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EISCATEUROPEAN INCOHERENT SCATTERSCIENTIFIC ASSOCIATIONANNUAL REPORT 2009

EISCAT Radar Systems
Location

Tromsø

Geographic coordinates69◦ 35’N
19◦ 14’E77◦ 30’N
66◦ 12’N

Geomagnetic inclination
Invariant latitude
Band
Frequency (MHz)Maximum bandwidth (MHz)Transmitter
Channels
Peak Power (MW)Average power (MW)
Pulse duration (ms)Phase coding
Minimum interpulse (ms)Receiver
System temperature (K)Digital processing
Antenna
Feed system
Gain (dBi)
Polarisation

KirunaSodankylä67◦ 52’N
67◦ 22’N20◦ 26’E26◦ 38’E76◦ 48’N76◦ 43’N64◦ 27’N
63◦ 34’N
VHF
UHF
UHF
UHF
224
931
931
931
3
8
8
8
1 klystron2 klystrons
8
8
8
8
1.6
2.0
0.20
0.25
0.001–2.0
0.001–2.0
binarybinarybinarybinary1.0
1.0
analoganaloganaloganalog
250–300
90–11050
50
14 bit ADC, 32 bit complex, autocorrelation functions, parallel channels
parabolic cylinder
120 m×40 m steerable
line feed
128 crossed dipoles
46
circularparabolic dish32 m steerable
Cassegrain

parabolic dish32 m steerable
Cassegrain

parabolic dish32 m steerable
Cassegrain

48.1
circular

48.1
any

48.1
any

Longyearbyen78◦ 09’N
16◦ 01’E82◦ 06’N75◦ 18’NUHF500
1016 klystrons
6
1.0
0.25
0.0005–2.0
binary0.1
analog
65–80
12 bit ADC, lag profiles
32 bit complex
Antenna 1
Antenna 2
parabolic dishparabolic dish32 m steerable
42 m fixed
Cassegrain
Cassegrain
42.5
circular

44.8
circular

EISCAT Heating Facility in TromsøFrequency range: 4.0–8.0 MHz, Maximum transmitter power: 12×0.1 MW, Antennas: Array 1 (5.5–8.0 MHz)
30 dBi, Array 2 (4.0–5.5 MHz) 24 dBi, Array 3 (5.5–8.0 MHz) 24dBi.
Additionally, a Dynasonde is operated at the heating facility.

Cover picture: Artist’s view of a future EISCAT_3D active site.

CAT SSICE

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EISCAT Scientific Association
2009

EISCAT, the European Incoherent Scatter Scientific Association, is established to conduct research on
the lower, middle and upper atmosphere and ionosphere using the incoherent scatter radar technique.
This technique is the most powerful ground-based tool for these research applications. EISCAT is also
being used as a coherent scatter radar for studying instabilities in the ionosphere, as well as for investigating the structure and dynamics of the middle atmosphere and as a diagnostic instrument inionospheric modification experiments with the heating facility.
There are eleven incoherent scatter radars in the world, and EISCAT operates three of the higheststandard facilities. The experimental sites of EISCAT are located in the Scandinavian sector, northof the Arctic Circle. They consist of two independent radar systems on the mainland, together witha further radar constructed on the island of Spitzbergen in the Svalbard archipelago — the EISCAT
Svalbard Radar — Scandinavia (see schematic and operating parameters on the inside of the front
cover).
The EISCAT UHF radar operates in the 931 MHz band with a peak transmitter power of 2.0 MW and
32 m, fully steerable parabolic dish antennas. The transmitter and one receiver are in Tromsø (Norway).
Receiving sites are also located near Kiruna (Sweden) and Sodankylä (Finland), allowing continuous
tri-static measurements to be made.
The monostatic VHF radar in Tromsø operates in the 224 MHz band with a peak transmitter powerof 1.6 MW and a 120 m × 40 m parabolic cylinder antenna, which is subdivided into four sectors. It
can be steered mechanically in the meridional plane from vertical to 60◦ north of the zenith; limited
east-west steering is also possible using alternative phasing cables.
The EISCAT Svalbard radar (ESR), located near Longyearbyen, operates in the 500 MHz band witha peak transmitter power of 1.0 MW, a fully steerable parabolic dish antenna of 32 m diameter, and afixed field aligned antenna of 42 m diameter. The high latitude location of this facility is particularly
aimed at studies of the cusp and polar cap region.
The basic data measured with the incoherent scatter radar technique are profiles of electron density,
electron and ion temperature, and ion velocity. Subsequent processing allows a wealth of further parameters, describing the ionosphere and neutral atmosphere, to be derived. A selection of well-designed
radar pulse schemes are available to adapt the data-taking routines to many particular phenomena,
occurring at altitudes between about 50 km and more than 2000 km. Depending on geophysical conditions, a best time resolution of less than one second and an altitude resolution of a few hundred meters
can be achieved.
Operations of 3–4000 hours each year are distributed equally between Common Programmes (CP)and Special Programmes (SP). At present, six well-defined Common Programmes are run regularly,
for between one and three days, typically about once per month, to provide a data base for long term
synoptic studies. A large number of Special Programmes, defined individually by Associate scientists,
are run to support national and international studies of both specific and global geophysical phenomena.
Further details of the EISCAT system and operation can be found in various EISCAT reports, including
illustrated brochures, which can be obtained from EISCAT Headquarters in Kiruna, Sweden.

The investments and operational costs of EISCAT are shared between:
China Research Institute of Radiowave Propagation, Peoples Republic of China
Deutsche Forschungsgemeinschaft, Germany
National Institute of Polar Research, Japan
Norges forskningsråd, Norway
Science and Technology Facilities Council, United Kingdom
Solar-Terrestrial Environment Laboratory, Nagoya University, Japan
Suomen Akatemia, Finland
Vetenskapsrådet, Sweden

4

Contents
The Council Chairperson’s section

7

Director’s pages

8

The EISCAT_3D Design Study

12

Scientific highlights 2009
Ionospheric studies . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
On the source of the polar wind in the polar topside ionosphere: First results from the
EISCAT Svalbard radar . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Characteristics of polar patches in the nightside ionosphere . . . . . . . . . . . . . . . . . .
The influence of ozone concentration on the lower ionosphere . . . . . . . . . . . . . . . .
Particle precipitation during NEIAL events: simultaneous ground based nighttime observations at Svalbard . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Omega band electrodynamics . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Characteristics of ion upflow and downflow observed with the European Incoherent
Scatter Svalbard radar . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Statistics of Joule heating, electric fields and conductances . . . . . . . . . . . . . . . . . .
Studies in the D-region . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
D-region electron density and effective recombination coefficients during twilight andsolar proton events . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Dynamics of the precipitation regions causing auroral radio absorption . . . . . . . . . . .
Auroral studies . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Small-scale auroras: Flickering and black auroras . . . . . . . . . . . . . . . . . . . . . . . .
Electric field enhancement in an auroral arc . . . . . . . . . . . . . . . . . . . . . . . . . . .
Relations between proton auroras, intense electric field and ionospheric electron density
depletion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Studies of the cusp . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Ion heating in high-speed flow channel within the duskside cell of the polar-cap ion
convection under large IMF-By condition . . . . . . . . . . . . . . . . . . . . . . . .
Cusp observations during a series of fast reversals of the interplanetary magnetic field . .
Moving meso-scale plasma precipitation in the cusp . . . . . . . . . . . . . . . . . . . . . .
Studies of polar mesosphere summer echoes . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Radio Physics of PMSE . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Frequency dependence of polar mesosphere summer echoes . . . . . . . . . . . . . . . . .
The layered dust plasma structure of PMSE . . . . . . . . . . . . . . . . . . . . . . . . . . .
Studies involving artificial ionospheric heating . . . . . . . . . . . . . . . . . . . . . . . . . . . .
HF heating campaigns by AARI . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Artificial modification of polar mesospheric winter echoes with the EISCAT Heater andthe role of charged dust particles . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Polar ionospheric heating . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
F-region electron heating by X-mode radiowaves . . . . . . . . . . . . . . . . . . . . . . . .
Ionospheric modification and plasma physics . . . . . . . . . . . . . . . . . . . . . . . . . .

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18
18
19
19
19
20
20
21
21
21
22
23
23
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23
24
24
27
28
28
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Studies of the thermosphere . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Temperature enhancements and vertical winds in the lower thermosphere associatedwith auroral heating during the Dynamics and Energetics of the Lower Thermosphere in Aurora (DELTA) campaign . . . . . . . . . . . . . . . . . . . . . . . . . .
Meso-scale thermospheric response . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Acceleration mechanism of high-speed neutral wind observed in the polar lower thermosphere . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
DELTA-2 campaign: Study of the energetics and the wind dynamics in the polar lower
thermosphere . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Studies of dust and meteorites . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Measurements of meteor smoke particles during the ECOMA-2006 campaign . . . . . . .
High statistics radar meteor studies at EISCAT . . . . . . . . . . . . . . . . . . . . . . . . .
Signatures of mesospheric particles in ionospheric data . . . . . . . . . . . . . . . . . . . .
Solar wind studies . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Interaction a between medium-scale transient in the solar wind and a stream interaction
region . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Theoretical studies of incoherent scattering spectra . . . . . . . . . . . . . . . . . . . . . . . . . .
20-moment approximation for ion velocity distribution and its application in calculationsof incoherent scatter spectra . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Incoherent scatter spectra of collisional plasma . . . . . . . . . . . . . . . . . . . . . . . . .

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List of publications 2009

37

EISCAT Operations 200940

Beynon medals

44

EISCAT organisational diagram 200945

Committee Membership and Senior Staff

46

Appendix: EISCAT Scientific Association Annual Report, 200949

The EISCAT Associates, December 200963

Contact Information

64

6

The Council Chairperson’s section
The transition from the traditional EISCAT activities to preparatory work for a new radar system — including major upgradings both in themainland radars and in Svalbard — was the mostimportant topic in the work of the EISCAT Council during 2009. The performance of the VHF radar
continued to be below optimal as only one of the
klystrons was in use. On the other hand, the plans
for renovation work were in fair wind. The EISCAT_3D concept was accepted to the ESFRI Road
Map at the end of 2008 and the EU-funded Design Study for the 3D concept ended successfullyin spring 2009. In addition, China made a very fascinating proposal to extend the ESR system with athird antenna dish.
The composition of the EISCAT Association andits management structures were discussed several times in the Council meetings. In particular,
the role of the EISCAT Management Committee(EMC) was reconsidered. The wish from the new
Director, Dr. Esa Turunen, was that this Committee would provide him a link towards the Council
not only during the Council meetings. The discussions in the Council and EMC finally led to a solution where EMC was renamed Council Advisory
Group (CAG) and its tasks in the Statutes were reformulated. CAG’s role is to advice the Council
on matters related to administrative issues, development of facilities and the Association, finances,
legal issues, planned operations and other items
relevant for the Council. Both the Director andthe Council chairperson participate in the CAG
work. The Council supporting roles of SOC (Scientific Oversight Committee) and CAG are different:
SOC can give its recommendations entirely fromthe basis of scientific argumentation while CAG’s
task is to evaluate SOC’s recommendations fromthe viewpoint of the available resources in the Association. For this reason it was recommended
that both SOC and CAG would arrange their gatherings before the Council meetings and in such atimeframe that CAG can take into account the SOC
output in its recommendations to the Council.
The criteria for full versus associate membership are under continuous discussion because dur-ing recent years some old member countries havedecided to leave EISCAT and new partners are
stepping in. The re-organization of UK science
funding structures in 2009 had an impact also to
the EISCAT management and economy situation
which further complicated the picture. In an additional Council meeting arranged as a telecom
at the end of 2009, the opportunities for the UK
to make some changes in its representatives andcommitments for the Association were discussed
extensively. The negotiations for Ukraine’s membership in EISCAT continued in 2009 and as a transition period solution EISCAT made a one-year
collaboration agreement with this country. Russia continued collaboration with the Association
by buying significant amount of observing time
and the links towards the Russian science community were strengthened by inviting a Russian representative to SOC. In the Council discussions it
was noted that the long-term commitments are essential for the core operations of the Associationand for this reason they can be considered as thecornerstone criterion for a full membership status.
On the other hand, joining EISCAT should be attractive and easy also for countries whose science
funding is organized in shorter cycles than the five
year cycle used in the EISCAT membership rules.
In this controversial situation it is still importantto guarantee fair and equal treatment for all members in the Association.
The practice where a staff representative participates in the Council meetings was tested during the year 2008. This practice ended in 2009
because the staff had expressed the opinion thatthe presence of their representative is needed only
when the Council needs the staff opinion to guideits solutions. The Council decided to accept thischange, but on the other hand it encouraged thestaff to continue the biennial selection of a staff
representative. The wish is to continue the dialogue between staff and the Council and the message from the Council Chairperson is that bothsides can serve as the initiator in this discussion.
Dr. Kirsti Kauristie
Chairperson of the EISCAT Council
7

Director’s pages
As in January 2009 I was handed over the responsibility of the daily management and operation of the facilities of the EISCAT Scientific Association, as the new Director, I felt strong confidence: first, on the continuing capacity of the Association being able to serve its users for their scientific needs in providing measurement opportunities at the modern ISR operational level, and second, in inspiring and motivating its user community to develop the ISR method towards a brandnew future. The future had been outlined during
the achievements in the soon to be finished EISCAT_3D Design Study. This confidence was not
only based on my earlier experience as a user ofthe EISCAT radars; having been the PI of many
Finnish radar campaigns through the years, I had
met devoted, committed and skilful staff at thesites. Similar feelings were passed to me while
meeting the enthusiasm and guidance given by
the various active EISCAT Committee members,
starting at the last year’s Council meeting in Kunming, China, throughout the year in the Science
Oversight and EISCAT Management Committee
meetings. Specially the previous director Tony van
Eyken, Prof. Asgeir Brekke and Dr. Kirsti Kauristie, the previous and new Council chairs respectively, stood by my side as immediate support, using a lot of their time when guiding me into how
the activities of the association are to be seen in international context.

for the future, is at place already. It would be
my task to ensure that this competence would not
be lost with possibly restricted financial resources
foreseen in the near future and that there would
be ways to find new resources, which could be directed towards the next renewal. The total number of EISCAT staff however had been cut during the recent years to a minimum, which would
not last too many unexpected losses. Even now
some part of preventive maintenance had to beabandoned, simply due to less manpower available. However, all technical problems appearing
at the sites during the year were solved with minimum delays, and the overall maintenance task appeared to be manageable at all the sites. As EISCAT is a distributed facility located in the territoryof three different countries, Sweden, Finland, Norway and Svalbard, the large distances set up somespecific demands in internal communication. We
decided to establish some new meetings, such as
twice a year a site leader meeting, where leading staff from Headquarters and from all the sites
would meet physically for one day discussions.
Naturally the internal site meetings were encouraged. These were regularly held at the sites but
were missing at the Headquarters and were introduced there. Also the EISCAT scientists decided tohave virtual meetings, testing a few times internetbased conference solutions. However, the conclusion of these tests was that with our various conBut the most significant strengthening of my nections and hardware set-ups, still at this phase a
confidence on the strengths of EISCAT appeared in standard teleconference by ordinary phones is thethe beginning of the year, when the EISCAT staff most reliable virtual meeting method.
gathered for its Annual Review meeting in PallasThe association is facing some changes, which
tunturi in Finland on 11–13 February. Staff reports should be seen as opportunities to renew signifiof the technical status of the various parts of our cantly within few years in future. Russia successdistributed facilities impressed me in dedication, fully conducted EISCAT experiments during theirdetail and honest evaluation. I was confirmed that affiliate agreement, where they essentially buy exEISCAT has its most important resource in the ex- periment time similar to what France is doing. The
isting staff, all doing their best at highest possi- Russian contribution is at an essential level finanble level of expertise and with experience gained cially and an agreement is written for three years.
through many, many years of operation and main- With Ukraine we had a minor level agreement,
tenance tasks. As EISCAT had gone through sev- which made the first purely Ukrainian EISCAT exeral successful upgrades during the history, the periments possible. This was a one year arrangecore competence to take similar renewal actions ment at this stage, but continuation is expected.
8

The long-standing EISCAT Associate Science andTechnology Facilities Council (STFC) in the UK informed EISCAT that by end of 2009, the UK associateship would be transferred to the National Environment Research Council (NERC). At this stageof the transfer, which includes some negotiations
within Council, an agreement with NERC is being signed to start as the UK associate from 2010.
We thank STFC for the extensive work during theyears, as generally known, the UK has led many
developments in EISCAT in the past. At the sametime we welcome NERC to continue the work andpossibly bring in new fields of their interests to the
EISCAT activities.
European Union has been funding access to EISCAT facilities in the TransNational Access program, which ended in 2009. The TNA program
did not reach its planned target, there were fewer
users than anticipated. As there is currently noforeseen similar funding appearing in Europe, one
could ask if there could be an EISCAT funded
TNA-type program available in the future? An option would be combine this somehow with the current third party proposals. In any case TNA has
succeeded in bringing new countries to the user
list of EISCAT. One should continue in creating
opportunities for these research groups who havelearnt to know EISCAT, in order to be able to create
an enlarging and collaborating EISCAT user community simply because the ISR method, data analysis and sophisticated combined use of ISR datawith other measurements, are concepts which willtake some time for any individual to master.

ing maintenance. It should be also noted here thatin addition to the Dynasonde in Tromsø, EISCAT
also has a Dynasonde in operation on Svalbard,
and all the Dynasonde data are available on the internet. At the remote sites Kiruna and Sodankylä,
we are still having three persons at each site, butthere is a reduction foreseen soon, as in 2010 wewill have one staff retirement at both sites. Refilling these positions is not anticipated since we
expect diminishing operations. The receiver frequency protections will end at both sites in 2010.
EISCAT continued some exceptional observations in 2009. Beyond standard ISR operations
one could mention the space debris detections after the Iridium-Cosmos satellite collision in spring2009. The Iridium cloud orbital plane passes aswell as the Cosmos cloud passes are clearly identifiable in data, which could be used to improvethe current statistical model. The Finnish EISCAT
user group introduced also the use of non-uniform
interpulse periods to receive echoes from all altitudes. In these experiments efficient space debris
and ISR measurements can be combined. Typical EISCAT measurements leave over 50% of theranges blank because the transmission and groundclutter always block echoes from the same ranges
for each transmission. Just now we are not foreseeing any more space debris measurements, unless European Space Agency is requesting related
operations.
EISCAT users are in the process of setting up
some extraordinary instrumentation at the radarsites: The Japanese lidar installation at the Tromsøsite includes three container houses. When in operation the lidar laboratory would be a major optical instrument to be used with EISCAT radars forOperations in 2009 were reduced as comparedto the previous year. This occurred naturally, sincein 2008 one still had the International Polar Year
operations running. The annual measurement
hours were 3688 in total. The Tromsø VHF radaris running with one klystron only. The repaired
one is kept as a reserve currently, since the EISCAT Site Leaders meeting in May 2009 estimateda 7 months break in operations to be the result if
the second klystron would be taken into use. The
Tromsø site has suffered from limited engineering
manpower, but this is now helped by hiring a newengineer Jan Børre Henriksen. The Tromsø scientist Dr. Lisa Baddeley left EISCAT in July 2009, inorder to work as the SPEAR scientist at UNIS. At
the heating upgrade in Tromsø, there are still issues to be solved, but the work is ongoing. Heating suffers from small amount of technical support
staff, which would be needed to help the responsible Senior Scientist. The Tromsø engineers are devoting part of their time in order to support Heat9

the next ten years. The interferometer at ESR site iscurrently under refurbishment and a new data acquisition is being installed. First operational data
is expected next year.
Year 2009 marked the successful finishing of
the 4-year long EU-funded Design Study of the
EISCAT_3D radar concept. In December 2008,
the European Strategy Forum on Research Infrastructures, ESFRI, had selected EISCAT_3D on
its Roadmap of strategically important infrastructures. As proposed facilities on this Roadmap
should be attractive for the global science community for the next 20–30 years, but located inEurope, EISCAT had gained a good science political starting point with the EISCAT_3D concept.
The proposal was submitted by Swedish ResearchCouncil as the initiator, and interestingly, EISCAT_3D was placed in the Environmental groupof RI projects. A similar ESFRI status was given at
the same time to a Norwegian proposal, The Svalbard Integrated Arctic Earth Observation System,
SIOS, where research activities from the bottom of
the sea up to the upper atmosphere and geospace,based on the existence of measurements and measurement sites in the Svalbard area, were proposed
to be strengthened and coordinated internationally as a concerted but interdisciplinary effort. The
EISCAT Svalbard radar would be an essential partof the upper atmospheric research programme of
SIOS. SIOS was in a very similar development
stage as the EISCAT_3D proposal, the next stepwould be to apply funds for a preparatory phaseaction with selected partner institutions. Such a
preparatory phase should solve all issues before
construction of the new research infrastructure: legal, governance, strategic, financial and, if necessary, technical work should be directed towards
making it possible to go to construction phase directly after the preparatory phase. As EU opened afinancing call to support preparatory phases of the
ESFRI Roadmap projects, EISCAT decided to hire
Dr. Ian McCrea from Rutherford Appleton Laboratory in part time, in order to coordinate writinga targeted funding application. A full time position of a project assistant was also established and
Dr. Anders Tjulin started to work at EISCAT Headquarters in Kiruna in September 2009. The finalising of a 6 Me funding application was conductedduring an intensive workshop with a small teamof international contributors, and the application
was sent to EU in December 2009.

