Kiruna KIR Lycksele SGU in collaboration with IRF since 2007 Staff M Yamauchi Daria Mikhaylova technical contact Mats Luspa softwaredatabase contact Lars Göran ID: 815937
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Slide1
Magnetometers by IRF observatory
Kiruna
(KIR)
Lycksele
: SGU
in collaboration with IRF (since 2007)
Staff:
M. Yamauchi,
Daria Mikhaylova (technical contact), Mats Luspa (software/database contact),Lars-Göran Vanhainen (technical subcontact), , Csilla Szasz, Peter Volger,Peje Nilsson, Fredrik RutqvistUrban Braendström (Observatory PI) Peter Wintoft (for TOR variometer)
only
variometer
(TOR)
Slide2(1) Vector field (every 1 sec):
Flux gate
variometer
(Kiruna)
# Primary ⇐ new one is standby
# Secondary (backup)
(3) Total field (every 4 sec): Proton magnetometer = scalar value (Kiruna) # in operation (old one) # spare (new one)Specialty of Kiruna: near the iron mining
can combine with other measurements - auroral image - riometer - ionosonde (new dynasode from 2017!)(2) Absolute measurement (weekly): DI flux magnetometer (Kiruna) # in operation # spareKiruna magnetometers
(
4) Higher frequency than 1 Hz: Pulsation
magnetometer (
Kiruna
)
#
3 sensors (XYZ) in
oparation
# no spae
Slide3Declination
5°
0°
in
20
years
Some of data products
northward (BX)
eastward (By)vertical downward (BZ
)
11100 nT
10600 nT
0 nT
-1400 nT
52000 nT
50600 nT
average
(baseline +
variometer
)
Slide4(1) Unique nowcast ability: combining with auroral image
all-sky image take meridian part make keogram combine
(concept: aurora = optical energy + electric current energy)
Web-interface
aurora ?
auroral keogram
northward component (B
X)
BY and BZ are also shown in the same graphwww2.irf.se/mag/
Slide5(2) Unique nowcast of dB/dt and sd(B) over 10 min (+/- 5 min) window.
all-sky image calculate aurora luminosity at all pixel strength index
Web-interface (New !)
2018-3-14
breakup 21:30 UT
∆B
X (10-min window)also shows big jump
Slide6Add Pulsation magnetometer (future)
Ionospheric ion response to the September 2017 space weather event
M. Yamauchi
1
, T. Sergienko
1
, C.-F. Enell2,
and M. G. Johnsen31. Swedish Institute of Space Physics (IRF), Kiruna, Sweden2. EISCAT Scientific Association Headquarter, Kiruna, Sweden3. Tromsø Geophysical Observatory (TGO), Tromsø, Norway
Slide8Advantage of
Scandinavia during the September 2017 event
EISCAT/Norwegian magnetic chain of IMAGE
near local noon when X9.3 flare occurred
near local midnight when ICME arrived, first with IMF
Bz
northward without substorm, and next day with IMF southward with substormnear local noon when only IMF changed from northward to < -15 nTmany sudden southward turnings of IMF in the morning sector where the outflow flux is highcf. Cluster: over cusp (only equinoxes)exactly at cusp when ICME arrived (multiple crossing the cusp) Yamauchi et al. (2018): http://doi.org/10.1029/2018SW001937 Schillings et al. (2018): http://doi.org/10.1186/s40623-019-1048-0
Slide9X flares
Bz change
Bz changes
1
st
SEP
/CME
2
nd
SEP
/CME
Slide10X flares
1
st
SEP
/CME
Bz change
Bz changes
2
nd
SEP
/CME
Slide11day 2017
arrival UTevent
IMF Bz
6 Sep.
~09:00X2.2 flare
< 0 nT
6 Sep.~11:55X9.3 flare < 0 nT 6 Sep.~18 UTX-ray < M-class
~0 nT (B ~ 3 nT) 6 Sep.~20 UT~22 UTSEP-like enhancementIts sharp increase 0 nT (B ~ 3 nT) 6 Sep.
~23:50ICME> 5 nT (change from near zero) 7 Sep.~02:25 – 10:45many Bz changes to < - 5 nT and < 0< -5 nT 7 Sep.~14:30(X1.3 flare)
positive
7 Sep.~20:45
Bz
change to < 0
< -8 nT
7 Sep.
~23:10
ICME
< -25 nT (enhanced from -9 nT)
8 Sep.
~02:
35 – 07:10
many sharp
Bz
polarity
changs
8 Sep.
~11:20
Bz
change to < 0< -5 nT (later -17 nT)
Event list #1
Slide12X flares
Bz change
Bz changes
No major substorm by X-flare or 1
st
CME arrival
strong substorm before 2
nd
CME arrival (match with SEP/proton event)
1
st
SEP
/CME
2
nd
SEP
/CME
Slide13EISCAT geometry
Density (Ne) spike @<200 km, at the time of X flare
Temperature increase after X flare (pre-condition for outflow)
Sq
current drastically increase after X flare (enough Joule heating)
Auroral-like activity
before CME without ∆BH (IMF was weak, Bz>0)
only SEP-like event can trigger such activityCME triggered strong Sunward convection at midnight to morning
X 2.2 flares
CME arrivalSEP-like evet
X 9.3 flares
Slide16Slide17Scandinavia was at right location
X9.3 flare at near local noon (increase ionization rate)EISCAT observed (a) density spike of < 10 min @<200 km (b) increase of Te
(c) No change in upflow after X flare (flare set up only pre-condition?)IMAGE chain detected
Sq current enhancement with ~30 min period (but EISCAT detected Ne enhancement ~ 15 min period) ICME/SEP-like event arrivals at midnight in consecutive days
(Cannot distinguish if the ionospheric effect is due to CME or SEP event)"substorm-like arc motion " without ∆B before ICME but after SEP event
IMF direction is important for substorm (1st: Bz>0, 2nd:
Bz<0)Dayside outflow was 8th>7th>6th increasing by 1-order of magnitude / Cluster observed increase of already-high O+ outflow flux after CME Ionospheric flow after IMF turning southHorizontal flow is enhanced, but upflow is decreased in the morning /Different timing between horizontal flow and vertical flowOutflow region becomes outside EISCAT field-of-view for Bz<0
Slide18X flares
1
st
CME
2
nd
CME
Bz change
Bz change
Slide19X flares
1
st
CME
2
nd
CME
Bz
change
Bz
changes
Slide20Summary
and Discussion
Effect of X-flares
Pre-condition for outflow rather than direct increase of outflow
Sq enhancement with oscillating nature
Effect of ICME (substorm, GOES proton event) or SEP-like event?
Substorm-like motion of auroral arc before ICME SEP is the cause?Outflow increases, but the cause cannot be distinguished between ICME and SEP-like eventSudden turning to IMF Bz<0It is not clear if southward IMF triggers more outflow in morningIn statistics, outflow flux for Bz<0 is only twice for Bz>0, while outflow flux depend on Kp exponentially
Outflow region becomes outside EISCAT field-if-view for southward IMF Bz>0 might favor outflow if only dayside effect is considered.