meddelelser nr · meddelelser nr.114 bjØrn e. l ytskjold topographer magnetic survey in svalbard...
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MEDDELELSER NR.114
BJØRN E. L YTSKJOLD Topographer
Magnetic Survey in Svalbard 1985 -1987
NORSK POLARINSTITUTT
OSLO 1991
Bjørn E. Lytskjold Norsk Polarinstitutt P.O.B. 158 N-1330 Oslo Lufthavn
ISBN 82- 90307- 88- 8 Printed Ma y 199 1
CONTENTS
1. lntroduction
2. Geomagnetism in general
3. Favourable conditions 4. The magnetic observatories in Svalbard 5. Instruments
5.1 The quartz horizontal-force magnetometer 5.2 The proton magnetometer
6. Field work 6.1 Selection of stations 6. 2 Marking of field stations 6.3 Positioning 6.4 Determination of azimuth
6.5 Magnetic observations
7. Data processing
7.1 Removal of diumal variation 7.2 Secular variation 7.3 Determining the components
8. Results 8.1 Presentation of ti.eld station measurements. 8.2 Geomagnetic contour charts 8.3 Correction table for secular variation
8.4 Valuation of the collected data
9. Suggestions for future works
10. Acknowledgements 11. References
Appendix 1: Map of magnetic stations 19 85-1987.
Page
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Appendix 2: List of field stations and matching geomagnetic components. Appendix 3: Correction tables for assumed secular variations. Appendix 4: Isoline map of geomagnetic declination for epoch 19 85.5.
Appendix 5: Isoline map of geomagnetic total intensity for epoch 19 85.5.
Appendix 6: Isoline map of geomagnetic horizontal component for epoch 1985.5.
Appendix 7: Isoline map of geomagnetic vertical component for epoch 1985.5.
1. INTRODUCTION
This report presents the result of a geomagnetic survey in Svalbard that took place during the summers of 1985, 1986 and 1987. The field survey was carried out by Norsk Polarinstitutt (NP) - the Norwegian Polar Research Institute - as parts of the Institute's annual Svalbard Expeditions. Topographer Sigurd Helle and the author were responsible for the field measurements in 1985 and topographer Knut Svendsen and the
author in 1986. The author finished the field work in 1987.
A magnetic map covering Svalbard was published in 1957 by Kaare Z. Lundquist, at that time hydrographer at NP. He collected available observations made in the area -the oldest made by Wtllem Barents in 1596 - and supplied it with own measurements from 1952 and 1953. With these observations he compiled a map that presented the magnetic declination in Svalbard for the epoch 1930 (NP, skrifter nr. 110). Systematic corrections for magnetic storms were not possible in his work. He corrected, however, all observations with a characteristic daily variation and a calculated secular variation. In 1957 and 1958 Lundquist continued the magnetic measurements to compile hetter isomagnetic maps. The purpose was to improve the mapping of the declination, which was highly needed when publishing sea charts and topographical maps.
Considering the inhomogenity of his material, a systematic survey was clearly needed.
The purposes for mapping the geomagnetic field were:
1. Determination of the declination for use on the main map series covering Svalbard.
2. Determination of the field intensity in Svalbard for scientific purposes.
It was decided to compile isoline maps of the geomagnetic components D, F, H and Z in the scale of 1: 1 200 000 to meet the purposes.
2. GEOMAGNETISM IN GENERAL
The earth's magnetic field has two intemal sources:
The earth's interior, in particular the core, being responsible for the major part of the field.
Magnetic minerals in the earth 's crust creating regional and local anomalies.
In addition there is one extemal source:
In the upper atmosphere and magnetosphere currents cause temporary disturbances in the field. A secondary effect of these currents is induced current
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in the ground. Thereby the observed effects of atmospheric currents also depend on the conductivity of the ground.
The geomagnetic field is described by these components:
F = The geomagnetic field's total intensity. H = The geomagnetic field's horizontal component. Z = The geomagnetic field's vertical component.
Measuring unit for F, H and Z is nT.
D = Geomagnetic declination, positive values represent easterly declination, negative values represent westerly declination.
I = Geomagnetic inclination.
Measuring unit for D and I is degree.