Physics, Uppsala, in the premises of the Ångström
Laboratory. The purpose of the meeting was
twofold: first, to offer opportunity to EISCAT
users to show their plans and needs for measurements in their science fields, second, to publish
the results of the EISCAT_3D Design Study to
the wide user community. The results of the Design Study were formally handed over to EISCATin the meeting by the partner consortium representative, the technical coordinator of the study:
Dr. Gudmund Wannberg from Swedish Instituteof Space Physics in Kiruna. Final reports of theStudy were submitted to EU afterwards and thesereports are available to anyone via the EISCATand EISCAT_3D web pages. Dr. Wannbergs earlier work for the EISCAT radars in general aswell as the recent work for the EISCAT_3D Design Study were given a recognition in the 73rd
EISCAT Council meeting in Lillehammer on 27–
28 November 2009, when he was awarded withthe 7th Beynon medal.
In spring 2009 we restarted discussion with thefrequency authorities of all EISCAT Host Countries, Norway, Sweden and Finland. Our main discussion was of course in order to ensure future operations of EISCAT_3D, but also current facilities
were discussed, specially because timing the possible ending of current frequency licenses shouldmatch opportunity to use the new EISCAT_3D frequency. Norway is currently offering the 229.9–
236.6 MHz to EISCAT, as a response to the application sent out during the EISCAT_3D Design
Study. We have replied this to be fine for us, but
so far there is no confirmation from the authority. Finland shows support to protect the band in
Northern Finland for EISCAT, provided the location(s) of measurement site(s) are in areas where
this would be possible. Sweden has future allocation to DAB (digital audio broadcast) development, but there are several authorities involvedin making decisions. Swedish Research Council offers to coordinate discussions with these authorities. The frequency allocation of EISCAT_3D
should be solved as soon as possible, since this is
one of the prerequisites before the technical realisation of the new generation radar can be brought
forward.

A showcase of all the EISCAT science wasthe 14th EISCAT Workshop on 3–7 August 2009,
in Tromsø, Norway. The number of participants was this time slightly less than during preA dedicated first international EISCAT_3D User vious workshops, in total 85, but included a
Meeting was organised in Uppsala on 27–29 May very international mix of participants from all
2009, hosted by the Swedish Institute of Space over the world. Among more traditional ses10

sions such as, space weather and solar windmagnetosphere-ionosphere-atmosphere coupling,high-latitude ionospheric response, mesosphereand thermosphere, meteors and space debris,
ionospheric modification, and new techniques,also sessions on the future with EISCAT_3D and
use of the enhancing global ISR network were organised. During the latter, the workshop participants were introduced a new conceptual need infuture geosciences: a more system-oriented approach and holistic view of the whole geospace environment and Earth itself as a composite system,
where one finally needs a more global approachboth to measurements and modelling efforts. At
the EISCAT workshop in Tromsø, the user community of EISCAT had a discussion on how to develop further the access to EISCAT data archive.
Parallel to the standard MADRIGAL database use,
EISCAT had started in 2008 to introduce a new opportunity, based on dedicated extensive softwaredevelopment on a hardware platform consistingof six computers transferred to EISCAT Kiruna
site from Rutherford Appleton Laboratory. A software consultant had worked on this system for
5.5 months to March 2009, in order to create amore elegant data access system, with extensive
metadata searches to access raw data, re-analysisof data collected by these metadata searches etc.
As EISCAT itself did not allocate more resources
to the combined software/hardware platform development, the next step was agreed to be taken by
the user community, by applying and developing
the system to fulfil needs of their selected sciencecases. It remains to be seen if such an alternative
resource via user engagement is enough to bring
the system to be a standard user level tool.
The next EISCAT International Workshop in2011 will be held in China. China has made an
ambitious project proposal to EISCAT, as a possible in-kind contribution to EISCAT in the form ofa third antenna on Svalbard. Originally the EISCAT Svalbard radar was proposed optimally tohave three antennas. Finally one was built andonly later another one was added as the Japanesein-kind contribution. Initial technical descriptionof the proposed third antenna is now given by
the Chinese associate CRIRP. This is similar to the
50 m antenna of the Chang’e Moon project in Beijing, and indeed the idea proposed is to use theantenna for multiple purposes, including ISR andSpace Debris measurements and communication
with the Chinese Moon projects, using both a separate transmitter at S band and the existing ESR
transmitter at 500 MHz. The Science OversightCommittee of EISCAT, SOC, finalised a documenton the science case of the third antenna; SOC recommends this addition to ESR. Several delegations from China visited Tromsø and Longyearbyen in order to discuss and map the case of thethird antenna. Also initial discussions were madewith a consultant who could serve in casting the
project into an action, including possible feasibility study and communication with local authorities on construction and operation permissions.
The next phase would be to make a decision on
taking such initial steps towards the realisation of
the third antenna.
Another possible development on Svalbard appeared during the Svalbard Science Forum, whereinternational research institutes who are active in
Svalbard area, gathered to discuss on coordinative
actions. In fact EISCAT proposed to start collaborative work towards a similar effort as was done
during the last International Polar Year in 2007–2008, a coordinated continuous measurement period, at least one year long, during the next solar
maximum. This would be possibly around 2013.
Such an operation with ESR is a major undertaking, and demands extra funding. The IPY operations with EISCAT were done using extreme effort
by EISCAT staff, also helped by others. As learned
from that experience, dedicated extra engineering
staff would be needed to be hired at the required
level. Without funding coming outside of the EISCAT standard budget, the continuous solar maximum operation will not be possible.
Although some minor reduction in resources
available to EISCAT in the nearest future may happen, I still think the current view towards future ismuch enlightened. We have the EISCAT_3D concept, which is having a political backing in Europe,and is certainly also of global science interest. With
coordinated science-led development, both within
and beyond the EISCAT community, and appliedboth in Svalbard, where the SIOS ESFRI project
and the Chinese third antenna proposal may develop further the traditional strengths in orderto address new science, as well as on mainland,
where the Heater upgrade should bring in new
developments in small-scale physics, and novel
applications, such as planetary radar and spacedebris measurement capability, enhanced data access and finally the EISCAT_3D ESFRI project, allshould develop new techniques to add new science. With this view in mind, I would like to thankthe EISCAT staff for their excellent work in 2009.
Dr. Esa Turunen
Director, EISCAT Scientific Association

11

The EISCAT_3D Design Study
In 2009 the four-year EISCAT_3D Design Study
was completed. This project was supported by
the Sixth Framework Programme of the European Union and was running from 1 May 2005 to
30 April 2009.
The aims of the Design Study were essentially
twofold:• To study the feasibility of constructing a thirdgeneration incoherent scatter research radar,using cutting-edge technology throughout
and providing an order-of-magnitude improvement in temporal and spatial resolution
so that the existing, aging, EISCAT VHF and
UHF systems, could be replaced.

• Digital time-delay beam-forming.
• Multiple simultaneous beams from each receiving array.
• Adaptive polarisation matching and Faraday
rotation compensation.
• Digital arbitrary-waveform transmitter exciter system.
• Full interferometry and imaging capabilities.
• Amplitude-domain data recording at fullsampling rate.

During the four-year Design Study, all mission• To produce a detailed costed design for such critical technical concepts were modelled, investia system.
gated by simulations and in critical cases also by
full-scale tests, and found to be realisable. Array
The Design Study did not include a task tosizes, transmitter power levels and receiver noise
develop the science case; this was carried out
performance that would be required to reach theas a parallel activity by EISCAT’s Science Advidesired time and space resolutions have also beensory Committee (SAC), later renamed as the Sciestablished. Based on this work, the target sysence Oversight Committee (SOC) from 1 January
tem was proposed to have the following technical2007. Members of the Design Study maintained
characteristics:
close links with the science case development, andThe EISCAT_3D core should comprise a 120 m
many of the ideas from SAC fed into the preparadiameter
filled circular aperture array with abouttion of the EISCAT_3D Performance Specification
16,000elements(see Fig. 1), laid out on an equilatDocument (PSD).
eral triangular grid, and in addition a number (sixFollowing extensive consultation with the scito nine) of smaller outlier receive-only arrays. It
entific user community in 2004 and 2005, it was
would then provide
determined that only a multi-static phased arraysystem could reach or approach the performance• Half-power beamwidth of about 0.75◦ which
demanded by present users and expected from fuis comparable to that of the present EISCAT
ture users.
UHF.
Accordingly, the target system specified in the
EISCAT_3D Performance Specification Document• Power-aperture
product
exceeding(PSD) comprises a central active (transmit-receive)
100 GWm2 which is an order of magnisite (the “core”) and four receive-only sites, lotude greater than that of the present EISCAT
cated on two approximately 250 km long baselines
VHF.
oriented North-South and East-West, respectively.
• Grating-lobe free pattern out to 40◦ zenith anTo achieve the desired performance, the progle.
posed system design incorporates a number of innovative ground-breaking concepts such as• Graceful degradation in case of single-point• Direct-sampling receivers.
equipment failure.
12Figure 1: Artist’s view of the EISCAT_3D core site as proposed in the Design Study.

Each core array element shuold be made up
from a radiator, a dual 2×300 W linear RF power
amplifier, a high performance direct-digitising receiver and support electronics. The recommended
radiator is a crossed Yagi antenna with a minimum
directivity of about 7 dBi.
Two filled 8000 element receive-only arrays
should be installed on each baseline at distancesof about 110 and 250 km from the core, respectively. Their radiating elements will be three- or
four-element X Yagis, essentially identical to thoseused in the core. The Yagis would be directed towards the core field-of-view and elevated to 45◦ .
Outlier arrays for interferometry should also be installed at the receive-only sites.
Advanced digital beam-forming systems would
allow the generation of a large number of simultaneous beams from each array, thus eliminating thetime/space ambiguity plaguing all present incoherent scatter systems and realise the possibilities
for volumetric imaging of vector quantities for the
first time.
It was verified that a system meeting the performance requirements put forth in the EISCAT_3D
Performance Specification Document could bebuilt today, using existing technology, if cost were
not an issue. Advances in semiconductor technology, signal processing and data storage between
now and the time of placing a contract are expected to reduce component and subsystem costs
to the point where a full-size core would cost

about 60 Me and each receive-only site 20 Me. It
is recommended that the member institutions of
the EISCAT Scientific Association commit to funding and constructing such a radar system according to the results and guidelines given in the technical reports (EISCAT_3D Deliverables) within thenext five to seven years.
As designed, the system would be highly modular and would lend itself excellently to gradualexpansion if funding should only be forthcoming
in installments. In this case, it is recommended
that in a first phase a 5000 element, 70 m diameter core array and at least two 1500 element receiver sites should be constructed to replace themulti-static capabilities of the present UHF radar,which are going to be lost in 2010. This configuration would already exceed the performance ofthe current VHF system, providing a 1.3◦ halfpower beamwidth, a power-aperture product ofabout 10 GWm2 , and full beam steerability at thetransmitter site. There are also stages beyond theoutlined system involving multiple core elements
arrays that could then be expanded as additional
funding became available or as part of a morecomprehensive initial build.
The Design Study team notes with pleasure that,as a result of their efforts and the hard work of the
EISCAT executives, EISCAT_3D was added to theEuropean Strategy for Research Infrastructure (ESFRI) roadmap, at its last revision announced in December 2008.

13

Scientific highlights 2009
Ionospheric studies
On the source of the polar wind in thepolar topside ionosphere: First resultsfrom the EISCAT Svalbard radar
In this study, we present quantitative radar observations of both hydrogen ion (H+ ) and oxygenion (O+ ) upflow in the topside polar ionosphere(Fig. 2) using measurements that were recently
carried out with the EISCAT Svalbard Radar andthe Reimei satellite. H+ upflow was clearly observed equatorward of the cusp above 500 km
altitude. Within the cusp the H+ density wasvery low, and the upflow was dominated by O+ions, but on closed field lines the H+ became thelarger contributor to the upward flux above about
550 km. The total flux seemed to be conserved,
and so below 550 km altitude O+ (with a small upward velocity of ∼50 m/s) appeared to determine
the upward flux which was then maintained by
H+ in the topside ionosphere. We also found thatthe H+ density in the topside polar ionosphere
was several times higher than current predictionsof ionospheric models like IRI2001.
Y. Ogawa, et al., “On the source of the polar wind in
the polar topside ionosphere: First results from the EISCAT Svalbard radar”, Geophysical Research Letters 36,
L24103, doi:10.1029/2009GL041501, 2009.

Characteristics of polar patches in thenightside ionosphere
The characteristics of polar patches in the European nightside ionosphere have been investigated.
These patches are the remnants of ionosphericplasma originating on the dayside and drawn antisunward across the polar region into the nightsideauroral region.
A multi-instrument study using the ESR, theAberystwyth radio tomography experiment, andthe SuperDARN radars observed the modulationof patch separation during a magnetic substorm.
14

Figure 2: Height profiles equatorward of the cusp
of H+ , O+ , and total electron density (panel a), H+
and O+ upward velocities (panel b), and H+ andO+ upward number fluxes (panel c). In panel cthe thick dashed lines indicate constant flux extended in height from the observed peaks for a
dipole magnetic field.

During substorm expansion the patches were separated by some 5◦ latitude but this was reduced
to some 2◦ when activity had subsided. The different patch separations resulted from the expansion and contraction of the high-latitude plasma
convection pattern on the nightside in response to
the substorm activity. The patches of larger separation occurred in the anti-sunward cross-polar
flow as it entered the nightside sector from the polar region. Those of smaller separation were also
in anti-sunward flow, but close to the equatorward
edge of the convection pattern, in the slower, diverging flow of the Harang discontinuity. A patch
repetition time of some 10 to 30 min was estimateddepending on the phase of the substorm.
A second multi-instrument study investigated
the influence of the season on the patchto-background density ratio in the nightside
ionosphere around solar maximum (1999–2001).
Patch-to-background ratios of up to 9.4±2.9 wereobserved by the ESR between midwinter andequinox with values of up to 1.9±0.2 in summer. The patch-to-background ratios in summer
were less than two, so the enhancements could
not formally be called patches, nevertheless they
were identified as significant density enhancements within the antisunward cross-polar flow.
Modelling of the difference between winter andsummer patch-to-background ratios primarily at-tributed the variation to the chemical compositionof the atmosphere, which in summer both reduced
the electron densities of the plasma drawn into thepolar cap on the dayside and enhanced plasma
loss by recombination. A secondary factor was themaintenance of the background polar ionosphereby photo-ionisation in summer.
A. G. Wood, S. E. Pryse, and J. Moen, “Modulation ofnightside polar patches by substorm activity”, Annales
Geophysicae 27(10), 3923–3932, 2009.
A. G. Wood, and S. E. Pryse, “Seasonal influence onpolar cap patches in the high-latitude nightside ionosphere”, Journal of Geophysical Research, in press,
2010.

The influence of ozone concentration on
the lower ionosphere
A numerical model of D-region ion chemistry isused to study the influence of the ozone concentration in the mesosphere on ion-composition andelectron density during solar proton events (SPE).
We find a strong sensitivity in the lower part of
the D-region, where negative ions play a majorrole in the ionisation balance. We have chosen thestrong SPE on 29–30 October 2003 when very intense proton fluxes with a hard energetic spectrum
were observed. Deep penetration into the atmosphere by the proton fluxes and strong ionisation
allows us to use measurements of electron density, made by the EISCAT 224 MHz radar, starting from as low as 55 km. We compare the electron density profiles with model results to determine which ozone concentration profiles are themost appropriate for mesospheric altitudes under
SPE conditions (Fig. 3). We show that, during
daytime, an ozone profile corresponding to depletion by a factor of 2 compared to minimum model
concentrations for quiet conditions (Rodrigo et al.,1986), is needed to give model electron density
profiles consistent with observations. Simple incorporation of minor neutral constituent profiles(NO, O and O3 ) appropriate for SPE conditions
into ion-chemistry models will allow more accurate modeling of electron and ion densities during
such events, without the need to apply a complete
chemical model calculating all neutral species.
A. Osepian, S. Kirkwood, and P. Dalin (2009), “The influence of ozone concentration on the lower ionosphere— modelling and measurements during the 29-30 October 2003 solar proton event”, Annales Geophysicae
27(2), 577–589, 2009.

