Abstract
| Original language | English |
|---|---|
| Pages (from-to) | 480-483 |
| Number of pages | 4 |
| Journal | Nature Physics |
| Volume | 14 |
| Issue number | 5 |
| Early online date | 05 Mar 2018 |
| DOIs | |
| Publication status | Published - 01 May 2018 |
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Alfvén wave dissipation in the solar chromosphere. / Grant, Samuel D.T.; Jess, David B.; Zaqarashvili, Teimuraz V.; Beck, Christian; Socas-Navarro, Hector; Aschwanden, Markus J.; Keys, Peter H.; Christian, Damian J.; Houston, Scott J.; Hewitt, Rebecca L.
In: Nature Physics, Vol. 14, No. 5, 01.05.2018, p. 480-483.Research output: Contribution to journal › Letter
TY - JOUR
T1 - Alfvén wave dissipation in the solar chromosphere
AU - Grant, Samuel D.T.
AU - Jess, David B.
AU - Zaqarashvili, Teimuraz V.
AU - Beck, Christian
AU - Socas-Navarro, Hector
AU - Aschwanden, Markus J.
AU - Keys, Peter H.
AU - Christian, Damian J.
AU - Houston, Scott J.
AU - Hewitt, Rebecca L.
PY - 2018/5/1
Y1 - 2018/5/1
N2 - Magnetohydrodynamic Alfvén waves have been a focus of laboratory plasma physics and astrophysics for over half a century. Their unique nature makes them ideal energy transporters, and while the solar atmosphere provides preferential conditions for their existence, direct detection has proved difficult as a result of their evolving and dynamic observational signatures. The viability of Alfvén waves as a heating mechanism relies upon the efficient dissipation and thermalization of the wave energy, with direct evidence remaining elusive until now. Here we provide the first observational evidence of Alfvén waves heating chromospheric plasma in a sunspot umbra through the formation of shock fronts. The magnetic field configuration of the shock environment, alongside the tangential velocity signatures, distinguish them from conventional umbral flashes. Observed local temperature enhancements of 5% are consistent with the dissipation of mode-converted Alfvén waves driven by upwardly propagating magneto-acoustic oscillations, providing an unprecedented insight into the behaviour of Alfvén waves in the solar atmosphere and beyond.
AB - Magnetohydrodynamic Alfvén waves have been a focus of laboratory plasma physics and astrophysics for over half a century. Their unique nature makes them ideal energy transporters, and while the solar atmosphere provides preferential conditions for their existence, direct detection has proved difficult as a result of their evolving and dynamic observational signatures. The viability of Alfvén waves as a heating mechanism relies upon the efficient dissipation and thermalization of the wave energy, with direct evidence remaining elusive until now. Here we provide the first observational evidence of Alfvén waves heating chromospheric plasma in a sunspot umbra through the formation of shock fronts. The magnetic field configuration of the shock environment, alongside the tangential velocity signatures, distinguish them from conventional umbral flashes. Observed local temperature enhancements of 5% are consistent with the dissipation of mode-converted Alfvén waves driven by upwardly propagating magneto-acoustic oscillations, providing an unprecedented insight into the behaviour of Alfvén waves in the solar atmosphere and beyond.
U2 - 10.1038/s41567-018-0058-3
DO - 10.1038/s41567-018-0058-3
M3 - Letter
VL - 14
SP - 480
EP - 483
JO - Nature Physics
JF - Nature Physics
SN - 1745-2473
IS - 5
ER -