The field originating from the earth's interior is changing slowly and irregularly. Typical time scales are years and longer. This variation, called secular variation, reflects prosesses of the interior of the earth and is consequently a source of information of these. The aim of a magnetic survey is to map this field.
The anomalies due to the magnetic characteristics of the crust are of permanent nature, changing only in geological time scales. Such anomalies are of value to geologists.
The extemal field is basically of solar origin. The particles of the solar wind interact with the earth's magnetic field resulting in complicated current pattems in the upper athmosphere. The magnetic fields set up by these currents are of value to the science of the upper athmosphere. From a magnetic survey point of view, however, they are regarded as disturbances. The time scale ranges from fractions of a second to weeks. There are regular components in these disturbances e.g. daily variations due to solar heating of the athmosphere. The major parts, however, have the form of so called magnetic storms. These are global phenomena, but their apperance varles strongly with the latitude. Especially the polar regions have large and very irregular disturbances.
Deviations of several hundred nT in F and a few degrees for D are quite common. The average field for days not affected by magnetic storms is usually a good approximation to the intemal field. Such quiet days are scarce in the aurora! zone and the polar cap regions. Observations over at least several months are needed to obtain a quiet field value. In the polar regions we encounter the additional problem that the quiet field is contaminated by the interplanetary magnetic field. This is due to the fact that the field lines in the region are open into the interplanetary space. The sector structure of solar wind is in this way seen in the ground field as variations of several tens of nT (Friis-Christensen 1971, Albrigtsen et. al. 1981).
The intemal field is assumed to coincide with the mean field of quiet days. Point measurements made during a field survey will most of the time be affected by extemal disturbances. Theoretically a solution is to wait for magnetically quiet conditions, but such are unpleasantly infrequent in the Arctic. Therefore this method is hopeless from a practical point of view. Measurments have to be done whenever the surveyor visits a field station and all readings are treated as if they are affected by disturbances.
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Recorded data from a nearby running observatory will enable us to correct the readings and find the quiet mean values.
3. FAVOURABLECONDITIONS
To avoid severe magnetic storms, the field work bad to be done when solar wind was supposed to be at a minimum. 1985, 1986and 1987 were supposed to be good years. A diagram of the sun spot activity is shown in figure 1.
240
220 Smoothed observed sunspot numbers
200
180
160
140
120
100
80
60
40
20
Junc 1976 1978 1980 1982 1984 1986 1988
Fig. 1: Smoothed observed sunspot num.ber
4. THE MAGNETIC OBSERVATORIES IN SVALBARD
When the survey took place, two magnetic observatories were operating:
Bjørnøya (since 1952) at 74°30' N 19°02' E Ny-Ålesund (since 1966) at 78°55' N 11°57' E
Both are run by Nordlysobservatoriet (The Auroral Observatory, University of Tromsø).
1990
The Polish Academy of Science is operating an observatory in Hornsund (77°00'N 15°36'E). Data from this site would be very valuable for this survey. Unfortunately we were not able to obtain the relevant information.
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5. INSTRUMENTS
The surveyors mainly relied on instruments belonging to NP, in addition some were borrowed from Statens Kartverk (Norwegian Mapping Authority) and the University of Oslo. In all the parties disposed:
- 2 Andersen & Sørensen Quartz Horizontal-Force Magnetometers (QHM) - 2 Elsec 770 Proton Magnetometers - 2 Wild T2 Theodolites - 2 Clocks, GMT syncronized - 1 Wild GAKl Gyro Theodolite (available in 1985 and 1986)
5.1 The Quartz Horizontal-Force Magnetometers
The QHM is primarily intended for determination of the horizontal component H of the magnetic field, but also usable for determination of the declination D. Both instruments were calibrated before and after each season at Danish Meteorological Institute to check their constants. No significant changes were noted.
5.2 The Proton Magnetometers
The proton magnetometer measures the total magnetic field intensity F. It is a scalar measurement independent of the field vectors direction with a resolution of 1 nT.
6. FIELD WORK
The survey took place during three summer seasons:
1985:
From July 19 to August 28 two parties measured in 59 field stations. This cruise visited the eastem part of Svalbard, including places such as Hopen, the east coast of Spitsbergen, islands in Hinlopenstretet, Tusenøyane, Edgeøya, Barentsøya, Nordaustlandet, Kong Karls Land, Kvitøya and Sjuøyane. On the northem coast of Spitsbergen surveying was carried out on Mosselhalvøya, Gråhuken and Reinsdyrflya.