Figure 3: Comparison of time series of the measured values of cosmic noise absorption from the
IRIS riometer at Kilpisjärvi (black curves) with absorption calculated on the basis of experimental(EISCAT) Ne -profiles (red curves). The solid lines
are on 29 October 2003, the dashed lines are on
30 October 2003. Absorption is given for a frequency of 30 MHz.

Particle precipitation during NEIAL
events: simultaneous ground basednighttime observations at Svalbard
In this investigation it was discovered for the firsttime that Natural Enhanced Ion Acoustic Lines(NEIALs) may occur during night time at high latitudes over Svalbard. The geophysical settings indicate that the NEIAL events in this case study
are associated with the substorm expansion phaseon the nightside. We have also found that thegreen line may exceed the red line intensity during
NEIAL events, causing enhancement in the upshifted shoulder in the incoherent scatter spectra.
This shows that both soft and hard precipitation isessential for the generation of NEIALs; the harderprecipitation being important for the enhancementin the up-shifted ion-acoustic line. We also findthat the enhancement of the down-shifted shoulder is not strictly related to the previously foundthreshold of about 10 kR for the 630.0 nm line intensities. There seems to be a possible link between the NEIAL events and the 844.6 nm line
emission intensity which probably makes this line
a more suitable indicator of NEIAL activity than
the 630.0 nm emission line. Both the 630.0 nm

15Figure 4: The optical emissions arriving from thefield aligned direction coinciding with the radar
beam. NEIAL events are marked with black arrows (and a black diamond), while the notation a,b, c and d marks emission peaks during which no
NEIAL events were observed.

Figure 5: The NEIAL event with an enhanced rightshoulder at the time when the green emission line
exceeded the red line (the enclosed frame in Fig. 4).

and 844.6 nm are emitted by atomic oxygen (OI),
excited by low energy precipitation, but the latter results from a prompt emission, and shows abetter correlation with NEIALs on the short timescales involved which makes this line a good candidate as an optical signature of NEIALs. Figure 4
shows the optical emissions arriving from the fieldaligned direction coinciding with the radar beam.
NEIAL events are marked with black arrows (anda black diamond), while the notation a, b, c and dmarks emission peaks during which no NEIAL
events were observed. The enclosed frame illustrates a case when the green line intensity exceeds
the red line. Figure 5 shows the NEIAL event withan enhanced right shoulder at the time when thegreen emission line exceeded the red line.
J. Lunde, U. P. Løvhaug, and B. Gustavsson, “Particle precipitation during NEIAL events: simultaneous
ground based nighttime observations at Svalbard”, Annales Geophysicae 27(5), 2001–2010, 2009.

Omega band electrodynamics
The study by Vanhamäki et al. (2009) presents acase study of omega band electrodynamics. This
study evaluates the performance of the new regional variant of the traditional KRM-method developed by Vanhamäki and Amm (1997). The
regional approach uses equivalent current dataand conductance values as input and yields estimates of ionospheric electric field and currents
as outputs. The contribution from EISCAT comesvia conductance estimates: From auroral intensities and riometer data the Hall and Pedersen
16

conductances are derived with a semi-empiricalmodel whose development EISCAT observations
have supported (Senior et al., 2008). Vanhamäki
et al. (2009) show that the electric field maps deduced with the regional KRM method are in general consistent with CUTLASS electric field measurements. The spatial distribution of most intense Joule heating regions in the omega band
structure is also investigated and the heating isfound to be higher in the dark region than in theauroral tongue (Fig. 6). However, the two auroral tongues analysed in the study have differencesin this respect: the heating rates associated withthe first auroral tongue are larger than those of thesecond tongue and of the dark region between the
tongues. On the other hand, the first tongue occurred in connection with pseudo-breakup auroras, so its higher Joule heating rates are not surprising. The lesson to learn from this study is thatthe spatial distribution of Joule heating in omegabands cannot be deduced on the basis of optical
data alone.
A. Senior, M. J. Kosch, and F. Honary, “Comparisonof methods to determine auroral ionospheric conductances using ground-based optical and riometer data”,
Annales Geophysicae 26(12), 3831–3840, 2008.
H. Vanhamäki, and O. Amm, “A new method to estimate ionospheric electric fields and currents using datafrom a local ground magnetometer network”, Annales
Geophysicae 25(5), 1141–1156, 2007.
H. Vanhamäki, et al., “Electrodynamics of an omegaband as deduced from optical and magnetometer data”,
Annales Geophysicae 27(9), 3367–3385, 2009.

Figure 7: Dayside ion upflow occurrence and ion
flux plotted over solar wind (SW) parameters:(a, b) SW density and (c, d) SW velocity. In panels b and d the black lines indicate average fluxes
in upflow events, while gray lines indicate average
fluxes of all data (upflow, downflow, and no-flow
events).

cause the region where ion upflow occurs is enlarged owing to SW density and IMF By magnitude, but it does not move significantly in geomagnetic latitude. The occurrence frequency of
dayside ion upflow displays peaks versus the geomagnetic activity index (Kp ), SW velocity, andnegative IMF Bz component; that is, ion upflow
is less frequently seen at the highest values of
Figure 6: The Pedersen conductance, electric fieldthese parameters. Dayside ion downflow in the F(vector field and intensity), and Joule heating rate
region/topside ionosphere occurs only when thein the vicinity of an omega band structure. The auKp index and/or SW velocity are high or whenroral tongue is located in the region of enhanced
IMF Bz is largely negative. The results suggest
Pedersen conductances and only a part of the largethat the region of ion upflow not only becomesomega structure is visible.
larger but also moves equatorward with increasing Kp , SW velocity, and negative IMF Bz . The
Characteristics of ion upflow and down- ESR can so be poleward of the upflow region andobserve ions convecting poleward and returning
flow observed with the European Inco- ballistically downward.

herent Scatter Svalbard radar

In this study, we investigated how geomagnetic
activity, the solar wind (SW), and the interplanetary magnetic field (IMF) influence the occurrenceof the F-region/topside ionospheric ion upflow
and downflow. Occurrence of dayside ion upflow
observed with ESR at 75.2◦ magnetic latitude ishighly correlated with the SW density (Fig. 7), as
well as with the strength of the IMF By component. We suggest that this correlation exists be-

Y. Ogawa, et al., “Characteristics of ion upflow anddownflow observed with the European Incoherent Scatter Svalbard radar”, Journal of Geophysical Research
114, A05305, doi:10.1029/2008JA013817, 2009.

Statistics of Joule heating, electric fields
and conductances
Properties of the Joule heating rate, electric fields
and conductances in the high latitude ionosphere17Figure 8: Median curves of Pedersen conductance(top panel), total electric field (middle panel) and
Joule heating rate (bottom panel) for K ≥ 3.

Figure 9: Effective conductance as a function ofelectric field in the midnight sector for Kp < 3(blue) and Kp ≥ 3 (red).

are studied by Aikio and Selkälä (2009). The
results are based on a one-month measurement
made by the EISCAT incoherent scatter radar inTromsø (66.6 cgmlat) from 6 March to 6 April,
2006. The data are thus from the same season(close to vernal equinox) and from similar sunspot
conditions (about 1.5 years before the sunspot
minimum) providing an excellent set of data to
study the magnetic local time (MLT) and theKp magnetic activity index dependence of ionospheric parameters with high spatial and temporal
resolution.
The results indicate that the response of morning sector conductances and conductance ratios toincreased magnetic activity is stronger than thatof the evening sector. The co-location of Pedersen conductance maximum and electric field maximum in the morning sector produces the largest
Joule heating rates 00–05 MLT for K ≥ 3 (Fig. 8).
In the evening sector, a smaller maximum occurs
at 18 MLT, mainly due to an intense electric field.
Minimum Joule heating rates in the nightside arestatistically observed at 23 MLT, which is the location of the electric Harang discontinuity.
Fits for the Joule heating rate as a function ofelectric field magnitude, separately for four MLT
sectors and two activity levels (Kp < 3 and K ≥ 3)
are also performed. In addition to the squared
electric field, the fit includes a linear term to study
the possible anticorrelation or correlation between
electric field and conductance. In the midday sector, positive correlation is found, as well as in themorning sector, for the high activity case. In themidnight and evening sectors, anticorrelation between electric field and conductance is obtained,
18

i.e. intense electric fields are associated with low
conductances (Fig. 9). This is expected to occur inthe return current regions adjacent to auroral arcs
as a result of ionosphere-magnetosphere coupling.
In addition, a part of the anticorrelation may comefrom polarisation effects inside high-conductanceregions, e.g. auroral arcs. These observations emphasise the importance of small-scale electrodynamics, which is not included in most of the global
models of Joule heating rate.
A. T. Aikio, and A. Selkälä, “Statistical properties ofJoule heating rate, electric field and conductances athigh latitudes”, Annales Geophysicae 27(7), 2661—2673,
2009.

Studies in the D-region
D-region electron density and effective
recombination coefficients during twilight and solar proton events
Accurate measurements of electron density in thelower D-region (below 70 km altitude) are rarely
made. This applies both with regard to measurements by ground-based facilities and by sounding
rockets, and during both quiet conditions and conditions of energetic electron precipitation. Deep
penetration into the atmosphere of high-energy
solar proton fluxes (during solar proton events,SPE) produces extra ionisation in the whole Dregion, including the lower altitudes, which gives
favourable conditions for accurate measurements
using ground-based facilities. In this study weshow that electron densities measured with two
ground-based facilities at almost the same latitude
but slightly different longitudes, provide a valuable tool for validation of model computations.
The two techniques used are incoherent scatter ofradio waves (by the EISCAT 224 MHz radar inTromsø, Norway, 69.6◦ N, 19.3◦ E), and partial reflection of radio-waves (by the 2.8 MHz radar near
Murmansk, Russia, 69.0◦ N, 35.7◦ E). Both radars
give accurate electron density values during SPE,
from heights 57–60 km and upward with the EISCAT radar (Fig. 10) and between 55–70 km withthe partial reflection technique. Near noon, there
is little difference in the solar zenith angle between
the two locations and both methods give approximately the same values of electron density at the
Figure 10: Electron density profiles measured byoverlapping heights. During twilight, when the
EISCAT radar (red curve) and calculated for thedifference in solar zenith angles increases, elecSPE on 30 October 2003 at 09:00 UT for zenith antron density values diverge. When both radars aregle 86.7◦ (black curve) using different models of O,◦
in night conditions (solar zenith angle >99 ) elecO3 and NO profiles (black and red dashed curves).
tron densities at the overlapping altitudes again
become equal. We use the joint measurements tovalidate model computations of the ionospheric Auroral studies
parameters f + , λ, αeff and their variations duringsolar proton events. These parameters are imporFlickering andtant characteristics of the lower ionosphere struc- Small-scale auroras:
ture which cannot be determined by other meth- black auroras
ods.
A study of two flickering auroral events using
the ASK (Auroral Structure and Kinetics) multispectral imaging system in combination with the
A. Osepian, et al., “D-region electron density and ef- UHF radar has led to improved understanding offective recombination coefficients during twilight — the mechanism responsible for flickering aurora
experimental data and modelling during solar proton (Fig. 11). Several ‘chirps’ were identified within
events”, Annales Geophysicae 27(10), 3713–3724, 2009.
the events, in which the frequency of flickering ascended or descended over a short period of time(∼1–2 s). By observing different optical emission
lines it was found that the energy of precipitation is inversely proportional to the flickering freDynamics of the precipitation regions quency over the duration of each chirp. This iscausing auroral radio absorption
predicted by the theory that flickering aurora isa result of the Landau damping interaction beThe analysis of D-region observations by the VHF tween electrons and electromagnetic ion cyclotron
radar in March 2008 investigated the dynamics (EMIC) waves, and that the wave speed is the priof the precipitation regions causing auroral radio mary factor determining the electron energy gain.
The ASK imager has also been used in conjuncabsorption. The motions were monitored by theimaging riometer at Kilpisjärvi. From the EIS- tion with the UHF radar to study the dynamics
CAT data the height of the absorbing layer was and energy characteristics of so-called ‘black audetermined, and hence the energy of the pre- rora’. The flux reduction of high energy participitating electrons causing the absorption. The cles versus low energy particles in the black regradient-curvature drift of electrons of these ener- gions compared to the diffuse background havegies would be much greater than the speeds ob- been investigated for different forms of black auserved. Magnetospheric circulation, as inferred rora. Two separate mechanisms have been sugfrom SuperDARN, is a more promising mecha- gested to cause black aurora. The larger reductionof high energy precipitation within the fine scalenism, though as yet unproven.
19Figure 11: UHF radar high resolution data. The
flickering aurora occurred between 18:16:30 and
18:17:30 UT and corresponds to higher energy particle precipitation causing ionisation to lower altitudes.

black structures favours a magnetospheric mechanism that blocks high energy electrons from being
scattered into the loss cone.
D. K. Whiter, et al., “Using multi-spectral optical observations to discriminate between possible acceleration
mechanisms for flickering aurora”, Journal of Geophysical Research, submitted, 2010.
J. Archer, et al., “Dynamics and characteristics of black
aurora as observed by high resolution ground-based imagers and radar”, International Journal of Remote Sensing, submitted, 2010.

Electric field enhancement in an auroralarc
The character of a change in the ionospheric electric field when several auroral arcs crossed the region of radar measurements has been analysed(Fig. 12). In one case the plasma conductivity
and electric field normal component in an arc
increased as compared to their undisturbed values. In another case the field and conductivity
changed traditionally (in antiphase). Arcs with anincreased field were previously classified as correlating arcs, but their existence was subsequently
open to question during optical observations. The
usage of the ALIS system of digital cameras madeit possible to decrease the errors introduced by optical equipment. The measurements in the vicinity of correlating arcs were performed when thesearcs were generated, and a traditional arc was acompleted formation. In an originating arc, thefield value can depend not only on the ionosphericplasma conductivity but also on the processes in
the magnetospheric-ionospheric system resulting
in the field enhancement.
V. V. Safargaleev, et al., “Electric field enhancement in
an auroral arc according to the simultaneous radar (EIS-

20

Figure 12: Optical and radar measurements in thevicinity of the correlating arc.

CAT) and optical (ALIS) observations”, Geomagnetism
and Aeronomy 49(3), 353–367, 2009.

Relations between proton auroras, intense electric field and ionospheric electron density depletion
A case study with simultaneous European Incoherent Scatter and optical auroral observations
was conducted in order to determine characteristics of the magnetosphere-ionosphere couplingfrom the viewpoint of the electrodynamics in theionosphere. Particular focus was on the relationships between ionospheric electron density depletion, perpendicular electric fields, and proton auroras. Intense electron density depletion was observed in the E and F regions poleward and in thevicinity of a thin equatorward moving arc (Fig. 13).
This depletion was associated with an intense,
equatorward perpendicular electric field close to∼80 mV/m and most likely with a downward
field-aligned current (FAC), but it did not accompany detectable proton aurora. Hence the down-

FUJII ET AL.: ELECTRODYNAMICS IN THE IONOSPHERE

A09304

A09304

ward FA electric field in the lower magnetosphereassociated with this depletion was weak or absent.
The motion of the FAC system with the depletionand the arc presumably enabled the downward
FAC to obtain enough current carriers as ionospheric electrons were lost by the evacuation process. The evacuation process associated with the
downward FAC was, however, efficient enoughto establish the depletion. On the other hand, awidely distributed proton aurora observed immediately after the depletion was associated with anintense, equatorward perpendicular electric fieldclose to 90 mV/m, enhanced electron density, andmost likely a downward FAC. No electron precipitation was associated with this proton aurora.
Thus the electron density enhancement, providing
the downward current carriers, had to be causedby the ionization of precipitating protons presumably accelerated by downward field-aligned electric fields in the lower magnetosphere.
Figure 1. A summary plot of the time variations of several parameters between 2020 and 2220 UT on
emissionsfrom time
the proton
aurora imager,of(b) electron
20 OctoberFigure
2006. From13:
the top
to bottom, (a) Hbplot
A summaryof thevariations
auroral emissions at 427.8 and 557.7 nm from the photometer, (c) the height profile of the electron
severalparameters
between
2020
and
2220
UT
on
density along the magnetic field line, (d) the ion, and (e) electron temperatures from European Incoherent
R. Fujii, et al., “Relations between proton auroras, inScatter. The event for the present study is an event around 2130 UT.

20 October 2006. From the top to bottom, (a) Hβtense electric field and ionospheric electron density deemissions from the proton aurora imager, (b) elecpletion”, Journal of Geophysical Research 114, A09304,
site (69.6°N, 19.2°E, 66.1° invariant latitude). The EISCAT image was obtained by using a star fit, assuming 120 km
tronfrom
auroralemissions427.8forand
557.7 nmfromdata used were obtained
an experimentin the Com-at altitude
the emissions.
The fourwavelength photometer
doi:10.1029/2009JA014319, 2009.
mon Programme One mode [Collis, 1995] where the had a field of view of 1.2°, which was comparable to thethe photometer, (c) the height profile of the electransmitter beam is emitted along the magnetic field line width of the EISCAT UHF radar beam. The photometer isof force. The half-powerbeamwidth of thealong
UHF radarbeammagnetic
coaligned to field
the radarline,
beam. (d) thetron
densitythewas 0.6°. The physical parameters directly measured wereand (e)electrontemperatures
fromandtheResults
EISCATthe electron density,ion
electron/ion
temperatures
and theline 4. Observationof sight ion drift velocity. The integration time of theradar. The interest for the present
an event[12] Figurestudy
1 shows aissummary
plot of the time variations
EISCAT data was selected to get enough S/N ratio; 60 s
in the present case. The
uncertainties
of theelectron density of several parameters between 2020 and 2220 UT on
around2130
UT.
20 October 2006 from top to bottom. Figure 1a shows H

Studies of the cusp

and electron/ion temperature were about 10% and 14%,b

emissions from the proton aurora imager, Figure 1b shows

respectively.
Ion heating in high-speed flow channel[ ] The proton aurora imager consisted of a digital CCD electron auroral emissions at 427.8 and 557.7 nm from thecamera and a fisheye lens with an H interference filter with photometer, Figure 1c shows altitude profile of the electron
along the hadmagnetic
field line, Figure
within the duskside cell of the polar-cap
a central wavelength
at 485.7 nm anda full widthhalf densitygases
depressed
wheretheatneutral
alreadyre- 1d shows ion,maximum of 2 nm. The image data were recorded every and Figure 1e electron temperatures measured with the
EISCAT
radar.
spondedtothehigh-speed
ions.
The
increase
in
60
s
with
50
s
integration
time.
The
panchromatic
digitalion convection under large IMF-By con[ ] One of the enhancements of the H emissions is seencamera to monitor electron auroras was equipped with atheion
temperature
atparticulargeomagnetic
latbetween
2025
and
2120
UT
(with
two
peaks)
and anotherfisheye lens and the image data were taken every 30 s withditionan exposure time of 15 s. The location of each pixel of the one is seen between 2125 and 2142 UT in Figure 1a. The
11

b

13

F region strong sunward ion flow embedded in theduskside cell of expanding polar cap ion convection and coincidental increase in the ion temperature were observed using the European Incoherent Scatter (EISCAT) radars at Tromsø, Sodankylä
and Longyearbyen together with the CUTLASS
HF radars. The convection map obtained by theSuperDARN HF radars showed that the highspeed flow channel elongated in 14–17 MLT was
moving equatorward. The increase of the measured ion temperature at the common scattering
volume of the EISCAT radars was in good agreement with the ion frictional heating estimated under the assumption of the null neutral wind velocity for about 20 min, and then it became much
lower than the estimate of the ion frictional heating. While the flow channel moved equatorward,
the ion temperature increase became less evident
at higher part of latitudes within the flow channel, which means that ion frictional heating wasbitude continued until the neutral wind was accel3 of 12
erated to the equivalentlevel of the surrounded
ion flow (Fig. 14).

