On the IP structures and geospace consequences during WHI

1
On the IP structures and geospace consequences
during WHI

• Alisson Dal Lago1 , Fernando Luis Guarnieri2 ,
  Marlos Rockenbach da Silva1 , Walter Gonzalez1 ,
  Carlos Roberto Braga1,3 , Nelson Jorge Schuch3 ,
  Kazuoki Munakata4 , C. Kato4 , John W. Bieber5 ,
  Takao Kuwabara5 , M. Tokumaru6 , M. L. Duldig7 ,
  J. E. Humble8 , Ismail Sabbah9

1 - National Institute for Space Research -
DGE/CEA/INPE - MCT, Sao Jose dos Campos, SP,
Brazil 2 - Universidade do Vale do Paraiba,
UNIVAP, Sao Jose dos Campos, SP, Brazil 3 -
Southern Regional Space Research Center -
CRS/INPE - MCT, in collaboration with the Santa
Maria Space Science Laboratory - LACESM/CT- UFSM,
Santa Maria, RS, Brazil. 4 - Shinshu University,
Japan 5 - Bartol Res. Institute, Department of
Physics and Astronomy, University of Delaware,
Newark, Delaware, USA. 6 - STE Laboratory, Nagoya
University, Japan 7 - Australian Antarctic
Division, Australia 8 - School of Mathematics and
Physics, Univ. of Tasmania 9 - Physics
Department, Faculty of Science, University of
Alexandria, Alexandria, Egypt
2
Outline

• Some observations during the period of the Whole
  Heliosphere Interval (WHI) of the effects of
  interplanetary (IP) structures on the near earth
  space
• Ground-based cosmic ray data from the Global
  Muon Detection Network (GMDN)
• Magnetic field and plasma from the Advanced
  Composition Explorer (ACE) satellite
• Geomagnetic indices (Disturbance storm-time Dst
  and auroral electrojet index AE)
• Summary

3
Whole Heliosphere Interval (WHI)

• CH2068 March 20 April 16, 2008

4
(No Transcript)
5
Muon Detector at SSO/CRS/INPE, São Martinho da
Serra, Brazil, (since 2005) PI N. J. Schuch
6
Global Muon Detector Network (GMDN)
Okazaki, 2008
PI K. Munakata
7
IP disturbances (CME,Shock)
Geomag. storms CR storms

• Cosmic-ray storms
• Isotropic intensity depression
• Forbush Decrease
• Enhanced anisotropy
• Parallel to IMF
• Loss-cone (deficit) flux, excess flux of shock
  reflected CRs
• Perpendicular to IMF
• B?n anisotropy
• enhancement is also seen preceeding shock
  arrival

(Munakata)
8
Global Muon Detector Network (GMDN) Loss-cone

Rufolo, 1999
Munakata et al., 2000
9
B?n streaming
Center direction of CME (local geometry of CME )
(Munakata)
10
WHI DOY 85-90
y
z
x
11
Okazaki, 2008
12

• The IMF sector in this period is "toward"
  impling that the Earth is north of the
  Heliospheric Current Sheet (HCS), on which the
  local maximum of GCR density is expected.
• It seems that the local maximum of GCR density
  on the HCS passed SOUTH of the Earth

13
High Speed Solar Wind Streams

• High velocity flows emanating from Coronal Holes.
• Usually these structures have a highly
  fluctuating magnetic field.
• These fluctuations are associated to high
  amplitude Alfvén waves remnants of heating
  processes in the solar corona. (Hollweg, 1978)
• On the Earths magnetosphere, these waves may
  produce particles penetration and precipitation.
  (Garret et al., 1974 Tsurutani and Gonzalez,
  1987 Tsurutani et al., 1990 Tsurutani et al.,
  1995 Tsurutani and Lakhina, 1997)
• May lead to weak or moderate geomagnetic storms
  on Earth.

14
HILDCAA events
High Intensity, Long Duration, Continuous AE
Activity (Tsurutani and Gonzalez, 1987)
- The AE peak must reach, at least, 1000 nT -
The event must last for, at least, two days -
The AE values cannot decrease to less than 200 nT
for more than 2 hours at a time - The event must
occur outside the main phase of a geomagnetic
storm.
HILDCAA Criteria
These events are not a continuous substorm, but a
new form of energy deposition in the auroral
ionosphere. (Tsurutani et al., 2004 Guarnieri et
al., 2004 Guarnieri, 2005 Guarnieri, 2006) The
interplanetary magnetic field during these events
presents large amplitude fluctuations (Alfvén
waves) instead of southward directed fields.
(Tsurutani and Gonzalez, 1987 Gonzalez et al.,
1999 Guarnieri, 2005)
15
HILDCAA events
Magnetic field component plots indicating the
presence of Alfvenic fluctuations in the solar
wind.
16
HILDCAA events
Magnetic field component plots indicating the
presence of Alfvenic fluctuations in the solar
wind.
The black arrow indicates the HILDCAA event
duration.
17
HILDCAA effects

• - Weak to Moderate geomagnetic activity (observed
  by the Dst index)
• - Very intense auroral electrojet activity (AE
  index)
• - HILDCAA auroras are mild, but widely spatially
  distributed (even in the dayside) and long
  lasting. Guarnieri (2007) had shown (using POLAR
  images) that the integrated emissions during
  these auroras can be even higher than those
  observed during some very intense geomagnetic
  storms
• - During these prolonged intervals of HILDCAAs,
  increased fluxes of relativistic electrons are
  observed, which can have significant impact over
  satellite systems. These electrons, in the energy
  range from 40-400 keV are called killer
  electrons. (Paulikas and Blake, 1976 Mann et
  al., 2004 Lam, 2004 Love et al., 2000
  Tsurutani et al., 2006 Guarnieri et al., 2007).

18
WHI HILDCAA
19
WHI HILDCAA
20
Summary

• Some observations during the period of the Whole
  Heliosphere Interval (WHI) of the effects of
  interplanetary (IP) structures on the near earth
  space
• Ground-based cosmic ray data from the Global
  Muon Detection Network (GMDN)
• Magnetic field and plasma from the Advanced
  Composition Explorer (ACE) satellite
• Geomagnetic indices (Disturbance storm-time Dst
  and auroral electrojet index AE