1986:
During this summer two field parties measured in 53 stations in Spitsbergen. From July 18 to August 21 one party based in Longyearbyen worked mainly in an area between 77°N and 79°N. From August 14 to 21 a party based in Ny-Ålesund worked mainly north of 79°N and west of Wijdefjorden.
1987:
One party worked on Spitsbergen from July 18 to August 22 visiting 20 stations. Most of these were new points while some were "trouble makers" from 1985 and 1986. The party was mainly stationed in Longyearbyen.
6.1 Selections of Stations
The selection of magnetic field stations followed these directions:
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- The network of stations should be as homogeneous as possible, characteristic distance between the stations set to 30-50 km.
- In cases stations used by K. Z. Lundquist could be identified, these were preferred.
- Geological maps were checked when new stations were selected to avoid regions with magnetic rock. In the field the area around a planned point was examined with a proton magnetometer. If no serious anomalies were found, the point could be used.
6.2 Mapping the Field Stations
All field stations were marked with aluminium bolts when situated on solid rock. The major part, however, was to be found in gravel deposits near the sea or on weathered rock, here 60-70 cm long aluminium tubes were forced in to the ground. In this way a permanent network enables remeasurments of the magnetic field in the future.
6.3 Positioning
When possible, the exact position of a station was determinded by topographical methods. Stations were normally marked on aerial photos and topographical maps.
6.4 Determination of Azimuth
In each field station the surveyor had to determine the direction to true north. During the survey two methods were used:
1. Determine the station's position and an azimuth by observations to triangulation points, using theodolite.
2. Determine the true north direction using gyro theodolite.
Alt. 1 was the methode mainly used, however it demands good weather conditions. This is a problem in Svalbard where fog and low cloud cover is a common obstacle during the summer. In addition, the triangulation network on Svalbard in general is sparse. This made solutions by triangulation impossible in some areas, especially in eastem and northem regions.
Alt. 2 was used for many of the measurements in east and north. Without the gyro many of the points would have been given up as no triangulation points could be seen. According to the gyro's users manual, the instrument is constructed for use below 70° latitude. Exceeding this the accuracy is supposed to decrease. In 1985 the gyro was used as far north as 80°15'. The oscillation around the true north axis bad a relatively low frequency, but the gyro still proved to be reliable. The accuracy was found to be sufficient for magnetic purpose, exceeding that of the QHM's telescope and circle reading devices.
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6.5 Magnetic Observations
It proved to be very difficult to avoid disturbances from the extemal field. The survey was canied out during what was supposed to be quiet periods, despite this nearly all measure- ments were affected more or less dramatically.
Special care bad to be taken when carrying out magnetic measurements, such as dressing to avoid magnetic disturbance, as well as keeping all other equipment at a distance.
The measurements were canied out in two sections:
1. QHM
In each station a QHM was mounted on a non-magnetic tripod. Observations were normally canied out to enable calculation of two values of the magnetic declination D and two values of the horizontal field component H. Points of time were noted together with the intemal temperature of the QHM.
If there was time for it, extra measurements were done.
Fig. 2: M easuring with QHM
The accuracy of the QHM used in field measurments in Svalbard are not supposed to exceed 1' due to the latitude. The instruments were very sensitive for wind and were difficult to use in humid weather, however, the QHMs proved to be very reliable.
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2. Proton Magnetometer
To detennine a good average value for the total field intensity readings were done minimum six times in each station, with half minute intervals. All points of time were noted. The magnetometers were easy to operate and highly reliable.
7. DATA PROCESSING
The purpuse was to compile isomagnetic maps of the four components D, F, H and Z.
All values should be calculated back to epoch 1985. 5 - that is for June 1985 - to coincide with The World Magnetic Survey standard. To do this all field measurements had to be corrected for diunal variations, in addition those from 1986 and 1987 also were corrected for secular variations.