S. Maeda, et al., “Ion heating in high-speed flow channel
within the duskside cell of the polar-cap ion convection
under large IMF-By condition”, Journal of GeophysicalResearch 114, A11307, doi:10.1029/2009JA014300, 2009.

Cusp observations during a series of fast
reversals of the interplanetary magnetic
field
A comparative study of the cusp was performed,
focusing on an interval in which the IMF Bz
component underwent four reversals, remaining
for around 30 minutes in each orientation. The
Cluster spacecraft were on an outbound trajectorythrough the northern hemisphere magnetosphere,
whilst the VHF and ESR were operating. The series of IMF reversals resulted in a sequence of pole-21

Figure 14: Plots of the line-of-sight ion velocity (left) and temperature (right) as a function of geomagnetic
latitude and UT. The TRO data in the latitudes lower than the common scattering volume (70.5◦ –71.0◦ ) is
combined with the ESR data in the latitudes higher than the volume. The positive value of the ion velocity
represents velocity away from the Tromsø radar and towards the ESR. The enhancements of the line-of-sightion velocity and temperature appeared in the highest latitudes at 13:30 UT and propagated to the lower
latitudes. The increase of the line-of-sight ion temperature at particular geomagnetic latitude started almost
simultaneously with the enhancements of the line-of-sight ion velocity. It continued for about 20 min andthen ceased before the end of the ion velocity enhancement.

4 min. At this time, the ground-based magnetometers of the IMAGE chain in Svalbard, located westward of LENA’s FOV, began to indicate perturbations. These perturbations immediately reached apeak and then ceased; the perturbations lasted 2–
3 min. During this interval, there was an enhanced
westward flow over Svalbard, as observed by theSuperDARN radars. The EISCAT Svalbard radar
detected an enhancement of electron density andtemperature that was concurrent with this flowenhancement, suggesting that a plasma precipitation burst accompanied with the flow. These observations, which cover a longitudinally extending region of the cusp, strongly suggest the existence of moving mesoscale plasma precipitation
H. T. Cai, et al., “Cusp observations during a series(MMPP). The MMPP travels westward with a lonof fast IMF Bz reversals”, Annales Geophysicae 27(7),gitudinally elongated form. Its leading and trail2721–2737, 2009.
ing edges should be created by the temporal effectof the cusp. The other edges, which lie along theMoving meso-scale plasma precipitation streamline, would originate in a spatially limited
region along the open-closed line. The boundary
in the cuspof the MMPP form is delineated by both the temOn 28 March 2001, when the interplanetary mag- poral and spatial structures of the cusp.
netic field was strongly duskward, the DMSP F12
spacecraft observed an ion precipitation burst ina latitudinally narrow region near 1200 MLT. A
few minutes earlier, the Low Energy Neutral Atom
(LENA) imager on the IMAGE spacecraft, whose
field of view (FOV) looks into the high-altitude
cusp, detected an enhancement of energetic neutral atom signals, which are produced by the ion S. Taguchi, et al., “Moving meso-scale plasma precipitainjection. The LENA data suggest that the ion in- tion in the cusp”, Journal of Geophysical Research 114,
jection moved out of its FOV after approximately A06211, doi:10.1029/2009JA014128, 2009.

ward and equatorward motions of the cusp. Consequently Cluster crossed the high-altitude cusp
twice before finally exiting the dayside magnetopause, both times under conditions of northward IMF Bz . The first magnetospheric cusp encounter, by all four Cluster spacecraft, showed reverse ion dispersion typical of lobe reconnection.
Subsequently, Cluster spacecraft 1 and 3 crossed
the cusp for a second time. During this second
cusp crossing, these two spacecraft were likely tohave been on newly closed field lines, which werefirst reconnected (opened) at low latitudes andlater reconnected again (re-closed) poleward of thenorthern cusp.

22

Studies of polar mesosphere sum- occurrence of PMSE. From the experimentallyderived volume reflectivity ratios together with
mer echoesmodelled volume reflectivity profiles for turbulent
Radio Physics of PMSE
Using the small scale structure of electron density caused by charged dust particles, the following relation between the volume reflectivity andfrequency occurring Polar Mesosphere Summer
Echoes (PMSE) was obtained−1η = R2 Θ−2
=
1/2 L



∆Ne re c2
2πf 2

2

e−

π 2 ln 2
2

−1
Θ−2
,
1/2 L

where ∆Ne denotes the absolute step of electron
density, re the classical electron radius, Θ1/2 oneway half-power half width, c the speed of lightand L the radar pulse width. Meanwhile, the statistical result−5

η = 3.8 × 10

×f

−4.37

scatter can be revealed that PMSE is indeed created by turbulent scatter in the presence of large
Schmidt number (Li et al., 2009a). Further investigations have been conducted and result in particle size distributions inside the PMSE layers which
has been recently published by Li et al. (2010).
Q. Li, et al., “Frequency dependence of PMSE: Resultsfrom simultaneous and common volume measurementswith EISCAT radars”, in Proceedings containing extended abstracts of twelfth workshop on technical andscientific aspects of MST radar, edited by W. Hocking,London, ON Canada, May 17–23, 2009a.

Q. Li, et al., “Microphysical parameters of mesospheric
ice clouds derived from calibrated PMSE observations
at 53.5 MHz and 500 MHz”, in The 9th international
workshop on Layered Phenomena in the Mesopause Region, Stockholm, Sweden, July 12–15, 2009b.

was obtained.
Also, by analysing the data obtained from ECT02, one can find that the dusty plasma in polarsummer mesopause is weakly ionised and weakly
coupling. The stronger disturbance of the electron Q. Li, et al., “Microphysical parameters of mesosphericdensity corresponds to the stronger radar echoes. ice clouds derived from calibrated observations of polar mesosphere summer echoes at Bragg wavelengthsof 2.8 m and 30 cm”, J. Geophys. Res. 115, D00I13,
doi:10.1029/2009JD012271, 2010.

H. Li, et al., “One analysis on the rocket detection ofpolar mesosphere summer echoes”, Chinese Journal ofSpace Science 29(4), 397–401, 2009.
H. Li, et al., “Study on the relation between the reflectivity and frequency in dusty plasma of polar summer
mesopause”, Plasma Science and Technology 11(3), 279–
282, 2009.

The layered dust plasma structure of
PMSE
The rocket experimental data indicated that theFrequency dependence of polar meso- layered dusty plasma structure has a sharp boundary in the summer polar mesopause. In order tosphere summer echoes
The frequency dependence of polar mesospheresummer echoes (PMSE) has been observed using simultaneous and common volume measurements.
Detailed observations using the EISCAT Svalbard radar (ESR, 500 MHz) and the
SOUSY Svalbard radar (SSR, 53.5 MHz) locatednear Longyearbyen on Svalbard (78◦ N, 16◦ E)
were presented by Li et al. (2009a,b). The campaign was conducted during the polar summer
in 2006 and the backscattered signal of the radars
were converted to absolute volume reflectivities(radar cross-section per unit volume) which is asystem-independent parameter. Figure 15 shows
the measured volume reflectivities obtained from
ESR/SSR measurements during periods of the

combine with the experimental results, traditionalhydrodynamic equations and charging equationis adopted to build physical models of the dusty
plasma to study the physics process about the
sharp boundary in the stratified structure. The
theoretical analysis and numerical results showthat a charged dust cloud immersed in a plasma
under the action of electric field and other force,
could develop a long-time and steady structures,
which can be used to explain the experimental observations, as is shown in Fig. 16.
H. Li, et al., “Study on the sharp boundary of layered
dust structure in the summer polar mesopause”, Chinese Journal of Polar Research 21(4), 272–278, 2009.

23

Figure 15: Height-Time-Intensity plots of the radar echoes observed with the ESR at 500 MHz (upper panels)
and SSR at 53.5 MHz (lower panels) on 18 June (left column) and 20 June 2006 (right column), respectively.
White vertical lines in the upper panels indicate times where meteor echoes were removed.

campaigns were supported by the Finland and Iceland CUTLASS HF radars. A number of important new results were obtained from these heating
campaigns in 2009.

Figure 16: The charged ice particle number density
distribution profiles.

Studies involving artificial ionospheric heating
HF heating campaigns by AARI
Two extensive HF heating campaigns were held
by Arctic and Antarctic Research Institute in 2009.
Russian EISCAT/Heating campaigns were carriedout from 3 to 12 March and from 29 October to
6 November 2009. The experiments were carriedout in the day and early evening hours in a deep
minimum of solar activity under quiet magnetic
conditions. Many hours of excellent data were obtained from the EISCAT monostatic UHF radar,the spectrum analyzer for monitoring the SEE frequency spectrum at Tromsø, and the bi-static HF
radio scatter at St. Petersburg. Importantly both
24

HF pump-induced phenomena near the third
electron gyro harmonic frequency, 3fce , using thefrequency stepping the HF heater frequency, wereanalysed in detail for a few days of March 2009.
As an example, Fig. 17 illustrates the behaviourof the electron temperature Te and the backscattered power at different operational frequencies
from the CUTLASS Finland radar on 9 March 2009
when the heater frequency was changed aroundthe third electron gyro harmonic frequency. The
third electron gyro harmonic frequency 3fce wasestimated as a frequency on which the disappearance of the DM component in stimulated electromagnetic emission (SEE) spectra occurs. It
was found that artificial field-aligned irregularities (AFAIs) with a spatial scale across the magnetic field of 9 m, corresponding the CUTLASS
operational frequency of 17 MHz, are depressedat the third electron gyro harmonic in the lesser
degree than the AFAIs with larger scale of 13–
15 m (CUTLASS operational frequency of 10 and
13 MHz). The Te changes are not significant at
third electron gyro harmonic when the heater frequency fH is below the critical frequency foF2
by 0.5–0.7 MHz. The strongest AFAIs were excited above the third electron gyro harmonic byfrom 20–30 to 50–70 kHz when the SEE spectra
exhibit the generation of the nDM and BSS spectral components. A distinctly different phenomena were observed when the heater frequency wasnear the critical frequency, fH ≈ 3fce ≈ foF2 .

Such situation was realised on 11 March 2009 during heater-on period from 16:00–16:20 UT (fH ≈3fce ≈ fUHR ≈ foF2 ). Upper hybrid resonance altitude of the pump wave was about 220–230 km.
In this case extremely strong electron heating (upto 4500 K) and increases in the electron density up
to 30–40% were observed. We expect that in thisevent the strong Langmuir turbulence was excitednear the reflection altitude leading the formationof cavities and acceleration of electrons. The combined effect of upper hybrid resonance and gyro
resonance at the same altitude under fH ≈ foF2
gives rise to strong electron heating and excitationof striations, which at the magnetic zenith leads
to HF trapping and extension of HF waves to altitudes where they can excite Langmuir turbulence,leading to fluxes of electron accelerated to energies
that produce the measurable ionisation.
The generation of HF heater-induced ion upflows from the ionosphere initiated by powerful O-mode HF radio wave, injected towards themagnetic zenith, has been measured on 11 and
12 March 2009. Note that the observed ion upflows were weaker compared with the heaterinduced ion upflows during solar activity maximum. Figure 18 illustrates data from the EISCAT UHF radar at Tromsø, showing effects of HF
pumping on 11 March 2009. The UHF radar beam
pointed towards magnetic zenith. From 16:15 UT
the critical frequency foF2 was near and then below the heater frequency fH =4040 kHz. It was
found that the most intense ion upflows accompanied by the strongest electron heating were observed when the HF pump frequency was near thecritical frequency of the F2 layer. In the courseof experiment the DMSP F15 satellite was flying
above Tromsø. The comparison between EISCATUHF radar and DMSP satellite observations has
been made for heater-on period 15:20–15:40 UT on
11 March 2009 (in collaboration with E. Mishin and
C. Roth).
Figure 19 shows variations in the vertical andhorizontal (westward) velocities and the ion density along with their trends obtained by averaging over 10 s sliding window. TMZ =15:26:15 UT
is the time of the shortest distance, about 70 km,
from the magnetic zenith of the heater. The oval
boundary is about 20 s from TMZ . F17 flew 5◦
to the west and showed no signatures of heating.
Clearly seen near MZ are the ion density enhancement and short-scale oscillations in both velocity
components.
It is well know that artificial field-aligned irregularities (AFAIs) are excited near the reflection

Figure 17: Behaviour of electron temperature Te
from UHF radar and backscattered power at operational frequencies of about 9, 13, and 17 MHzfrom the CUTLASS Finland radar on 9 March2009 from 13 to 14:04 UT. The heater frequency
was changed by steps from 4040 to 4190 kHz.
The heater frequency was very close to thethird electron gyro harmonic frequency at 13:12–
13:14 UT. Heater-on periods at 13:36–13.38 and
14:08–14.10 UT were aborted and cycles from 13:32,
13:40 had a slow tune (more than 1 min).

level of powerful HF radio wave with O-modeof polarization at the the upper-hybrid resonance(UHR) altitude. Theoretical work undertaken in
the 1970s indicated that the thermal parametric instability (Grach and Trakhtengerts, 1976) and resonance instability (Vas’kov and Gurevich, 1976)

25

Figure 19: Variations in the vertical and horizontal (westward) velocities and the ion density alongwith their trends obtained at the DMSP F15 satellite on 11 March 2009. Insets show the detrended
values. The shortest distance, about 70 km, fromthe magnetic zenith of the heater was observed at
TMZ =15:26:15 UT.

Figure 18: Data from the EISCAT UHF radar atTromsø, showing effects HF pumping on 11 March
2009. The UHF radar beam pointed towards magnetic zenith.

plays an important role in the generation of suchirregularities. The generation of AFAIs is not possible for a powerful HF radio wave with X-mode
polarisation. The reason is that such HF wave isreflected below from the UHR height and AFAIs
can not be excited. During the October-November
2009 campaign for the first time very strong AFAIs
were detected with unusual features when HF
pumping was produced at X-mode polarisationand the heater frequency fH significantly exceeded
foF2 . A comparison between backscattered signals observed from CUTLASS radars and bi-static
HF radio scatter observations in St. Petersburg has
been made (in collaboration with T. Yeoman). Figures 20 and 21 depict CUTLASS Hankasalmi radar
data obtained on 5 and 6 November 2009.
From Figs. 20 and 21 it can be seen that thechange of the HF pump wave polarisation from
O-mode to X-mode leads to the appearance ofstrong backscattered signals. HF pumping was
produced at frequency of 4040 kHz. The criticalfrequency of ordinary mode from ionosonde data
was about 3.2 MHz. It is important to note thatstrong backscattered signals under X-mode polarisation of HF pump wave appeared when fH wascomparable with fxF2 . The signals scattered from
26

Figure 20: Backscattered power from CUTLASS
Hankasalmi radar at operational frequency of
about 10 MHz in the 18 range gate (top panel) andin range gates from 13 to 23 (bottom panel) on
5 November 2009.

heater-induced irregularities did not disappear after the heater was turned off. In addition, the temporal decay of heater-induced irregularities, seenin CUTLASS beam 5 backscatter, is unusually longFigure 22: The PMWE layer used in the analysis.

A. V. Zalizovski, et al., “Self-scattering of a powerful
HF radio wave on stimulated ionospheric turbulence”,
Radio Science 44, RS3010, doi:10.1029/2008RS004111,
2009.
Figure 21: Backscattered power from CUTLASS
Hankasalmi radar at operational frequency of
about 10 MHz in the 18 range gate (top panel) andin range gates from 13 to 23 (bottom panel) on 6
November 2009.

Artificial modification of polar mesospheric winter echoes with the EISCATHeater and the role of charged dust particles

and ranges up to 30 minutes. In the course of experiments the UHF radar was running at Tromsø.
Data from the UHF radar showed some increasein electron temperatures in the comparison with
O-mode heating at frequencies far above the foF2 .
The physical justification of the observed new phenomenon is not well-understood at present. Thereis a need to continue studies in this area by using avariety of techniques and methods to provide theformulation of a clear theoretical picture of highpower HF ionospheric interactions.
N. F. Blagoveshchenskaya, et al., “Phenomena inducedby powerful HF pumping towards magnetic zenith witha frequency near the F-region critical frequency and thethird electron gyro harmonic frequency”, Annales Geophysicae 27(1), 131–145, 2009.
N. F. Blagoveshchenskaya, et al., “SPEAR-induced fieldaligned irregularities observed from bi-static HF radio
scattering in the polar ionosphere”, Journal of Atmospheric and Solar-Terrestrial Physics 71(1), 11–20, 2009.
T. D. Borisova, et al., “Peculiarities of stimulated electromagnetic emission under action of higher-power HF
radiowaves, emitted by the SPEAR facility, on the sporadic E layer of the polar ionosphere”, Geomagnetism
and Aeronomy 49(5), 653–663, 2009. ERRATA: Geomagnetism and Aeronomy, 49(6), 822, 2009.
T. D. Borisova, et al., “Splitting of the Doppler frequency
shift of bi-static backscatter signals during the Sura experiments”, Geomagnetism and Aeronomy 49(4), 510–
518, 2009.

An investigation of polar mesosphere winterechoes (PMWE) has been carried out withthe mesosphere-stratosphere-troposphere Mobile
Rocket and Radar Observatory (MST MORRO)
radar operating at 56 MHz. MORRO has been deployed at the European Incoherent Scatter (EISCAT) installation near Tromsø in northern Norway, co-located with the EISCAT’s VHF and UHF
radars and RF heating facility. The main object of
the investigation is to examine whether, and if so,how, RF heating influences PMWE. In particular,
an experimental confirmation of the overshoot effect would indicate the presence of charged dust
particles. On 11 February 2008 we measured several weak and variable PMWE layers and we used
the RF heater with an on period of 20 s and off
period of 100 s to modulate the radar scatter fromthe layers. We chose one layer, which for 44 min
was the strongest and most stable layer, for further
analysis; see Fig. 22 where the layer in question isframed.
The signal intensity variation during an averaged on/off heater period shows the expected
weakening of the signal intensity when heating isturned on, followed by a significant small recovery of the signal during the on phase and a corresponding small overshoot of the signal strengthof about 13—15% over the background level when
heating is switched off, see Fig. 23. The recovery
and overshoot are attributable to charge accumulation on the dust particles due to electron heating. The overshoot characteristic curve shows thata considerable increase in the electron temperature

27

Figure 24: Spectra with electric field.
Figure 23: Characteristics of the signal strength
during an on/off heater period.

did take place during heating and that charged
dust particles should be present, probably with aradii of some nanometers.
C. La Hoz and O. Havnes, “Artificial modification of polar mesospheric winter echoes with an RF
heater: Do charged dust particles play an active
role?”, Journal of Geophysical Research 113, D19205,
doi:10.1029/2008JD010460, 2008.

