal depletions, etc. We also show that the eruption can cause an observable Moreton wave and a secondary coronal front only if it is powerful enough and is preferably characterized by significant lateral expansion. In weaker eruptions, only the coronal and transition-region signatures of primary waves are expected to be observed. In powerful events, the primary wave moves at an Alfvén Mach number significantly larger than 1 and steepens into a shock that is due to the nonlinear evolution of the wavefront. After the eruption-driven phase, the perturbation evolves as a freely propagating simple wave, characterized by a significant deceleration, amplitude decrease, and wave-profile broadening. In weak events the coronal wave does not develop into a shock and propagates at a speed close to the ambient magnetosonic speed.

coronal mass ejections ; waves ; magnetohydrodynamic ; waves ; shock ; flares ; waves

nije evidentirano

nije evidentirano

nije evidentirano

nije evidentirano

nije evidentirano

nije evidentirano

Podaci o izdanju

291 (1)

2016.

88-115

objavljeno

0038-0938

10.1007/s11207-015-0822-9

Povezanost rada

Fizika

Poveznice
Indeksiranost