7.1 Removal of Diumal Variation
Each field component had to be corrected for diurnal variations to detennine the actual quiet mean values at the stations. The corrections were stright forward. Field data were recorded with the point of time noted for all observations. Available data from the observatories were studied. Registrations from 1987 were stored directly in digital form while those from 1985 and 1986 were digitized from registration paper sheets. A computer programme gave the differences between actual field values at the noted points of time and corresponding quiet mean level were calculated. The differences were removed from the field observation to get the quiet mean value for the stations. In addition a three hours mean value was calculated around each observation moment.
nT
53950
15 GMT 16 17 18 19 20 2 1 22 23
UNSTABLE MAGNETIC CONDITIONS
Fig. 3: Diurnal variation o/Z at an observatory_ during unstable conditions.
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Experiences from similar projects in the Arctic show that such corrections are applicable within 100- 150 km from the observatory (Wilhjelm 197 1). Outside this range the spatial correlation decreases rapidly. In case of several observatories a linear interpolation is an acceptable procedure.
For stations within a range of 150 km from Ny-Ålesund the diurnal corrections were taken directly from the registered data there. South of 78° 45' N on Spitsbergen and Edgeøya - and on Hopen - corrections were applied averaging the three hours mean values from the Ny-Ålesund and Bjørnøya observatories. Outside these areas - like Kong Karls Land, Nordaustlandet and Kvitøya - corrections were not applied due to large uncertainties.
7 .2. Secular Varia ti on
The secular variation is the difference between the annual quiet mean values.
The field measurements were done during three seasons. Since all components should be given for epoch 1985. Five secular variations were applied all measurements from 1986 and 1987. Values from Ny-Ålesund were used north of 78 °45'N, south of this latitude average values for Ny-Ålesund and Bjørnøya were applied.
At Ny-Ålesund and Bjørnøya the annual quiet mean values for the three components D, H and Z are listed below:
OBSERVATORY YEAR D H z
NY-ÅLESUND: 1985 2°42' w 7496 nT 53800nT
1986 2°36' 7460 53780
1987 2°29' 7425 53770
BJØRNØYA: 1985 3°47' E 9155 nT 52890nT
1986 3°55' 9132 52890
1987 4°01' 9104 52890
From the quiet mean annual values the secular variations are found to be:
OBSERVATORY YEARS D H z
NY-ÅLESUND: 1985-86 6'E -36 nT -20 nT 1986-87 7' -35 -10
BJØRNØYA: 1985-86 8' E -23 nT OnT 1986-87 6' -28 0
7.3 Determining the Components
For a field station the final value of a component C is given as follows:
C = C(St,t) + �C
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6C = C(Ob,s) + [C(Ob,85) - C(Ob,t)]
c = final field station value, epoch 1985.5.
C(St,t) = value measured at the field station at time t.
6C = correction taken from the observatory
C(Ob,s) = secular variation found at the observatory.
C(Ob,85) = reference value for epoch 1985.5 calculated at the observatory.
C(Ob,t) = value measured at the observatory at the time the field measurement was done.
The observatories registrate the components D, H, Z and belonging corrections, while D, H and F were measured in the field. This meant that l:§) and� H could be found directly from the recorded data, while & was defined like & =&/sin I . Following this procedure the field component values were given as:
D = D(St,t) + l:§J
H
z
=
=
H(St,t) +NI cos I = H I ( F + &. )
H tanl
F = F(St,t) +&/sin I
8. RESULTS
8.1 Presentation of Field Station Measurements
Location of all field stations and the two observatories are showed on the map in appendix 1.
The field stations are listed in appendix 2. The list contains this information about each field station:
- Number and name - Measurement date - Position - The magnetic components D, F, H, Z and I - Name of observator
The listed values in appendix 2 are average values found in each station. F is the average of minimum six measurements, D and H were measured minimum two times.
8.2 Geomagnetic Contour Charts
The results of the ground magnetic survey in Svalbard are represented by isomagnetic maps for epoch 1985.5. Four separate maps at a scale of 1:2 000 000 were compiled for D, H, Z and F. For each map the component in question is represented by contour lines.
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The contour lines were drawn by hand simply by interpolating linearly between the field station values.
The declination map has contour lines with 30' intervals. The intensity maps have contour lines with 50 nT intervals.
To ease the reading relative highs are indicated by an arrow pointing up (i) and relative lows by an arrow pointing down (T). The isoline maps pertaining to the survey appear in appendix 4 - 7:
- Appendix 4 : Geomagnetic declination D, epoch 1985.5. - Appendix 5 : Geomagnetic field's total intensity F, epoch 1985.5. - Appendix 6 : Geomagnetic field's horizontal component H, epoch 1985.5. - Appendix 7 : Geomagnetic field's vertical component Z, epoch 1985.5.