Polar ionospheric heating
By analysing ISR observation data, the heating effects in polar winter ionospheric modification experiments carried out in January 2008 at Tromsø,
Norway, were studied. A clear disturbance effect is present under the O-mode over-dense heating conditions. The enhancement of the electron
temperature is up to 60%–120%, extending from150 km to 400 km. The disturbance of the electron density is not obvious, with a 12% maximum
decrease. A 1–2 kHz increase in the acoustic frequency can be observed, an enhancement in thepeak-to-valley ratio of the ion line and sometimes
its high-order harmonics can be seen as well. The
power of the ion line and plasma line has shown
overshoot effect, single-humped, double-humped
and triple-humped structures have appeared in
the power profile of plasma line, and the enhancement in power amplitude of the plasma line decreases exponentially as the frequency increases.
Additionally, with consideration of the elastic
collision between electrons and neural particles
and the excitation of rotation energy level, the effects of ionospheric heating on the spectra are in28

Figure 25: Spectra with pump frequency.

vestigated. Results show that with the increasein electric field, the non-Maxwellian feature is enhanced as indicated by Fig. 24. Figure 25 showsthat the non-Maxwellian feature is weakened as
the increase in heating frequency.
B. Xu, et al., “Incoherent scatter spectra due to HF heating in the low ionosphere region, Science in China Series E (Technical Sciences) 52(2), 1–5, 2009.
B. Xu, et al., “Observations of the heating experimentsin the polar winter ionosphere”, Chinese Journal of Geophysics 52(4), 859–877, 2009.

F-region electron heating by X-mode radiowaves
Modifications of the electron temperature in theF-region produced by powerful high frequency
radiowaves at 4.04 MHz transmitted in X-mode
were observed (Fig. 26). The experiments wereperformed during quiet nighttime conditions with
low ionospheric densities so no reflections occurred. Electron temperature enhancements of theorder of 300–400 K were obtained. Numerical simulation of ohmic heating by the pump wave reproduces both altitude profiles and temporal dependence of the temperature modifications in theexperiments.
H. Löfås, et al., “F-region electron heating by X-mode radiowaves in underdense conditions, Annales Geophysicae 27(6), 2585–2592, 2009.

Ionospheric modification and plasma
physics
The Space Plasma Exploration by Active Radar(SPEAR) facility, co-located with ESR, has beenused to study aspect sensitive phenomena when
the ionosphere is pumped with HF radio waves.
Observations of E- and F-region SPEAR-induced
spectral enhancements consistent with the actionsof both the purely growing mode and the parametric decay instability, together with E-region
enhancements consistent with mode conversion
along sporadic E-layer vertical gradients near thecritical layer have been made (Fig. 27). Consistent enhancements from field-aligned, around vertical and also from 5◦ south of field-aligned were
found. Reasons for the prevalence of observations
from (close to) vertical include the existence of
the Spitze region, throughout which propagating
high-power waves may reach their highest possible reflection point where RF-induced instabilities
may be excited. In addition, observations of enhanced field-aligned scatter may be aided by thepresence of field-aligned irregularities, which may
guide the electrostatic waves that are excited by
RF-induced instabilities. However, the enhancements for pointing directions of ∼5–8◦ south offield-aligned require further investigation.
The first power-stepping experiments using
SPEAR have been performed. Both CUTLASS
SuperDARN radars detected backscatter from
SPEAR-induced Artificial Field-Aligned Irregularities (AFAIs) while the effective radiated power of
SPEAR was varied from 1–10 MW. It was demonstrated that AFAI could be excited by a SPEARERP of only 1 MW and that once created the irregularities could be maintained for even lower
powers. The experiment also demonstrated thatthe very high latitude ionosphere exhibits hysteresis, where the down-going part of the power cycle
provided a higher density of irregularities than for
the equivalent part of the up-going cycle. The ESR

Figure 27: ESR ion and plasma line amplitudes
from 7 December 2005. Panels (a) to (d) show
the F-region ion-line (150–250 km), E-region ionline (80–110 km), the upshifted plasma-line anddownshifted plasma-line, respectively. Panel (e)shows the 32 m dish elevation angle. ESR fieldaligned (FA) pointing is denoted by black rectangles. The red bars indicate periods of high ionor plasma line amplitude consistent with the action of SPEAR. There are clear ion and plasma line
spectral enhancements from several directions, including from FA+15◦ , FA+10◦ , FA+5◦ , FA, FA-5◦
and FA-15◦ , with notable enhancement occurringin FA. The upshifted and downshifted plasma line
enhancements occur mainly in the E-region and areclearly well correlated, both with each other andwith the ion line enhancements.

failed to detect any hysteresis in the plasma parameters over Svalbard in stark contract with previous UHF measurements.
SPEAR has also been employed to excite ULF
waves on local magnetic field lines. An intervalfrom February 2006, when SPEAR was transmitting a 1 Hz modulation signal with a 10 min on/off
cycle was investigated. Ground magnetometerdata indicated that SPEAR modulated currents in29

Figure 26: Temporal evolution of the electron temperature for the three different days, (a) 17 October, (b) 18
October and (c) 19 October. Temperatures derived from conditionally averaged raw radar data, received at
the same offset time from the nearest HF on time, are plotted vs time along with the error bars. Exponential
fits to temperature rise and fall are shown in green. Results of the time dependent modeling of collisional
ohmic heating by the pump wave are shown in red.

the local ionosphere at 1 Hz, and enhanced a natural field line resonance with a 10 min period. Overhead signatures of the SPEAR-enhanced field line
resonance were present in the magnetic field datameasured by the magnetometer on-board Cluster 2. These results were the first joint groundand space-based detections of field line tagging by
SPEAR.

Aurora (DELTA) campaign. N2 rotational temperature was measured with a rocket-borne instrument launched from the Andøya Rocket Range,
neutral winds were measured from auroral emissions at 557.7 nm with a Fabry-Perot Interferometer (FPI) at Skibotn and the KEOPS, and ionospheric parameters were measured with the European Incoherent Scatter (EISCAT) UHF radar atTromsø. Altitude profiles of the passive energy deR. S. Dhillon, T. R. Robinson, and T. K. Yeoman, “Aspect
position rate and the particle heating rate were essensitive E- and F-region SPEAR-enhanced incoherent
timated using data taken with the EISCAT radar.
backscatter observed by the EISCAT Svalbard radar”,
The local temperature enhancement derived from
Annales Geophysicae 27(1), 65–81, 2009.
the difference between the observed N2 rotational
D. M. Wright, et al., “Excitation thresholds of field- temperature and the MSISE-90 model neutral temaligned irregularities and associated ionospheric hys- perature were 70–140 K at 110–140 km altitude.
teresis at very high latitudes observed using SPEAR- The temperature increase rate derived from theinduced HF radar backscatter”, Annales Geophysicae estimated heating rates, however, cannot accountfor the temperature enhancement below 120 km,
27(7), 2623–2631, 2009.
even considering the contribution of the neutral
S. V. Badman, et al., “Cluster spacecraft observations
density to the estimated heating rate. The obof a ULF wave enhanced by Space Plasma Exploration
served upward winds up to 40 m/s seem to reby Active Radar (SPEAR)”, Annales Geophysicae 27(9),spond nearly instantaneously to changes in the3591–3599, 2009.
heating rates (see Fig. 28). Although the windspeeds cannot be explained by the estimated heating rate and the thermal expansion hypothesis, theStudies of the thermospherepresent study suggests that the generation mechanism of the large vertical winds must be responsiTemperature enhancements and vertical ble for the fast response of the vertical wind to thewinds in the lower thermosphere asso- heating event.

ciated with auroral heating during the
Dynamics and Energetics of the Lower
Thermosphere in Aurora (DELTA) campaign

A coordinated observation of the atmospheric response to auroral energy input in the polar lower
thermosphere was conducted during the Dynamics and Energetics of the Lower Thermosphere in30

J. Kurihara, et al., “Temperature enhancements and vertical winds in the lower thermosphere associated withauroral heating during the Dynamics and Energeticsof the Lower Thermosphere in Aurora (DELTA) campaign”, Journal of Geophysical Research 114, A12306,
doi:10.1029/2009JA014392, 2009.

30
20

40

10
30

0
-10

20

-20
10

Vertical Wind Speed [m s-1]

Height-integrated Heating Rate [mW m-2]

40

Q
w

50

-30
0
21:00

22:00

23:00
00:00
01:00
02:00
Universal Time (12-13 Dec 2004)

-40
03:00

Figure 28: Time variations of the height-integrated
heating rate derived from the data observed with
the EISCAT UHF radar at Tromsø (solid line) andvertical wind speed derived from the auroral green
line observation with the Fabry-Perot Interferometer at Skibotn (dashed line).

Meso-scale thermospheric response
The meso-scale response of the thermosphere has
been studied at ESR on 5 Dec 2007 in conjunction with the Svalbard Fabry-Perot Interferometer(FPI) and SCANning Doppler Imager (SCANDI)
for a very localised heating event, in both time andspace, corresponding to the IMF Bz going negative for ∼50 minutes. Both optical instruments
measure neutral wind velocity and temperature,
which began to respond within 15 minutes to theonset of the disturbance. This is far more rapid
than expected. The localised winds were accelerated by up to 100 m/s over a period of half an hourwhile the winds in the rest of the region were fairly
steady. The neutral temperature rose by ∼100 K
over a period of 40 minutes over the entire field ofview. The importance of these observations is thatsignificant meso-scale variability is present in thethermosphere and therefore needs to be incorporated into models in order to properly account forenergy dissipation in the thermosphere.
E. M. Griffin, et al., “Upper thermospheric ion-neutral
coupling from combined optical and radar experiments
over Svalbard”, Annales Geophysicae 27(11), 4293–
4303, 2009.

Acceleration mechanism of high-speed
neutral wind observed in the polar lower
thermosphere
We investigated the acceleration mechanism of thelower thermospheric neutral wind when the iono-

Figure 29: The ion velocity at 211 km and (bottom)
ion (dotted line) and neutral wind (solid line) velocities at 118 km observed from 0600 to 1800 UT
on 16 June 2005 with ESR.

spheric convection becomes enhanced. The ESR
CP2 measurement on 16 June 2005 detected thatthe lower thermospheric wind accelerated to unusually high speed (∼500 m/s) (Fig. 29). Thiswind acceleration seemed to be well corresponding with the enhanced ionospheric convection after changes of the solar wind parameters by the
ACE satellite. We evaluated the ion drag and theJoule-heating-induced pressure gradient contributions on the generation of the high-speed neutral
wind. We concluded that the pressure gradient
force was the most probable force in this event.

T. T. Tsuda, et al., “Acceleration mechanism of highspeed neutral wind observed in the polar lower thermosphere”, Journal of Geophysical Research 114, A04322,
doi:10.1029/2008JA013867, 2009.

31

DELTA-2 campaign: Study of the ener- with instruments to measure several plasma pagetics and the wind dynamics in the po- rameters during the flight at mesospheric altitudes. A detailed analysis of the results of thelar lower thermosphere
Dynamics and Energetics of the Lower Thermosphere in Aurora 2 (DELTA-2) campaign was conducted under collaboration with the rocket, the
EISCAT UHF radar, Fabry-Perot interferometer(FPI), and various optical instruments in order tostudy the energetics and the wind dynamics in thepolar lower thermosphere from January 14 to 26,
2009. The S-310-39 sounding rocket, which carried trimethyl aluminum (TMA) to conduct in-situ
measurement of the neutral wind, was launchedfrom the Andøya rocket range at 00:15 UT on
26 January 2009. An auroral breakup occurred
about 10 minutes from the rocket launch. The
EISCAT UHF radar was operated for 107.5 hours
during the campaign under international collaborations with Norway, Sweden, Finland, Germany,
France, and Japan. The data set taken during the
campaign is appropriate for studying many scientific issues such as the wind dynamics, ionosphericconductivity, and current system. FPI (557.7 nm)
was operated with the rocket observation, andit provided dramatic wind variations associatedwith the breakup.

Studies of dust and meteorites
Measurements of meteor smoke particles during the ECOMA-2006 campaign
The EISCAT (European Incoherent SCATter)
radars did support the ECOMA (Existence andCharge state Of Meteoric smoke particles in the
middle Atmosphere) campaign conducted at Andenes (Andøya Island, Norway, 69◦ N, 16◦ E) in2006. Instrumented rockets were launched to investigate meteoric smoke particles. These particles
play an important role in atmospheric processes
such as in the nucleation of noctilucent clouds(NLC) and polar stratospheric clouds (PSC). The
experimental quantification of these meteor smoke
particles is a highly challenging and ongoing scientific project using in-situ rocket and groundbased radar observations. A new rocket-borne
particle detector which is a combination betweena classical Faraday cup and a Xenon flashlamp
for active photoionisation of meteoric dust particles and their subsequent detection of corresponding photoelectrons was introduced by Rappand Strelnikova (2009). The first rocket during
the ECOMA-2006 campaign was further equipped
32

ECOMA-01 rocket launch was published by Strelnikova et al. (2009) which clearly describes the instrumentation of the rocket payload and the scientific results.

In the following, one experiment on ECOMA01 will be presented in more detail. Onboard the
ECOMA payload an radio wave propagation experiment was launched to measure electron densities using the differential absorption of radio
waves. The neutral and ionised background atmosphere was simultaneously observed by the EISCAT radars located near Tromsø, Norway. During the night of the rocket launch the EISCAT
radars detected an enhanced ionization in the
D-region created after an energetic partical precipitation starting at 21:58 UT on Sep. 8, 2006.
Shortly after this time a sporadic E-layer (Es ) developed with maximum electron number densities of ∼105 cm−3 at an altitude of 94.5 km. The
layer was quite stable for about an hour and settled down until it disappeared around 0:00 UT.
The electron densities were observed with both
EISCAT radars on the mainland (VHF and UHF).
Fig. 30 shows the electron density measurements
obtained from the EISCAT UHF radar around thelaunch time of the rocket which is indicated by
the vertical line. The ionospheric conditions weremoderate to quiet which was also confirmed byriometer measurements. The right hand panel
shows the electron densities obtained from both,
UHF and VHF, radars and the radio wave propagation experiment. Between 93 and 96 km an increase of electron number densities was observed
where the red line shows the results from the Faraday rotation experiment. Note that the altitudedifference of the sporadic E-layer might be dueto the horizontal distance between the radar sites
and the rocket location (∼130 km). Comparing
ground-based and in-situ experimental results ofelectron number density measurements leads toqualitatively and quantitatively similar results.
Simultaneously, temperatures measurements
were obtained from the colocated Na-lidar and the
RMR-lidar as well as from the rocket-borne neutral
air density measurements. These measurements
show temperatures in large excess of the frost
point of water indicating that ice particles could
not be formed at mesospheric altitudes at the timeof the in-situ rocket measurements (Strelnikova etal., 2009). On the other hand, the ECOMA detector
registered particle signatures in both data chan-

Figure 30: Left panel: Electron number densities measured with the EISCAT UHF-radar on 8 September
2006. The red vertical line indicates the time of the ECOMA-01 start. Right panel: Electron number density
profile from the EISCAT UHF and VHF radars (black and blue lines) from the time of the ECOMA-01 launch
compared to the in situ results from the Faraday rotation experiment (red line) and the current to the positively
biased front grid of the ECOMA particle detector (green line, normalized to the Faraday rotation experimentat 110 km altitude). Note that the difference in altitude of the sporadic layer seen in the radar and rocket
measurementsis likely due to the horizontal distance between the different observations (∼130 km).

nels, the directly impacted particles on the detector electrode and the photoelectrons generated byphotoionisation or photodetachment of particles.
These photoelectron measurements showed thatparticles exist in the entire altitude range between
60 and 90 km. The measured currents were converted to meteor smoke particle number densities
which are in qualitatively agreement with model
predictions.
M. Rapp, and I. Strelnikova, “Measurements of meteor
smoke particles during the ECOMA-2006 campaign:
1. Particle detection by active photoionization”, Journal of Atmospheric and Solar-Terrestrial Physics 71(3–4), 477–485, doi:10.1016/j.jastp.2008.07.011, 2009.
I. Strelnikova, et al., “Measurements of meteor smoke particles during the ECOMA-2006
campaign:
2. Results”, Journal of Atmosphericand Solar-Terrestrial Physics 71(3–4),
486–496,
doi:10.1016/j.jastp.2008.07.011, 2009.

High statistics radar meteor studies at
EISCAT
An experiment was conducted with the European
Incoherent Scatter (EISCAT) radars during three 8hour runs on consecutive nights in December 2008
aiming to detect and study the high-altitude meteor population along with the meteors detected atclassical ∼100 km altitudes. The experiment usedcoaxial ultrahigh-frequency (UHF) and very highfrequency (VHF) radar beams pointed verticallyto the zenith of Ramfjordmoen near Tromsø (Norway), and remote UHF receivers at Kiruna (Sweden) and Sodankylä (Finland) for tristatic observations of a very limited volume at an altitude of
170 km above the transmitter site.
The EISCAT VHF radar detected during the 24hour period 22,698 echoes identified as meteors.
The number of UHF echoes in the same period
was 2138, most detected also at VHF. Among the
VHF meteors, 11 were detected at altitudes higher
than 150 km. Of these, the record highest meteor
was at 246.9 km. No high-altitude UHF echoes
were detected, none was tristatic, and no echoeswith a Doppler velocity above ∼60 km/s wereidentified. Given the large number of echoes,
which argues in favour of a highly significant characterization of the meteoroid population, we discuss the statistical properties of the detections andtheir possible physical nature.
The average detection rate of VHF radar meteors was about 16 min−1 . Comparing this high ratewith that of the faintest optically detected meteors
indicates that the radar detections originate froma meteoroid population that could be as optically
faint as 13–14 mag. We did not observe a marked
enhancement of the rates at the peak of the Gem-

33

backscatter due to the occurrence of polar mesosphere summer echoes (PMSE) rather than electron densities. The interpretation of the radarbackscatter for altitudes below 90 km is based on
the physics of PMSE.
M. Friedrich, et al., “Signatures of mesospheric particles
in ionospheric data”, Annales Geophysicae 27(2), 823–
829, 2009.

