Fast appearances and disappearances of weak intranetwork magnetic fields

Details Fast appearances and disappearances of weak intranetwork magnetic fields Fast appearances and disappearances of weak intranetwork magnetic fields

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990cha%26a..14..325s&link_type=abstract

Chinese Astronomy and Astrophysics, Volume 14, Issue 3, p. 325-337.

Astronomy and Astrophysics

Astrophysics

3

Solar Quiet Regions-Solar Magnetic Field-Solar Observations

Scientific paper

Under good seeing conditions (<2'), the high resolution magnetic field observation at Huairou Solar Observing Station'is capable of detecting the intranetwork field. An analysis of some magnetograms of 1988 September 5 shows: 1. That the observed weak intranetwork magnetic fields (WINF) with maximum flux B between 5 and 10 G are real structures. 2. That About 70% of the WINF became undetectable at +/- 5 G level after 3.4 min and about 30% can be seen again. 3. That the number of WINF seen decreased exponentially with time, from which we estimated an upper limit of about 3 min for the mean life of a WINF. 4. That a WINF is a collection of unresolved flux elements, with a flux between 2.0(+16) and 1.0(+18) mx. Our results are similar to those in the magnetograms of 1984 September 9 obtained by the Big Bear Solar Observatory.

Affiliated with

Also associated with

No associations

Rating

Fast appearances and disappearances of weak intranetwork magnetic fields does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Fast appearances and disappearances of weak intranetwork magnetic fields, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Fast appearances and disappearances of weak intranetwork magnetic fields will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1403748