Issue |
A&A
Volume 396, Number 1, December II 2002
|
|
---|---|---|
Page(s) | 255 - 267 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361:20021361 | |
Published online | 22 November 2002 |
Temporal variability in the Doppler-shift of solar transition region lines
1
Armagh Observatory, College Hill, Armagh, BT61 9DG, N. Ireland
2
Center for Space Environment Modeling, 1414 Space Research Building, The University of Michigan, Ann Arbor, MI 48109-2143, USA
3
Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy
4
Sect. of Astrophysics, Astronomy and Mechanics, Dept. of Physics, Univ. of Athens, Athens 15783, Greece e-mail: madj@star.arm.ac.uk; iroussev@umich.edu; lte@arcetri.astro.it
Corresponding author: J. G. Doyle, jgd@star.arm.ac.uk
Received:
19
December
2001
Accepted:
19
September
2002
High cadence datasets taken in C iii 977 Å, O
vi 1032 Å and Ne viii 720 Å were analysed
in an effort to establish the extent of the variability in the Doppler-shift of
typical mid-transition region lines. The shortest time-scale variability seems
to occur in the network boundary regions where the line-shift can vary by
7–8 km in less than 1 min. The internetwork region also shows
variability although this tends to be longer lived, ~2–3 min. The average
line-shift in C iii is a red-shift which ranges from ~2 km
to
~20 km
with an average value for all regions selected being around
10 km
in very good agreement with that derived by others. The red-shift
values indicate a clear difference between network and internetwork regions,
with the largest red-shift being present at the network boundary. For O vi,
this gives an average red-shift ranging from 5 to 10 km
. For Ne viii, there
is a 13 km
difference between internetwork and bright network plasma with the bright
network being more red-shifted. This could imply that the bright network regions are
dominated by spicule down-flow.
In the second part we present results from 2-dimensional (2D) dissipative
magnetohydrodynamic (MHD) simulations of the response of the
solar transition region to micro-scale energy depositions. A variety
of temperatures at which the energy deposition takes place as well as the amount
of energy deposited are examined. This work is a continuation of previous
related simulations where small-scale energy depositions were modelled in 1D
hydrodynamics. The observable consequences of such transient events are then computed
for three transition region lines, namely C iv 1548 Å,
O vi 1032 Å, and Ne viii 770 Å, under the consideration of
non-equilibrium ionization.
Key words: Sun: atmosphere / Sun: transition region / Sun: activity
© ESO, 2002
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