Solar wind studies
Interaction a between medium-scaletransient in the solar wind and a stream
interaction region

Figure 31: Altitude–Doppler-intensity plot for one
meteor track. The deceleration is evident since theDoppler velocity is smaller at lower altitudes. The
visible curvature of this plot implies that the deceleration was not constant; the meteoroid decelerated faster at lower altitudes.

inid shower, confirming once again the proposalthat most faint meteors, be these radar or optical,
belong to the sporadic population and not to a specific shower.
For a few meteors, our data show definite deceleration and possible fragmentation (Fig. 31). A
simple calculation indicates that one of the detected meteoroids was a submillimetre body thatfragmented when the ram pressure reached about
0.5 Pa. This is much lower than the pressure thatfragments brighter cometary meteors, which is atleast two orders of magnitude higher.
N. Brosch, et al., “Unusual features in high statistics
radar meteor studies at EISCAT”, Monthly Notices of
the Royal Astronomical Society 401(2), 1069–1079, 2010.

Signatures of mesospheric particles inionospheric data

We have combined Inter-Planetary Scintillation(IPS) measurements from EISCAT with whitelight observations from the STEREO spacecraft
HI instrument to study the interaction a between
medium-scale transient in the solar wind and a
stream interaction region, showing the transient
started within the slow wind and was subsequently captured by the star interaction region.
We have also observed smaller scale transients inthe slow wind, associated with significant fieldrotations. It is not yet clear whether these features are ubiquitous in the slow wind or associatedwith Coronal Mass Ejection (CME) wakes, butthey might be the same class of structures as the
pixel-scale features seen in LASCO spacecraft observations of the slow wind. An associated study
combined EISCAT and STEREO HI solar wind observations with in-situ measurements from Venus
Express ASPERA-4 instrument to study the impact
of stream interaction regions and solar wind transients on the Venus environment.
The large-scale structure in the solar wind has
been investigated using IPS. EISCAT data playeda key role in improving understanding of the evolution of the large CME of May 2005. A programme of comparing EISCAT IPS and STEREO
white-light results with the predicted signaturesderived from a multi-scale numerical model is underway, simulating IPS and white-light scattering by a CME, interacting CMEs or CME/stream
interaction region structures as they propagate
through the background solar wind. This development will significantly improve our ability to determine precisely which region of a CME the EISCAT observations correspond to.

During a ECOMA/MASS campaign in 2007, threesounding rockets were launched from Andøya,
Norway. This campaign was supported by several ground-based observations including the EISCAT UHF and VHF radars near Tromsø. The
electron density measurements from the EISCATUHF radar were considered in the discussion by
Friedrich et al. (2009). In the ionospheric E-region
the agreement between the EISCAT UHF and thein-situ probing of electron densities is remark- G. D. Dorrian, et al., “Transient structures and stream
ably good. It is well known that below 90 km interaction regions in the solar wind: Results from EISthe ground-based radar data reflect the coherent CAT interplanetary scintillation, STEREO HI and Venus
34

Express ASPERA-4 observations”, Solar Physics, submitted, 2010.
I. C. Whittaker, et al., “In-situ observations of a corotating interaction region at Venus identified by IPS
and STEREO”, Solar Physics, in press, 2010.
M. M. Bisi, et al., “Three-dimensional reconstructions of
EISCAT IPS velocity data during the declining phase ofsolar cycle 23”, Solar Physics, in press, 2010.

Figure 32: The 20-moment approximation for theincoherent scattering spectra parallel to E × B for
different electric field E.

M. M. Bisi, et al., “From the Sun to the Earth: the 13 May
2005 Coronal Mass Ejection”, Solar Physics, submitted,
2010.
M. Xiong, et al., “Forward modelling to determine theobservational signatures of white-light imaging and interplanetary scintillation for the propagation of an interplanetary shock in the ecliptic plane”, Journal of Atmospheric and Solar Terrestrial Physics, submitted, 2010.

Theoretical studies of incoherent
scattering spectra
20-moment approximation for ion velocity distribution and its application in calculations of incoherent scatter spectra
According to Grad’s theory, the ion velocity distribution function is expanded about a 20-moment
approximation based on Maxwellian distribution.
The effects of the stress tensor and the heat flow
vector on the ion velocity distributions are discussed. When the electric field is weak, it is reasonable to neglect the heat flow vector and thestress tensor parallel to E × B and E, respectively.
The ion temperature anisotropy and asymmetry inthe distribution function are caused by the stresstensor and the heat flow term. The incoherent
scatter spectra calculated by the 13-moment approximation and the 20-moment approximation
are compared. When the electric field is weak,the 13-moment is nearly consistent with the 20moment approximation. However it is unreasonable to neglect the heat flow tensor, and the temperature anisotropy is distinct in case of strong
electric field as is seen in Fig. 32). It is reasonable
to use the 20-moment approximation to describe
the non-Maxwellian plasma characterized by thetemperature anisotropy.
In addition, a sixteen moment approximation
based on a bi-Maxwellian that contains the stresstensor and the heat flow vector is applied to describe the ion velocity distribution which is suitable for the non-Maxwellian plasma characterisedby the large temperature anisotropy. A discussion
is made about the effects on the incoherent scatter spectra caused by different values of the normalized perpendicular drift velocity D, aspect angle φ between the magnetic field and the line-ofsight direction, and the ratio α of the ion-neutral
collision to ion cyclotron frequency. Numerical results show that the shifting and asymmetry of incoherent scatter spectra appear parallel to E × B
and E as the normalised perpendicular drift velocity D increases due to the ion drift velocity,
the stress tensor and the heat flow vector respectively. However, the spectrum is always typicallydouble-humped Maxwellian parallel to B. The
ion velocity distribution is more distorted from theMaxwellian as the aspect angle φ increases from0◦ to 90◦ , and consequently the incoherent scatter spectra is no longer typically double-humped
Maxwellian. As α increases, the ion velocity distribution becomes Maxwellian and the incoherent
scatter spectra become typically double-humped
Maxwellian even with a large value of the normalised perpendicular drift velocity D.
K. Xue, et al., “20-moment approximation for ion velocity distribution and its application in calculations ofincoherent scattering spectra”, Chinese Journal of Geophysics 52(2), 342–351, 2009.
K. Xue, et al., “16-moment approximation for ion velocity distribution and its application in calculations of incoherent scattering spectra”, Plasma Science and Technology 11(2), 152–158, 2009.
K. Xue, et al., “The ion distribution function fromMaxwell molecule collision model and calculations ofincoherent scatter spectra”, Chinese Journal of Space
Science 29(3), 287–295, 2009.

Incoherent scatter spectra of collisional
plasmaIncoherent scatter spectra of a collisional plasma
with an arbitrary velocity distribution function is35

Figure 33: Variation of the power spectrum withdifferent collision frequency.

presented. Two integrals with complex singularpoints have been solved in order to obtain the results. The incoherent scatter spectra during HF
heating in low ionosphere region are computed. A
super-Gaussian function is adopted in the calculation with a non-Maxwellian factor m. The effect ofcollision frequency, non-Maxwellian factor, electron density, electron temperature and ion temperature on power spectra is discussed (Fig. 33).
Under the action of collision frequency and nonMaxwellian factor, the original relationship between ionospheric parameters and the characteristics of spectra shape is invalid, which will bringa large error in the inversion of ionosphere parameters, thus the original theoretical model must be
corrected.
B. Xu, et al., “Incoherent scatter spectra of a collisional
plasma”, Acta Physica Sinica 58(7), 736–742, 2009.

36

List of publications 2009
Aikio, A.T., and A. Selkälä, Statistical properties of Joule
heating rate, electric field and conductances at high latitudes, Ann. Geophys., 27, 2661-2673, 2009.
Blagoveshchenskaya, N.F., H.C. Carlson, V.A. Kornienko, T.D. Borisova, M.T. Rietveld, T.K. Yeoman, and
A. Brekke, Phenomena induced by powerful HF pumping towards magnetic zenith with a frequency near theF-region critical frequency and the third electron gyro
harmonic frequency, Ann. Geophys., 27, 131-145, 2009.

Havnes, O., M. Kassa, G.E. Morfill and C. La Hoz, On
the sizes, charges and effects of dust particles in polar mesospheric winter echoes, Proceedings of the 19th
ESA Symposium on European rocket and Balloon Programmes and Related Research, 7-11 June 2009, Bad Reichenhall, Germany, Esa publication, 2009.

Cai, H.T., McCrea I.W., Dunlop M.W., Davies J.A., Bogdanova Y.V., Pitout F., Milan S.E., Lockwood M. and Ma
S.Y., Cusp observations during a series of fast IMF Bz
reversals., Ann. Geophys., 27, 2721-2737, 2009.

Havnes, O., C. La Hoz, M.T. Rietveld, M. Kassa, G. Baroni and A. Biebricher, Observation and analysis of olar
mesospheric winter echoes modulated by artificial electron heating, Proceedings of the 19th ESA Symposium
on European rocket and Balloon Programmes and Related Research, 7-11 June 2009, Bad Reichenhall, Germany, Esa publication, 2009.

Cai H.T., Ma S.Y., McCrea I.W., et al., Polar ionospheric
responses to 4-times rapid turnings of the IMF B-z
component-EISCAT/ESR radar observations, Chinese J.
Geophys. (in Chinese), 52(7): 1685-1692, 2009.

Kalogerakis, K.S., T.G. Slanger, E.A. Kendall, T.R. Pedersen, M.J. Kosch, B. Gustavsson, and M.T. Rietveld,
Remote Oxygen Sensing by Ionospheric Excitation(ROSIE), Ann. Geophys., 27, 2183-2189, 2009.

Dhillon, R.S., T.R. Robinson, and T.K. Yeoman, Aspectsensitive E- and F-region SPEAR-enhanced incoherent
backscatter observed by the EISCAT Svalbard radar,Ann. Geophys., 27, 65-81, 2009.

Kozlovsky, A., T. Turunen, and S. Massetti, Fieldaligned currents of postnoon auroral arcs, J. Geophys.
Res., 114, A03301, doi:10.1029/2008JA013666, 2009.

Friedrich, M., K.M. Torkar, W. Singer, I. Strelnikova, M.
Rapp, and S. Robertson, Signatures of mesospheric particles in ionospheric data, Ann. Geophys., 27, 823-829,
2009.
Fujii, R., Y. Iwata, S. Oyama, S. Nozawa, and Y. Ogawa,
Relations between proton auroras, intense electric field,
and ionospheric electron density depletion, J. Geophys.
Res., 114, A09304, doi:10.1029/2009JA014319, 2009.
Griffin, E.M., Aruliah, A.L., McWhirter, I., Yiu, H.C.I., and Charalambous, A.: Upper thermospheric ionneutral coupling from combined optical and radar experiments over Svalbard, Ann. Geophys., 27, 4293-4303,
2009.

Kurihara, J., Oyama, S. Nozawa, S., Tsuda, T.T., Fujii, R., Ogawa, Y., Miyaoka, H., Iwagami, N., Abe, T.,
Oyama, K.-I., Kosch, M., Aruliah, A., Griffin, E. , and
K. Kauristie, K., Temperature enhancements and vertical winds in the lower thermosphere associated with auroral heating during the Dynamics and Energetics of theLower thermosphere in Aurora (DELTA) campaign, J.
Geophys. Res., 114, A12306, doi:10.1029/2009JA014392,
2009.
Lanchester, B.S., M. Ashrafi, N. Ivchenko, Simultaneous
imaging of aurora on small scale in OI (777.4 nm) and
N21P to estimate energy and flux of precipitation, Annales Geophysicae 27(7), 2881–2891, 2009.

Hartquist, T., O. Havnes and M. Kassa, Exploring polarmesospheric summer echoes, Astronomy & Geophysics,
50, 1, 1.08 - 1.14, 2009.

Leyser, T.B., and E. Nordblad, Self-focused radio frequency L wave pumping of localized upper hybrid oscillations in high-latitude ionospheric plasma, Geophys.
Res. Lett., 36, L24105, doi:10.1029/2009GL041438, 2009.

Havnes, O., and M. Kassa, On the sizes and observable effects of dust particles in polar mesospheric winter echoes, J. Geophys. Res., 114, D09209,
doi:10.1029/2008JD011276, 2009.

Leyser, T.B., and A.Y. Wong, Powerful electromagnetic
waves for active environmental research in geospace,Rev. Geophys., 47, RG1001, doi:10.1029/2007RG000235,
2009.

37

Li, Hailong, Study on the echo characteristics of Polar
Mesosphere Summer Echoes, PhD thesis, Xidian University, China, 2009.

Pitkänen, T., A.T. Aikio, A. Kozlovsky, and O. Amm,
Reconnection electric field estimates and dynamics ofhigh-latitude boundaries during a substorm, Ann. Geophys., 27, 2157-2171, 2009.

Li Hailong, Wu Jian, Huang Jiying, Wang Maoyan, Oneanalysis on the rocket detection of polar mesospheresummer echoes, Chin. J. Space Sci., 29(4): 397-401,2009a.

Rapp, M., I. Strelnikova, B. Strelnikov, R. Latteck, G.
Baumgarten, Q. Li, L. Megner, J. Gumbel, M. Friedrich,
U.-P. Hoppe, and S. Robertson, First in situ measurement of the vertical distribution of ice volume in a mesospheric ice cloud during the ECOMA/MASS rocketcampaign, Ann. Geophys., 27, 755-766, 2009.

Li Hailong, Wu Jian , Huang Jiying , WANG Maoyan,
Study on the relation between the reflectivity and frequency in dusty plasma of polar summer mesopause,
Plasma Science and Technology, 11(3): 279-282, 2009b.

Rentz, Stefanie, The Upper Atmospheric Fountain Effectin the Polar Cusp Region, PhD thesis, Fakultät für Elektrotechnik, Informationstechnik, Physik der Technischen Universität Carolo-Wilhelmina zu Braunschweig,
Germany, 2009.

Li Hui Wu Jian Wu Jun Che Hai-Qing, Study on the
Sharp Boundary of Layered Dust Structure in the Summer Polar Mesopause, Chinese journal of polar research,
21(4): 272-278, 2009.
Lofas, H., N. Ivchenko, B. Gustavsson, T.B. Leyser, and
M.T. Rietveld, F-region electron heating by X-mode radiowaves in underdense conditions, Ann. Geophysicae,
27, 2585-2592, 2009.

Safargaleev, V.V., T.I. Sergienko, A.E. Kozlovsky, I. Sandahl, U. Brändström and D.N. Shibaeva, Electric fieldenhancement in an auroral arc according to the simultaneous radar (EISCAT) and optical (ALIS) observations,Geomagnetism and Aeronomy, 49, 3, 353-367, 2009.

Lunde, J., Particle Precipitation: Effects on Selected
Ionospheric Phenomena, Ph.D thesis, University ofTromsø, Norway, 2009.

Sojka, J.J., R.L. McPherron, A.P. van Eyken, M.J. Nicolls,
C.J. Heinselman, and J.D. Kelly, Observations of ionospheric heating during the passage of solar coronalhole fast streams, Geophys. Res. Lett., 36, L19105,
doi:10.1029/2009GL039064 , 2009.

Lunde, J., U. P. Løvhaug, and B. Gustavsson, Particle precipitation during NEIAL events: simultaneous
ground based nighttime observations at Svalbard, Ann.
Geophys., 27, 2001-2010, 2009.

Strelnikova, I., Mesospheric aerosol particles: Evidence from rocket and radar techniques, Ph.D. Thesis, Mathematisch-Naturwissenschaflichen Fakultat der
Universitat Rostock, Germany, 2009.

Maeda, S., Y. Ogawa, K. Hosokawa, S. Nozawa, S.
Oyama, T. Tsuda, and A. Brekke, Ion heating in highspeed flow channel within the duskside cell of the polarcap ion convection under large IMF-By condition, J.
Geophys. Res., 114, A11307, doi:10.1029/2009JA014300,
2009.

Strelnikova, I., M. Rapp, B. Strelnikov, G. Baumgarten,
A. Brattli, K. Svenes, U.-P. Hoppe, M. Friedrich, J. Gumbel, B.P. Williams, Measurements of meteor smoke particles during the ECOMA-2006 campaign: 2. Results, J.
Atmos. Sol.-Terr. Phys., 71, 3-4, 486-496, 2009.

Ogawa, Y., S. C. Buchert, R. Fujii, S. Nozawa, and
A. P. van Eyken, Characteristics of ion upflow anddownflow observed with the European Incoherent Scatter Svalbard radar, J. Geophys. Res., 114, A05305,
doi:10.1029/2008JA013817, 2009.

Taguchi, S., S. Suzuki, K. Hosokawa, Y. Ogawa, A.S.
Yukimatu, N. Sato, M.R. Collier, and T.E. Moore,
Moving mesoscale plasma precipitation in the cusp,J.
Geophys. Res., 114, A06211, doi:10.1029/2009JA014128,
2009.

Ogawa, Y., I. Haggstrom, S. C. Buchert, K. Oksavik,
S. Nozawa, M. Hirahara, A. P. van Eyken, T. Aso,and R. Fujii, On the source of the polar wind in thepolar topside ionosphere: First results from the EISCAT Svalbard radar, Geophys. Res. Lett., 36, L24103,
doi:10.1029/2009GL041501, 2009.

Tsuda, T. T., S. Nozawa, S. Oyama, T. Motoba, Y.
Ogawa, H. Shinagawa, N. Nishitani, K. Hosokawa,
N. Sato, M. Lester, and R. Fujii, Acceleration mechanism of high-speed neutral wind observed in the polar lower thermosphere, J. Geophys. Res., 114, A04322,
doi:10.1029/2008JA013867, 2009.

Osepian, A., S. Kirkwood, P. Dalin, and V. Tereschenko,
D-region electron density and effective recombination
coefficients during twilight - experimental data andmodelling during solar proton events, Ann. Geophys.,27, 3713-3724, 2009.

Vierinen, V., et al., Measuring space debris with phase
coded aperiodic transmission sequences, Proceedings of
the 5th European Conference on Space Debris, 2009.

