1 / 14

3 rd MagNetE Workshop on European Geomagnetic Repeat Station Survey

3 rd MagNetE Workshop on European Geomagnetic Repeat Station Survey. REPEAT STATION MEASUREMENTS IN AUSTRIA 2005 AND 2006. Josef Berger, Gerald Duma, Barbara Leichter Central Institute for Meteorology and Geodynamics Vienna, Austria. The repeat station network in Austria.

phila
Télécharger la présentation

3 rd MagNetE Workshop on European Geomagnetic Repeat Station Survey

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 3rd MagNetE Workshopon European Geomagnetic Repeat Station Survey REPEAT STATION MEASUREMENTS IN AUSTRIA 2005 AND 2006 Josef Berger, Gerald Duma, Barbara Leichter Central Institute for Meteorology and Geodynamics Vienna, Austria

  2. The repeat station network in Austria • 14 RS measured every year since 1999 • Since 2001 marked with limestones

  3. Measurement-/Processing- Practice • Measurement sets • 1995-2004: One set of 4-5 measurements • 2005: One set in the evening and in the morning • Quality control • Standard deviation SD of 4-5 results (1 set) • Removal of data: dev >> SD (D – 30“, I – 20“, H – 5nT)

  4. Standard deviation (in sec) – reduction THY 2003 2004 2005

  5. Standard deviation (nT) – reduction THY 2003 2004 2005

  6. Max. differences of e- and m- measurement sets • D:  30 sec • I:  20 sec • HZF:  5 nT •  much bigger than scatter in single e- or m-set

  7. Reduction to different observatories • Differences in D (min): WIK-BDV 2004

  8. Reduction to different observatories • Differences in F-values: WIK-FUR 2004

  9. 2005 - Reference Observatory THY

  10. 2006 - not reduced yet!

  11. The average secular variation in Austria 2000 - 2004 • Average of 5 observatories (without WIK) • Average of 14 repeat stations

  12. The average secular variation in Austria 2000 - 2004 • Average of 5 observatories • Average of 14 repeat stations

  13. Results • Practice of evening and morning measurements • SD of e-set and m-set measurements similar • SD of e+m-measurements bigger (2x) • SD depends on magnetic disturbances • Reduction to different observatories • Max. differences of station value: WIK-OBS D:  2 min I:  0.8 min H,Z,F:  10 nT (near SV) compare Newitt,Barton, Bitterly (1996): D:1min, I:0.5min HZF: 5nT on average • Differences change from year to year for same reference observatory (more or less abitrary) • On average: differences WIK-THY smaller • Stay with the same reference observatory ( for “final RS data“)

  14. To quote Newitt, Barton, Bitterly (1996) „A determination of the error in a repeat station observation is an important but often difficult exercise“ CH.6.3 We fully agree! Thank you for your attention !

More Related