Modelling of solar explosive events in 2D environments. III. Observable consequences

Details Modelling of solar explosive events in 2D environments. III. Observable consequences Modelling of solar explosive events in 2D environments. III. Observable consequences

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...380..719r&link_type=abstract

Astronomy and Astrophysics, v.380, p.719-726 (2001)

Astronomy and Astrophysics

Astrophysics

23

Mhd, Sun: Atmosphere, Sun: Chromosphere, Sun: Uv Radiation, Sun: Magnetic Fields -\ Line: Profiles

Scientific paper

We examine the response via line synthesis of two representative transition region lines, namely C IV 1548.2 Å and O VI 1031.9 Å, in various physical environments representing the ``quiet'' Sun to magnetic reconnection events. Our calculations of ion populations allow for departures from equilibrium ionization (EI), which is critical in studies of transient events. Both lines reveal highly blue- and red-shifted Doppler components, and some of the results are examined in the context of solar explosive events. The observable consequences of magnetic reconnection are subtle in the various physical circumstances examined here and differ from one emission line to another, because of the difference in their formation temperatures.

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