38

Vierinen, V., and M. S. Lehtinen, 32-cm wavelengthradar mapping of the moon, Proceedings of the 6th European Radar Conference, 2009.
Vierinen, J., J. Markkanen, and H. Krag, High powerlarge aperture radar observations of the IridiumCosmos collision, Proceedings of the 10th Advanced
Maui Optical and Space Surveillance Technologies Conference, 2009.
Virtanen, I., Multi-purpose Methods for Ionospheric
Radar Measurements, Ph.D. Thesis, Department of
Physics, University of Oulu, Finland, Report No. 59, Report Series in Physical Sciences, ISBN 978-951-42-9283-5,
ISSN 1239-4327, Oulu University Press, Oulu 2009.
Virtanen, I.I., J. Vierinen, and M. S. Lehtinen, Phasecoded pulse aperiodic transmitter coding, Ann. Geophys., 27, 2799-2811, 2009.
Wood, A.G., S. E. Pryse, and J. Moen, Modulation ofnightside polar patches by substorm activity, Ann. Geophys., 27, 3923-3932, 2009.
Xu, Bin, Study on the incoherent scatter spectra and its
application in the ionospheric heating, PhD thesis, Xidian University, China, 2009.
Xu Bin, Wu Jian, Wu Zhensen and Xue Kun, Incoherent Scatter Spectra due to HF Heating in the Low Ionosphere Region, Sci China Ser E-Tech Sci , 52 (2): 1-5,
2009b.
Xu Bin, Wu Jun, Wu Jian, Wu Zhensen, Che Haiqin,
Xu Zhengwen, Xue Kun, Yan Yubo, Observations of
the heating experiments in the polar winter ionosphere,
Chinese Journal of Geophysics, 52(4): 859-877, 2009c.
Xue, Kun, Theoretical and Experimental Study on the
Incoherent Scatter Spectrum of High Latitude Auroral
Ionosphere, PhD thesis, Xidian University, China, 2009.
Zalizovski, A.V., S.B. Kashcheyev, Y.M. Yampolski, V.G.
Galushko, V. Belyey, B. Isham, M.T. Rietveld, C. La
Hoz, A. Brekke, N.F. Blagoveshchenskaya, and V.A. Kornienko, Self-scattering of a powerful HF radio wave
on stimulated ionospheric turbulence, Radio Sci., 44,
RS3010, doi:10.1029/2008RS004111., 2009.

39

EISCAT Operations 2009
The EISCAT radars operate in two basic modes,
using approximately half the available observing
time for each. In the Special Programme mode,
users conduct individual experiments dedicatedto specific experiments and objectives. The resulting data are reserved for the exclusive use of theexperimenters for one year from the date of collection. Special programmes often make use of
the well developed pulse schemes and observing
modes of the Common Programme. EISCAT Common Programmes are conducted for the benefit of
the entire user community and the resulting data
are immediately available to all. The common Programme modes are developed and maintained by
EISCAT staff, and the overall programme is monitored by the Scientific Advisory Committee. Common Programme operations are often conducted
as part of the coordinated World Day programmeorganised by the International Union of Radio Scientists (URSI) Incoherent Scatter Working Group(ISWG).
Common Programme One, CP-1, uses a fixedtransmitting antenna, pointing along the geomagnetic field direction. The three-dimensional velocity and anisotropy in other parameters are measured by means of the receiving stations at Kiruna
and Sodankylä (see map, inside front cover). CP-1
is capable of providing results with very good time
resolution and is suitable for the study of substorm
phenomena, particularly auroral processes whereconditions might change rapidly. The basic time
resolution is 5 s. Continuous electric field measurements are derived from the tri-static F-region
data. On longer time scales, CP-1 measurements
support studies of diurnal changes, such as atmospheric tides, as well as seasonal and solar-cycle
variations. The observation scheme uses alternating codes for spectral measurements.
Common Programme Two, CP-2, is designed tomake measurements from a small, rapid transmitter antenna scan. One aim is to identify wave-likephenomena with length and time scales comparable with, or larger than, the scan (a few tens ofkilometers and about ten minutes). The present
version consists of a four-position scan which iscompleted in six minutes. The first three positions
form a triangle with vertical, south, and south-east
positions, while the fourth is aligned with the geomagnetic field. The remote site antennas provide
three-dimensional velocity measurements in the Fregion. The pulse scheme is identical with that of
CP-1.
Common Programme Three, CP-3, covers a 10◦
latitudinal range in the F-region with a 17-position
scan up to 74◦ N in a 30 minute cycle. The observations are made in a plane defined by the magnetic meridian through Tromsø, with the remotesite antennas making continuous measurements at
275 km altitude. The coding scheme uses alternating codes. The principle aim of CP-3 is the mapping of ionospheric and electrodynamic parameters over a broad latitude range.
Common Programmes One, Two, and Three are
run on the UHF radar. Three further programmes
are designed for use with the VHF system. The
UHF and VHF radars are often operated simultaneously during the CP experiments. Such observations offer comprehensive data sets for atmospheric, ionospheric, and magnetospheric studies.
Common Programme Four, CP-4, covers geographic latitudes up to almost 80◦ N (77◦ N invariant latitude) using a low elevation, split-beam configuration. CP-4 is particularly suitable for studies
of high latitude plasma convection and polar cap
phenomena.
Common Programme Six, CP-6, is designed for
low altitude studies, providing spectral measurements at mesospheric heights. Velocity and electron density are derived from the measurements
and the spectra contain information on the aeronomy of the mesosphere. Vertical antenna pointing
is normally used.
Common Programme Seven, CP-7, probes highaltitudes and is particularly aimed at polar windstudies. The present version uses both of the VHF
klystrons and is designed to cover altitudes up to2500 km vertically above Ramfjordmoen.
Equivalent Common Programme modes areavailable for the EISCAT Svalbard Radar. CP-1
is directed along the geomagnetic field (81.6◦ in-40

clination). CP-2 uses a four position scan. CP3 is a 15 position elevation scan with southerly
beam swinging positions. CP4 combines observations in the F-region viewing area with fieldaligned and vertical measurements. Alternatingcode pulse schemes have been used extensively
for each mode to cover ranges of approximately
80 to 1200 km with integral clutter removal below
150 km.
The tables on the next pages summarise the accounted hours on the various facilities for eachmonth and for each Common Programme mode
(CP) or Associate (SP).

41

2009
KST COMMON PROGRAMMES
2009
CP1
CP2
CP3
CP4
CP6
CP7
UP1
UP2
UP3
Total
%

Jan

Feb
Mar
7.5
5

Apr
3

May
102.5

Jun

Jul

Aug

Sept

87.5

Oct

Nov

352.5
80.5
32.5

87.5

11

87.5
9

11
1

24.5

87.5
9

64.5
7

85.5
9

3
0

102.5
11

0
0

352.5
38

0
0

0
0

Dec

%

Dec

Total Incl AA Target
132
135
51
169
174
86
75
78
50
95.5
101
102
234
245
196
211
219
141
101.5
109
132
43
1061
1061
758
100

Total
118
440
135 215.5
0
131
0
24.5
0
0
135
929
15
100

Target%
13
16
47
16
23
12
0
10
14
20
0
18
3
0
0
100

KST SPECIAL PROGRAMMES
2009
CN
FI
GE
NI
NO
SW
UK
AA
Total
%

Jan

Feb

Mar

15
13.5
32.5
33
21
6.5

Apr

May

Jun

Jul

Aug
Sept
132

Oct

31
14.5
6
12.5

121.5
11

0
0
EI

CN
6.7

Target

36
16

15
11
72.5

47.5
27
107.5
10

0
0
FI
11.4

31
3
GE
6.56

Nov

100

35.5

46
10
154.5

46.5
4

246.5
23

203
19

6

21

24.5

2

37
3

112
11

140
13

NI
13.41

NO
25.91

SW
18.6

16
16
2

87
16

UK
17.43 %KST OTHER PROGRAMMES
2009
3P
EI
TNA
TB
Total

Jan

Feb

Mar

Apr

May

Jun

8

Jul
Aug
Sept
18.5
1

35
11.5
19.5

0

63.5
63.5

0

0

35

Oct

Dec

0.5
67.5
54.5
122.5

8
101
48.5
157.5

Oct

Nov

0
46.5
25
71.5

0
246.5
122.5
369

Dec
Total Target
135
929
980
203
1061
758
157.5 527.5
369
495.5 2517.5
2107

Oct
44.5

Nov
215.5
40
26.5
346.5
0

85
18.5

1

85

Total Target
15
27.5
31
8.5
120
288.5
203
203
369
527.5

Nov

25
25

KST CUMULATIVE TOTALS
2009
CP
SP
OP
Total

Jan
87.5
121.5
19.5
228.5

Feb
Mar
64.5
85.5
0 107.5
0
63.5
64.5 256.5

Apr
3
0
0
3

May
102.5
31
0
133.5

Jun
87.5
37
35
159.5

Jul
11
112
18.5
141.5

Aug
0
140
1
141

Sept
352.5
16
85
453.5

USAGE BREAKDOWN
2009
UHF
VHF
Heating
Passive UHF
ESR
Passive ESR

Jan
179
14
142
126.5

Feb
Mar
29.5 131.5
32.5
49.5
46
11
119
120
98.5

Apr
3

May
75.5

Jun
108
8

11.5

133
82

177.5
108
58

Jul
42
70
30
0

Aug
Sept
60 278.5
28
16
50.5
19
9.5
560
33.5 267.5

42Page 1

12.5
58.5
21

Dec
Total Target
257
1424
856
128
386
363
13.5
198
285
374.5 1931.5
2414
287.5
1156
1342
58

2009
ESR COMMON PROGRAMMES
2009
CP1
CP2
CP3
CP4
CP6
CP7
UP1
UP2
UP3
Total
%

Jan
3
30.5

Feb
Mar
82.5
49

2.5

Apr
May
0.5
54

1.5

Jun

Jul

Aug

Sept
1.5
254.5

Oct

Nov

83.5
1.5

33.5
5

85
13

50.5
8

2
0

54
8

83.5
13

0
0

0
0

256
38

0
0

0
0

Dec

Total
141.5
334
103
103
0
87.5
1.5
0
0
0
103 667.5
15
100

%

Target%
21
54
50
16
15
12
0
10
13
0
0
0
0
100

Dec

Total Incl AA Target
0
4
34
26.5
33
58
15
19
33
61.5
69
68
94.5
110
132
44.5
56
95
97
107
89
59.5
398.5
399
509
100

ESR SPECIAL PROGRAMMES
2009
CN
FI
GE
NI
NO
SW
UK
AA
Total
%

Jan

Feb

Mar

Apr

May

Jun

Jul

Aug

Sept

Oct

Nov

4

22.5
15
33.5

8
14.5
57.5
84
21

10
13
22
35
9

12
26
48
12

9.5

28

21

7
29.5
30

9.5
14.5

9.5
2

28
7

39
10

0
0

33.5
8

11.5
11.5
3

21
5

0
0

89
22

ESR OTHER PROGRAMMES
2009
3P
EI
TNA
TB
Total

Jan

Feb

Mar

Apr

May

Jun

Jul

Aug

Sept

Oct

Nov

Dec

0

Total Target
9
12
0
25
0
95.5
95.5
96
95.5 104.5
133

0
0
0
0

Dec
Total Target
103 667.5
700
89 398.5
509
95.5 104.5
133
287.5 1170.5
1342

9

9

0

0

0

0

0

0

0

0

0

ESR CUMULATIVE TOTALS
2009
CP
SP
OP
Total

Jan
33.5
84
9
126.5

Feb
Mar
85
50.5
35
48
0
0
120
98.5

Apr
2
9.5
0
11.5

May
54
28
0
82

Jun
83.5
39
0
122.5

Jul

Aug
0
0
0
0

0
33.5
0
33.5

43
Page 2

Sept
256
11.5
0
267.5

Oct
0
21
0
21

Nov

Beynon medals
5th Prof. Nobuo Matuura 2007 Awarded by theCouncil of the EISCAT Scientific Association
to Professor Nobuo Matuura. In recognitionof his contributions to the successful establishment of the EISCAT Svalbard Radar at
Longyearbyen and to the expansion of the
EISCAT Scientific Association to include nonEuropean members
6th Prof. Markku Lehtinen 2008 Awarded by theCouncil of the EISCAT Scientific Association
to Professor Markku Lehtinen. In recognition of his seminal contributions to the development of advanced modulation techniques
for incoherent scatter radars and to the mathematical foundations and implementation ofeffective incoherent scatter radar data analysis systems

The EISCAT Council awards distinguished persons the Sir Granville Beynon medal.

7th Dr. Gudmund Wannberg 2009 Awarded by
the Council of the EISCAT Scientific Association to Doctor Gudmund Wannberg. In
recognition of his persistent work for the
1st Prof. Tor Hagfors 2002 Awarded to Professor
technical development of EISCAT radars and
Tor Hagfors on 4th February 2002 for his outhis invaluable contribution to the EU Design
standing services to the EISCAT Scientific AsStudy project for the EISCAT_3D radars.
sociation and to Ionospheric Physics

Recipients

2nd Prof. Tauno Turunen 2003 In recognition ofimportant contributions to the techniques of
Incoherent Scatter Radar and outstanding services to the EISCAT Scientific Association
3rd Prof. Jürgen Röttger 2004 In recognition ofoutstanding services to the EISCAT Scientific Association including the establishmentof the EISCAT Svalbard Radar at Longyearbyen
4th Prof. Henry Rishbeth 2006 Awarded by theCouncil of the EISCAT Scientific Association
to Professor Henry Risbeth. In recognition ofoutstanding contributions to the scientific exploitation of incoherent scatter in Europe including the UK PUSCAT and MISCAT radars
and the radars of the EISCAT Scientific Association
44

EISCAT organisational diagram, December 2009.

Hosts

Instruments

ActiveSites

Headquarters

Council andCommittees

Funding
Agencies

University of Oulu/SGO

Sodankylä

DFG
Germany

DeutscheForschungsgemeinschaft

STEL
Japan

Dynasonde

Heating

UHF

Headquarters

Tromsø

IRF Kiruna

NIPR
National Institute ofPolar Research

NFR

VHF

NorwayNorgesforskningsråd

University of Tromsø

EISCAT Council

Japan

Solar Terrestrial
Environment
Laboratory, Nagoya

KirunaSOC
Science OversightCommittee

Finland

China

SA
Suomen Akatemia

CRIRP
China ResearchInstitute ofRadiowave
Propagation

VR

STFC
United Kingdom

Science andTechnology
Facilities Council

NTIFIC AS
IE

ESR

Longyearbyen

Management
Committee/
Council Advisory Group

SwedenVetenskapsrådet

CAT S
C
EIS

45

CIATIONSO

EISCAT Scientific Association
December 2009
Council

Director

The Council consists of a Delegation of each Associatewith a maximum of three persons from each Associate.

Dr. E. Turunen

Council Advisory Group
FinlandDr. K. Kauristie
Prof. T. Nygrén
Dr. K. Sulonen
Germany
Dr. H. BoosProf. J. Röttger
Japan
Prof. R. Fujii
Dr. H. Miyaoka
NorwayProf. A. Brekke
Dr. B. Jacobsen
Dr. L. Lønnum
SwedenDr. T. Andersson
Prof. D. Murtagh
P. R. of China
Prof. Q. Dong
Prof. J. Wu
United Kingdom
Dr. I. McCrea
Ms. R. Young

Towards the end of the year the previous Management
Committee was reformed into the Council Advisory
Group. Its members were not yet finalised in December
2009, the list here is of the acting members.

Chairperson
Delegate
Delegate

Mr. H. Andersson
Dr. T. Andersson
Prof. A. Brekke
Dr. K. Kauristie
Dr. E. Turunen

Delegate
Delegate

Delegate

Head of Administration
Council Vice-Chairperson
Council Member
Council Chairperson
Director

Executives
Senior Management

Vice-Chairperson, Delegate

Mr. H. Andersson
Dr. E. Turunen

Delegate

Head of Adm., Deputy Dir.
Director

Site Leaders
Delegate

Station Managers
Mr. H. Boholm
Mr. R. Jacobsen
Mr. M. J. Postila
Dr. M. T. Rietveld
Mr. L.-G. Vanhainen

Scientific Oversight Committee
Under the guidance of the Council, the EISCAT scientific community organises a Scientific Oversight Committee.
Dr. A. Aikio
Dr. N. BlagoveshchenskayaDr. S. Buchert
Dr. J. Chau
Dr. M. Kosch
Prof. C. La Hoz
Prof. R. Liu
Prof. S. Nozawa
Prof. J. Röttger

FinlandExternal member
SwedenExternal member
United Kingdom
NorwayChairperson, P. R. of China
Japan
Germany

46

EISCAT Svalbard Radar
Tromsø Radar
Sodankylä Site
Tromsø Heating
Kiruna Site

EISCAT staff at the Annual Review Meeting, 11–13 February 2009, at Pallastunturi, Finland.

48

Appendix:
EISCAT Scientific Association
Annual Report, 200949

EISCAT Scientific Association Annual Report 2009

EISCAT Scientific Association
Registered as a Swedish non-profit organisation
Organisation number: 897300-2549
Annual report for the financial year 2009-01-01 – 2009-12-31
The EISCAT Council and the Director for the Association herewith submits the annual reportfor 2009.
Content
Administration report
Profit and loss accounts
Balance sheet
Statement of cash flows
Notes

Page
1
5
6
7
8

50

EISCAT Scientific Association Annual Report 2009

ADMINISTRATION REPORT
Ownership, organisation and objective
The EISCAT Scientific Association was established in 1975 through an agreement between six
European organisations. Japan joined in 1996 and the Peoples Republic of China in 2007.
The EISCAT Associates at 2009-12-31 are: China Research Institute of Radiowave Propagation(Peoples Republic of China), Deutsche Forschungsgemeinschaft (Germany), National
Institute of Polar Research (Japan), Norges forskningsråd (Norway), Science and Technology
Facilities Council (United Kingdom of Great Britain and Northern Ireland), Solar-Terrestrial
Environment Laboratory, Nagoya University (Japan), Suomen Akatemia (Finland), andVetenskapsrådet (Sweden).
A new EISCAT Agreement came into force 2007-01-01, with all Associates making long term
funding commitments to the Association. The Association has its formal seat in Kiruna,
Sweden, and is registered as a non-profit organisation.
The aim of the Association is to make significant progress in the understanding of physicalprocesses in the high latitude atmosphere by means of experimental programmes generally
conducted using the incoherent scatter radar technique, which may be carried out as part ofwider international projects. For this purpose, the Association has developed, constructed,
and now operates, a number of radar facilities at high latitudes. At present, these comprise asystem of stations at Tromsø (Norway), Kiruna (Sweden), Sodankylä (Finland), andLongyearbyen (Svalbard).
The Association is fully funded by the Associates but additional operations may also be
funded by short term additional contributions from both Associate and non-Associatebodies. Depending on the available funding, scientific priorities and operational targets areadjusted on an annual basis.
The EISCAT Council is charged with the overall administration and supervision of the
Association's activities. The Council appoints a Director, who is responsible for the daily
management and operation of the facilities of the Association.
Operation and scientific development
The EISCAT Radars delivered a full programme of operations for the user community andoperated reliably throughout the year with only minor interruptions due to equipment oroperational problems.
The various EISCAT radars operated for a total of 3 688 accounted hours (5 209 hours in2008).
Common Programmes amounted to 43% (34%) of the operations. Special Programmes
amounted to 40% (34%) and other operations, such as the TNA project runs, amounted to17% (32%) of the total run hours.