8.3 Correction Table for Secular Variation
The stueture of the contour lines compiled for epoch 1985.5 is supposed to be representative for the actual magnetic field for the following 10-15 years.
To find an updated value for the magnetic components, the epoch 1985.5 values have to be corrected by the secular variation since June 1985. Tables of assumed secular variations for D, F ,H and Z are found in appendix 3.
8.4 Valuation of the Collected Data
The present survey yields the best maps of the magnetic field in Svalbard so far. However, a couple of weak points are evident:
* In certain areas the anomalies are so large that a more dense network is needed to resolve detailed structures.
It is evident bow to heal this weakness: More measurements in the actual areas.
* The reduction to quiet mean level is not properly carried out for measurements too · far from the geomagnetic observatories.
This problem was especially serious when operating around K vitøya, Kong Karls Land and Nordaustlandet in August 1985. All stations there are outside the 150 km limit set for applying diurnal corrections found in Ny-Ålesund. In addition to this the magnetic conditions were very unstable. When the field observations were carried out the registrator in Ny-Ålesund noted significant fluctuations.
This calls for more observatories. Hornsund is already there and should be used in a future supplement survey of southem Spitsbergen. In 1988 Nordlysobservatoriet established an observatory on Hopen. This station will improve surveys on Edgeøya and Tusenøyane and of course provide important data from Hopen itself. Still lacking is the coverage of the northeastem part of Svalbard. This may be sol ved by putting out automatic observatories during a field survey.
* In the most remote areas uncertainties were connected to the determination of azimuth due to few triangulation points or limitations of available instruments.
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To solve this the field stations should be connected to triangulation points by more complex topographical surveying or by bringing two GPS (Global Positioning System) satellite recievers which would give both position and azimuth. The gyro theodolite used was not made for high latitudes. The gyro oscillated with relatively big amplitudes and needed a long time to stabilize. Longer observation periods were preferable, however time was limited during the field survey.
9. SUGGESTIONS FOR FUTURE WORK
Future ground magnetic surveys should take in advantage the development of the D/i-theodolite. This is an unmagnetic theodolite with a fluxgate sensor mounted parallel to the optic axis that measure declination and inclination (Kring Lauridsen, 1985). For field work the theodolite is superior to the traditional QHM.
The main purpose for the 1985-87 survey was to obtain sufficient knowledge about the magnetic declination for use on the main topographic map series of Svalbard. While planning the survey it was obvious to combine this with measurements needed to determine all the geomagnetic components. However, if the aim is to compile a complete set of high quality maps of the geomagnetic field covering Svalbard an aeromagnetic survey is needed.
The structure of the earth's interior undergoes a constant, but slow and irregular change. As the field originates from this source remeasurments are needed to keep the isoline maps updated. Idealistically this should be done every 10-15 year.
10. ACKNOWLEDGEMENTS
The author wishes to thank the staff at The Aurora! Observatory, University of Tromsø - particulary Truls Lynne Hansen - for their considerable contribution to the manuscript. Norsk Hydro has also contributed with useful information.
11. REFERENCES
Wilhjem, J. 1971: Ground based geomagnetic measurements in Greenland. Danish
meteorological institute, geophysical papers R-15. Friis-Christiansen, E. 1971: The influence of the direction of the interplanetary magnetic
field on the morphology of geomagnetic variations at high magnetic latitude. Danish
meteorological institute, geophysical paper R-27. Albrigtsen, S., Berger, S. & Brekke A. 1981: Influence of the interplanetary magnetic field on the
earth's magnetic field observed at Ny-Ålesund. Geophysica Norvegica,32 pp 23-28 . •
Kring Lauridsen, E. 1985: Experiences with D/i-fluxgate magnetometer inclusive theory of the instrument and comparison with other methods. Danish meteorological institute, geophysical
papers R-71. Lundquist, K. Z. 1957: Magnetic observations in Svalbard 1596-1953. Norsk Polarinstitutt, skrifter
nr. 110.
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Appendix 1: Map ofmagnetic stations 1985-1987 _____..
