Issue |
A&A
Volume 403, Number 2, May IV 2003
|
|
---|---|---|
Page(s) | 715 - 723 | |
Section | The Sun | |
DOI | https://doi.org/10.1051/0004-6361:20030387 | |
Published online | 06 May 2003 |
Photospheric flows measured with TRACE II. Network formation
1
Sterrekundig Instituut, Postbus 80 000, 3508 TA Utrecht, The Netherlands
2
Laboratoire d'Astrophysique de Toulouse, Observatoire Midi-Pyrénées, 14 Avenue E. Belin, 31400 Toulouse, France e-mail: roudier@bagn.obs-mip.fr
Corresponding author: J. M. Krijger, J.M.Krijger@astro.uu.nl
Received:
26
July
2002
Accepted:
7
March
2003
We analyse a 7 d (167 h) sequence of TRACE white-light
images with 1´´ angular resolution taken at 1 min cadence.
The TRACE resolution and the fast cadence
allows us to produce maps of the horizontal flow fields with high
angular (1´´) and temporal
resolution (5 min).
The field of view of
(≈
93 Mm
93 Mm) covers approximately an area of 10 to 30 supergranules. This area was followed during solar rotation.
Magnetic flux was artificially inserted into the successive flow maps
in the form of ephemeral regions
with positive and negative polarity.
The emergence rate of
2
1022 Mx h-1
with an average flux per region of about 1.1
1019 Mx
produces a good reproduction of the chromospheric network
as observed in images taken simultaneously at 1600 Å.
In addition, we show that the quiet network can be maintained only if field elements of both polarities are inserted into the flow fields.
Our analysis suggests that the network
is fully replenished on a time scale of a day and
the lifetimes of the magnetic elements are of a similar duration.
Key words: Sun: photosphere / Sun: chromosphere / Sun: granulation
© ESO, 2003
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