-2-

51

EISCAT Scientific Association Annual Report 2009

Both contracts under the European Union’s Sixth Framework Programme initiative, the
EISCAT_3D design study and the Transnational Access project ended during the year.
Both projects were completed in a proper manner. The EISCAT_3D project planning
continues and a bid for the European Union’s Seventh Framework Programme, ESFRI
projects preparatory phase, was submitted in December.
The Transnational Access project funded six user campaigns and 195 hours (92 hours) ofoperation during the final period of the four year project.
Scientists from France, Ukraine and Russia paid for the use of the facilities. Totally
298.5 hours (211.5 hours) were run on behalf of these affiliated countries.
The annual staff review meeting was held in Pallastunturi, Finland, mid February. EISCAT
scientists attended several international conferences during the year. The EISCAT_3D
continued work, including setting up the new consortium that submitted the preparatory
project bid, and promotion trips also meant frequent travel. The number of travel days
increased by about 50% in 2009.
Future operation and scientific development
During the coming year, EISCAT will continue to support the wide range of existing and new
programmes proposed by the various Associates’ scientific communities, including thehosting of user-supplied equipment.
It is though expected that UHF tristatic runs will no longer be possible beyond July 2010
since the required disturbance free frequency slots in Finland and Sweden will be taken inuse by mobile phone operators. In Sweden, the operators will have access to the frequency
spectrum 1 March 2010 and in Finland 1 January 2010, though it has been stated that the
Finnish operator will only start using it near the Finnish site 1 July 2010 and the Swedish one
perhaps not at all in 2010.
Ways of continuing tristatic capabilities are considered. The primary option is the planned
EISCAT_3D system which will give full three-dimensional capabilities. Since the EISCAT_3D
project is still years from build, intermediate steps are evaluated which could fill somescientific requirements, like meteor studies, while waiting for the new system.
The three other radar systems, UHF in monostatic mode, VHF and the Svalbard Radarcontinues undisturbed. The Heating facility has recently been modernised and its extended
capabilities allows for new experimental modes.
The work of the Council and its committees
The Council had two ordinary and one extraordinary meeting under the leadership of the
Chairperson, Dr. Kirsti Kauristie: in June, Berlin, Germany and in October, Lillehammer,
Norway. An extraordinary telephone conference meeting was held as in December.

-3-

52

EISCAT Scientific Association Annual Report 2009

The management committee had two meetings: in May, Longyearbyen, Svalbard and in
September, Sodankylä, Finland.
The Scientific Oversight Committee had two meetings during the year: March, Kühlungsborn,
Germany and in September, Arecibo, Puerto Rico.
Council considered mainly regular business matters. The transfer of Associateship from UK’s
Science and Technology Facilities Council (STFC) to the Natural Environment ResearchCouncil (NERC) resulted in the extraordinary meeting. The addressed issue, the length of the
UK commitment at the time of transfer, is now resolved.
Council decided also to change the remit of the management committee such that it
becomes an advisory group for Council. The new Council Advisory Group is headed by theCouncil Chairperson and will provide guidance and advice to Council.
Budget development during the year
The 2009 operations ended very close to the operating target set for the year. Both EU
supported projects ended during the year. Both were four year projects and both ended asenvisaged though bit below the initial budget total.
French and Ukrainian scientists took advantage, against payment, of the systems. It is
anticipated that both countries, and Russia, will continue to make use of the systems also inthe coming years.
Most of the regular Associates, Finland, Japan, Norway, P. R. of China, Sweden and United
Kingdom agreed to add an inflationary compensation to their annual contributions in 2009.
In addition, since the contributions are in local currencies, the income side benefited fromthe relatively weak SEK-currency. Due to low global interest levels, the budgeted bankinterest on own funds did not meet the target.
The continued EISCAT_3D work resulted in a bid for a preparatory phase, under the EU
Framework Programme 7 initiative. The application was submitted in December 2009 andthe first evaluation results look promising.
The long-term budget plan
The long-term budget plan is becoming challenging due to the current known funding
shortage from 2012 onwards. For 2010 and 2011, we do not anticipate any issues other than
the reported tristatic problem and the overall operating target for these years can be
maintained.
The result for 2009 and the deficit handling
The year was balanced by transferring the surplus, relative to the budget, of 3 415 kSEK, tothe investment fund.

-4-

53

EISCAT Scientific Association Annual Report 2009

PROFIT AND LOSS ACCOUNTS
in thousands of Swedish Crowns
2009
26 5866 180
32 7662008
23 6118 592
32 203‐5 257‐4 517‐17 706‐2 198‐29 677‐6 361‐4 253‐23 956‐5 026‐39 596

Operating profit/loss

3 089‐7 393

Interest income
Other financial income and cost
Own reserves and funds

85‐622‐1 335‐1 871

866
351
‐145
1 072

1 217

‐6 321‐3 415
2 198‐1 217

1 295
5 026
6 321

0

0

Note 1

Associate contributions
Other operating income

Note 2

Operation costs
Administration costs
Personnel costs
Depreciation of fixed assets

Note 3Note 4

Profit/loss after financial items
Appropriations
Transfer from funds invested

Note 5Note 6

Net profit/loss for the year

‐5‐

54

EISCAT Scientific Association Annual Report 2009

BALANCE SHEETin thousands of Swedish Crowns
2009

2008

3 843
821
2 099
6 764

3 995
2 041
1 643
7 679

3 871
640
19 22223 7331 723
610
20 37022 70330 49630 383Note 116 764
18 76325 526

7 108
16 05323 161

Note 120509

Note 13

4 469
155
345
4 970

4 768
37
1 908
6 713

30 49630 383

0

509

none

none

ASSETS
Fixed assets
Tangible fixed assets
Buildings
Radar systems
Equipment and tools

Note 7

Current assets
Receivables
Prepayments and accrued income
Cash at bank and in hand

Note 8Note 9Total assets
CAPITAL AND LIABILITIESCapitalFunds invested
Funds held on reserve

Note 10

Long term liabilities
Long term liabilities
Current liabilities
Liabilities, trade
Provisions
Other liabilities

Note 14

Total capital and liabilities
Pledged assets
Contingent liabilities

‐6‐

55

EISCAT Scientific Association Annual Report 2009

STATEMENT OF CASH FLOWS
in thousands of Swedish Crowns
2009

2008

Operating activities
Operating result before financial items
Transfer from funds invested

3 089
2 198

‐7 393
5 026

Interest received
Currency exchange rate changes
Extra ordinary income and cost

85
‐658
36

866
314
37

‐2 148‐30‐2 252878
5‐11 364321‐11 631

Investment activities
Investments in tangible assets‐1 469‐908

Cash flow from investment activities‐1 469‐908

Cash flow for the year

‐1 148‐12 539

Liquid assets at the beginning of the year

20 37032 909Liquid assets at the end of the year

19 22220 370

Increase/decrease of receivables
Increase/decrease of prepayments and accrued income
Increase/decrease of creditors and liabilities
Cash flow from operations

‐7‐

56

EISCAT Scientific Association Annual Report 2009

NOTES
Note 1 Accounting principles

2009

2008

Salaries and emoluments paid to the Directors

1 240

6 583

Other personnel, employed and provided
via site contracts

11 031

11 472Social security contributions amounted toof which for pension costs

3 944
1 992

4 717
3 170

Personnel costs in total

The accounting and valuation principles applied are consistent with theprovisions of the Swedish Annual Accounts Act and generally accepted
accounting principles (bokföringsnämnden allmänna råd ochvägledningar).
All amounts are in thousands of Swedish kronor (SEK) unless otherwise
stated.
Receivables
Receivables are stated at the amounts estimated to be received, basedon individual assessment.
Receivables and payables in foreign currencies
Receivables and payables in foreign currencies are valued at the closing
day rate. Where hedging measures have been used, such as forwarding
contracts, the agreed exchange rate is applied. Gains and losses relating
to operations are accounted for under other financial income and cost.
Bank accounts in foreign currencies
Bank balances in foreign currencies are valued at the closing day rate.
Fixed assets
Tangible fixed assets are stated at their original acquisition values after
deduction of depreciation according to plan. Assets are depreciatedsystematically over their estimated useful lives. The following periods ofdepreciation are applied: Buildings 5 ‐ 50 years, Radar systems 3 ‐ 20years and Equipment and tools 1 ‐ 5 years.
Note 2 Associate contributions
The Associates contributed to the operation during the year inaccordance with the agreement. The commitments are in local
currencies. The received contributions have been accounted in SEK.
2009
CRIRP (P. R. of China)
3 129
DFG (Germany)
1 964
NIPR (Japan)
1 820
RCN (Norway)
6 010
SA (Finland)
3 996
STFC (United Kingdom)
4 039
VR (Sweden)
5 628
26 586
Accumulated contributions status as of 2009‐12‐31
1976 ‐ 2009
Previous Associates
190 074
CRIRP (P. R. of China)
10 609DFG (Germany)
188 749
NIPR (Japan)
66 904
RCN (Norway)
134 376
SA (Finland)
58 817
STFC (United Kingdom)
214 391
VR (Sweden)
108 029971 948
Note 3 Personnel costs and average number of employees
The Association employs directly the Headquarters staff, currently about
six positions, including the Director. The Headquarters is located in
Kiruna, Sweden. The personnel working at the Kiruna (Sweden),
Sodankylä (Finland), Svalbard and Tromsö (Norway) sites are not
employed by the Association. Instead, the personnel are provided via
site contracts by the Swedish Institute of Space Physics (Kiruna site
staff), Oulu University (Sodankylä staff) and Tromsö University (Tromsö
and Svalbard staff). The Association refunds all expenses related to theprovided staff, as well as an additional overhead.

‐8‐

57

The new Director, Dr. Esa Turunen, started his employment 2009‐01‐01.
His employment contract with Council is for three years.
Of the pension costs, 320 kSEK (previous directors 1 660 kSEK) relates tothe Director. He and all other directly employed staff are included in ITP
like occupational pension plans. For the personnel provided via site
contracts, the pension plans are handled by their respective employer.
The members of the board (EISCAT Council) and members ofcommittees, who represents Associates, do not receive remunerations
from the Association. Travel expenses in connection with Council andcommittee meetings are normally covered by the Associates. For theCouncil Advisory Group (earlier named Management Committee), theAssociation cover meeting and travel costs.
Salaries and emoluments and average number of staff per country
Finland
Salaries and emoluments
Average number of staff ‐ men and women

1 528
3+0

1 767
4+0

Norway (including Svalbard)
Salaries and emoluments
Average number of staff ‐ men and women

5 370
9+0

12 033
10 + 1

SwedenSalaries and emoluments
Average number of staff ‐ men and women

5 372
8+1

4 255
6+1

Members of the board and Directors at year‐end ‐ men and women
The board consist of delegations from every Associate country eachhaving a Delegate (formal member) and up to two Representatives.
Board members (EISCAT Council)
Directors

12 + 4
1+0

12 + 42+0

Capital Operating reserve
Budgeted transfer to the reserve
Transfer from the reserve
Investments made‐1 6141 469‐2 040

‐396
908
‐942

External projects reserve
Design study project complete,contingency released

1 504

‐675

Restructuring reserve
Budgeted restructuring costs

1 500

1 355

‐28
9

‐27
9

Note 4 Own reserves and funds
Transactions involving own reserves and funds.

Spare parts reserve
Budgeted transfer to the reserve
Transfer from the reserve

EISCAT Scientific Association Annual Report 2009

2009

2008

Investment fund
Budgeted transfer to the fund

‐2 0000

Surplus fund
Budgeted transfer from the fund
Budgeted transfer to the fund

4 062
‐4 1963 685‐4 062Sum own reserves and funds‐1 335

‐145

2009

2008

Note 8 Prepayments and accrued income
The main buildings and systems insurance for 2009 was paid in
December.
Prepaid rents
Prepaid insurances
Other items

Note 5 Appropriations

Note 9 Bank balances status

The outcome for this year became a surplus relative to the budget
amounting to 3 415 kSEK. The amount has been transferred to theInvestment fund. The 2008 outcome was a loss (‐1 295 kSEK) which wascovered by funds from the Restructuring reserve.

NordeaCash in hand

Note 6 Transfer from funds invested

Buildings
Radar Systems
Equipment and Tools

91
460
89
640

92
492
26
610

19 2202
19 22220 3691
20 370

3 843
821
2 099
6 764

3 424
2 041
1 643
7 108

Note 10 Funds invested status
The depreciation cost is covered by funds from Capital ‐ funds invested
Note 7 Tangible fixed assets
Changes in tangible fixed assets during 2009.
Note 11 Funds held on reserve
Buildings
Opening acquisition value
Acquisitions during the year
Disposals during the year
Closing acquisition value
Opening accumulated depreciation
Depreciations during the year
Disposals during the year
Closing accumulated depreciation
Closing residual value
Radar systems
Opening acquisition value
Acquisitions during the year
Disposals during the year
Closing acquisition value
Opening accumulated depreciation
Depreciations during the year
Disposals during the year
Closing accumulated depreciation
Closing residual value
Equipment and tools
Opening acquisition value
Acquisitions during the year
Disposals during the year
Closing acquisition value

42 237137
042 37442 23700
42 237‐38 242‐289
0‐38 531‐37 956‐286
0‐38 242

3 843

3 995

244 381103
0
244 484

244 38100244 381‐242 340‐1 3230‐243 662‐238 389‐3 9510‐242 340

821

2 041

31 9251 229‐98
33 05731 078908‐61
31 925‐30 283‐586‐89‐30 958‐29 442‐789‐52‐30 283

Closing residual value

2 099

1 643

Sum tangible fixed assets

6 764

7 679

Opening accumulated depreciation
Depreciations during the year
Disposals during the year
Closing accumulated depreciation

Investments were made a bit below the budgeted expectation. Less
spare parts than budgeted were acquired. Since the EISCAT_3D design
study ended close to the planned target, the External project reserve did
not need to be used and the funds were released. The positive outcomeof this year (3 415 kSEK) has been put into the Investment fund. The
other transfers were as budgeted.
Capital operating reserve
Equipment repair fund
External projects reserve
Investment fundRestructuring reserve
Spare parts reserve
Surplus fund

1 369
754
0
7 971
4 101
371
4 196
18 763

1 223
754
1 504
2 556
5 601
353
4 062
16 053Note 12 Long term liabilities
Husbanken Norway loan concerning the owned flat on Svalbard was
paid‐off during the year. In 2008 the loan was amortized (34 kSEK).
Note 13 Liabilities, trade
Both EU‐contracts, the EISCAT_3D Design Study and the
EISCAT_USERS_1 Transnational access project ended during the year. In
2008, non released funds were accounted as liabilities.
Liabilities EU, EISCAT_3D pre‐financing
Liabilities EU, USERS_1 pre‐financing
Other liabilities, trade

0
0
4 469
4 469

0
913
3 855
4 768

Note 14 Provisions
The electricity provider on Svalbard did an errorounus cost debit Q1
2009. It is assumed that it will be corrected when settling the year.
Council cost
Electricity cost

‐9‐

58

0
155
155

37
0
37

EISCAT Scie nt ific Associa tion Annual Report 2009

Tokyo 2010-06-03

Dr. Tomas Andersson

Prof. Ryoich i Fujii

Dr. Michael SchultzProf. Jian Wu

Dr. Kati Sulonenk~~Dr. Karin Zac

L-z=- -Dr. Esa Turunen
Director

Our audit report was issued on 2010- 0b-

11

iJL

rs. Annika Wedin

Authorised Public Accountant- 10 -

59

Ohrlings

Audit report
To the council of EISCAT Scientific Association
Corporate identity number 897300-2549[ have audited the annual accounts, the accounting records and the administration of the council
and the director of E[SCAT Scientific Association for the year 2009. These accounts and theadministration of the association and the application of the Annual Accounts Act when preparing
the annual accounts are the responsibility of the council and the director. My responsibility is toexpress an opinion on the annua l accounts and the administration based on my audit.
[ conducted my audit in accordance with generally accepted auditing standards in Sweden . Thosestandards require that [ plan and perform the audit to obtain reasonable assurance that the annual
accounts are free of material misstatement. An audit includes examining, on a test basis, evidence
supporting the amounts and disclosures in the accounts. An audit also includes assessing theaccounting principles used and their application by the council and the director and sign ificant
estimates made by the counci l and the director when preparing the annual accounts as well as
evaluating the overall presentation of information in the annual accounts. As a basis for my opinion
concerning discharge from liability, I examined significant decisions, actions taken andcircumstances of the association in order to be able to determine the liability, if any, to the council
or the director. I a lso examined whether any council member or the director has, in any other way,
acted in contravention of the Annual Accounts Act or the statutes. I believe that my audit provides
a reasonable basis for my opinion set out below.
The annual accounts have been prepared in accordance with the Annual Accounts Act and give atrue and fair view of the association's financial position and results of operations in accordancewith generally accepted accounting principles in Sweden.
The statutory administration report is consistent with the other parts of the annual accounts.
The council and the director have not acted in contravention of the statutes.

Gavle, 14 June 2010

Annika Wedin
Authorized Public Accountant

60

61

Report 2009 of the EISCAT Scientific Associationc EISCAT Scientific Association
EISCAT Headquarters
Box 812, SE-981 28 Kiruna, Sweden
Scientific contributions: EISCAT Associates and staff

62

CAT SCEISCIATIONSO

NTIFIC AS
IE

The EISCAT Associates
December 2009

CRIRP

China Research Institute of Radiowave Propagation
China
www.crirp.ac.cn

SA

Suomen Akatemia
Finlandwww.aka.fi

DFG

Deutsche Forschungsgemeinschaft
Germany
www.dfg.de

STEL

Solar Terrestrial Environment Laboratory, NagoyaJapan
www.stelab.nagoya-u.ac.jp

NIPR

National Institute of Polar ResearchJapanwww.nipr.ac.jp

NFR

Norges forskningsråd
Norwaywww.forskningsradet.no

VR

Vetenskapsrådet
Swedenwww.vr.se

STFC

Science and Technology Facilities Council
United Kingdom
www.scitech.ac.uk

EISCAT Scientific Association
Headquarters
EISCAT Scientific Association
Box 812
SE-981 28 Kiruna, Sweden
Phone: +46 980 79150
Fax: +46 980 79159
www.eiscat.se

Sites
KirunaEISCAT Kiruna Site
Box 812
SE-981 28 Kiruna, Sweden
Phone: +46 980 79136
Fax: +46 980 29276

Sodankylä
EISCAT Sodankylä Site
Tähteläntie 54B
FIN-99600 Sodankylä, Finland
Phone: +358 16 619880
Fax: +358 16 610375

Tromsø
EISCAT Tromsø Site
Ramfjordmoen
N-9027 Ramfjordbotn, Norway
Phone: +47 776 20730
Fax: +47 776 20740

Longyearbyen
EISCAT Svalbard Radar
Postboks 432
N-9171 Longyearbyen, Svalbard
Phone: +47 790 21236
Fax: +47 790 21751