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AF
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AH
nT AZ 85 86 87 88 89 90 91 92 93 94 95
YEAR
Appendix 3: Correction tablesfor assumed secular variations
APPENDIX 3
Appendix4: Appendix 5:
Appendix 6:
Appendix 7:
lsoline map of geomagnetic declination for epoch 1985.5
I soli ne map of geomagnetic total intensity for epoch 1985 .5
lsoline map of geomagnetic horizontal component for epoch 1985.5
lsoline map of geomagnetic vertical component for epoch 1985.5
// 9• I
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SCALE 1: 1 200 000
APPENDIX 4
I I I
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20 40 80 80
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GEOMAGNETIC DECLINATION 1985.5
Contour lines of the geomagnetic declination, 1985.5
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& A I
---
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I APPENDIX 5
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SCALE 1: 1 200 000
40 80
Contour interval 50 nT
LEG END:
80
Relative high A Relative low �
I -,1so--t- 8 1•-t-- 1a•
T I I I I I
.,,
.,. "
0 ..,
I I ':' � I \t �
\t " f
i o " I s
I---I r- J_ 18°
8J0tlNOY
19°
r t
.::...
:.,
r T r
T T T t \-� 1- \ 21° 24° � a1• 2 7 °
r -t- �
.....
0 0 0 I!'> I!'>
0 I.I) O> '<1' I.I)
�·�l:J • t r .-,.O . <
/)
S T O R. fJ 0 R O B A N K
-l i 1 L 21° 24°
GEOMAGNETIC TOTAL COMPONENT 1985.5
Contour lines of the total component of the
geomagnetic field, 1985.5
B
F
\ �, 30°
A
p
N
27'
R E N
E N
H A V
NORSK POLARINSTIT llTT OSLO 1991
33°
ao•
79°
78°
s -
i 7 7°
E
...
!
80.!,..
•. "
I I I I I I
I I I I 77'
I
I I I I I I I I I
I
I
f 1e·
9•
1()
-· .._,_ T 12° -r I
• �dl ' flØ'' � . � S.t.l'OlA R lt!S
SVALBARD
--
0
SCALE 1: 1 200 000
APPENDIX 6 N 0 It $ "' E
/_. I I
l ;."
20
8 A � I( E N
I I I
I I I
+ -I-I 1 5° AUST OREEN'MCH
SCALE 1: 1 200 000
•O
Contour interval 50 n T
LEG END:
"'""&>
80
Relative high "' Relative low "
-1s-o---I
>
L
100km
r 1-a1•--r 1a• -t -1 -
-:. 1-.,.
c "'
I I
' .:.
.:. ".
I \t ti
\t f l 0
-\' ,, " I I -/- I-1s•
I B'so
BJOR NØY
74° 30'
19°
T
J� �6 s 1 •• " ss0 " . " •
r � 24° a1•
T- I
l�
--+
� \ L 27° 30•
\
6650
St ,,o
5700 6750
B A
P E
27°
GEOMAGNETIC HORIZONTAL COMPONENT 1985.5
H
Contour lines of the horizontal component
of the geomagnetic field, 1985.5
33°
6400 6so34so
R E
N
E N
H A
NORSK POLARINSTITUTT OSLO 1991
.eo•
79°
I I I
!
"
re·--
I I I
I I -77• f-
I I I I I
76'
9 •
10
-� 12• I _ _._ 15�
I
SVALBARD SCALE 1: 1 200 000
APPENDIX 7
8 A ,l\J I( EN
,, S0Rl( A p p ...
I I 8 ANl(fN
I t I >
I -/--. t-' I
15 o AUST ORff"Wj CH
SCALE 1: 1 200 000
0 20 eo eo 100k.m
Contour interval 50 n T
LEG END: Relative high • Relative low •
f--81° -J-
I I I j I I \) �
) 0 '!-
� ·( ll <!- I I
t 1a•
r - 1a•
r--t I
'
-1.
24° a1• L fio
,-
S T O R f
t 24°
GEOMAGNETIC VERTICAL COMPONENT 1985.5
Contour lines of the vertical component of
the geomagnetic field, 1985.5
30°
\
B A
l
27'
z
R E
E N -
K E N
H A V
NORSK POLARINSTITUTI OSLO 199•
33°
79
78
s -
77'
E
\
