Substorm Activity during CME and CIR Driven Storms

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Substorm Activity during CME and CIR Driven Storms

• Smitha Thampi, Diwakar Tiwari, Ruigang Wang, Hui
  Zhang, Ling Qian Zhang, Yihua Zheng
• Tutor Robert L. McPherron

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Introduction Scientific Background

• Geomagnetic storms, in which the global
  geomagnetic field intensity decreases on the
  order of tens to hundreds nT, are large scale
  phenomena in the solar wind-magnetosphere-ionosphe
  re coupling.
• Geomagnetic storms develop when solar
  wind-magnetosphere couplings are intensified by
  solar wind disturbances (coronal holes and CMEs).
  
• Types of Geomagnetic storms CME driven, CIR
  driven, (others)

Solar maximum (CMEs)
Solar minimum (CIRs)
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Introduction Scientific Background --- continued

• Characteristics (view of the present) the storms
  driven by the fast CMEs are usually very intense
  (Dst lt-100 nT), while the storms diven by CIRs
  are usually weaker and their main phase has
  irregular profile and long recover phase lasting
  many days to weeks and cause High Intensity Long
  Duration Continuous AE Activity (HILDCAAs). Since
  they are caused by recurrent high speed streams,
  they are ordered in time.
• Importance Although CIR storms are weak, they
  may be very important in generating relativitic
  electrons (semiannual variation of killer
  electrons and Dst in solar minimum), which are
  detremental to spacecraft, human in space and so
  on. gt
• Focus of the proposal Characteristics of CIR
  storms and the differences and similarities
  between the two types of magnetic storms

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CIR storms killer e- fluxes
High flux of killer electrons appear in solar
minimum
Killer electrons' semiannual variations
Dst also has semiannual variations
gt solar min storms correlate with killer
electron fluxes
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Scientific Objectives

• Scientific objectives to understand the
  characteristics, and the differences and
  similarities of the solar origin (the driver) of
  the two types of magnetic storms and the
  differences and similarities of the ionosphere's
  responses to the two-type storms via auroral
  activities. Specifically, we will use 40 years of
  solar wind and IMF data along with other
  necessary parameters to study
• Difference (if any) between CME and CIR Storms
  (solar wind and IMF para.)
• Distribution of AE during CME and CIR storms
• Duration of AE disturbances in the recovery phase
  of two types of storms
• The role of Russell-McPherron effect on CIR
  storms
• Effects of the two storm types on relativistic
  electrons
• Other Ionospheric effects caused by the two
  types. (???? more specific?)

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Significance of the proposal

• Scientifically this investigation will help in
  better understanding the following outstanding
  questions related to geomagnetic storms a) the
  role of solar wind density in storm growth? b)
  How do the properties of storms change with the
  solar cycle? c) Does storm development depend on
  season and universal time?
• Pratically with better understanding of the
  driver characteristics of two types of storms
  during solar minimum and solar maximum, it will
  help us in a better definition of forecasting
  procedure from the solar origin, which is crucial
  in space weather forecasting.
• Relativistic (killer) electrons are
  detremental to satellites, human in space and can
  also create great damage on the ground. They are
  known to have high fluxes during solar minimum
  and are possibly correlated to CIR driven storms.
  Understanding their relationship is very
  important for reducing or minimizing their
  damaging effects.

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Approach

• Data sets required
• OMNI data
• Synchronous relativistic electron fluxes
• ISCAT/SuperDARN Range-Time-Intensity/Velocity
• Preprocessing
• Data editing and creation of Matlab binary files
• Analysis tools
• Plot solar wind and IMF data along with AE and
  Dst indices to select events and then the
  significant times for further analysisgt
• Use Matlab built-in functions and/or procedures
  and also develop necessary software to perform
  statistical analysis and display tools

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Details on analysis approaches
An example of how to find CIR recurrent high
speed stream interface
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Preliminary results
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Preliminary results
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Preliminary Results
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Work Plan (1 year)

• Data Downloading Ruigang Wang and Hui Zhang
  (1month)
• Software development Diwakar Tiwari, Smitha
  Thampi (1 month)
• Literature search and knowledge enhancement
  Yihua Zheng and Ling Qian
• Zhang (1 month)
• These are done simultaneously.
• Event selection and data analysis divide and
  conquer, each of
• the team members perform the investigation for
  several years (10 month)
• nterpretation of the results all (1 month)

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References
1. Gonzalez, W. D., B. T. Tsurutani and A. L. C.
Gonzalez, Interplanetary origin of geomagnetic
storms, Space Sci. Rev. 88, 529-562,1999 2.
Kamide, Y., R.L. McPherron, W.D. Gonzalez, D.C.
Hamilton, H.S. Hudson, J.A. Joselyn, S.W. Kahler,
L.R. Lyons, H. Lundstedt, and E. Szuszczewicz,
Magnetic storms Current understanding and
outstanding questions, in Proceedings of the
Chapman Conference on Magnetic Storms, pp. 1-19,
American Geophysical Union, Jet Propulsion
Laboratory, Pasadena, CA, 1997. 3. McPherron,
R.L., Physical processes producing magnetospheric
substorms and magnetic storms, in Geomagnetism,
Vol 4, edited by J. Jacobs, pp. 593-739, Academic
Press Ltd., London, England, 1991. 4. O'Brien,
T.P., Empirical Analysis of Storm-Time Energetic
Electron Enhancements, Unviersity of California
Los Angeles, Los Angeles, 2001. 5. O'Brien, T.P.,
R.L. McPherron, D. Sornette, G.D. Reeves, R.
Friedel, and H.J. Singer, Which magnetic storms
produce relativistic electrons at geosynchronous
orbit?, Journal of Geophysical Research, 106
(A8), 15533-44, 2001. 6. Tsurutani, B. T., and
W. D. Gonzalez, The cause of high-intensity
long-duration continuous AE activity (HILDCAAS)
Interplanetary Alfven wave trains, Planet.
Space Sci., 35, 405-412, 1987. 7. Tsurutani,
B.T., and W.D. Gonzalez, The causes of
geomagnetic storms during solar maximum,
presented at Eos Trans. AGU, 1994. 8. Tsurutani,
B.T., W.D. Gonzalez, and Y. Kamide, Magnetic
storms, Surveys in Geophysics, 18, 363-383, 1997.
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Extras
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Motivation---some open questions in Solar Cycle
Variations in Storms

• Is there a difference between storms at solar
  minimum and maximum?
• Do solar minimum storms develop differently from
  solar-max storms?
• Do these storms last longer?
• Does the occurrence rate of substorms, SMC,
  Sawtooths in different phases of a storm change
  with solar cycle?
• Why are there more killer electrons at solar
  minimum?
• Why is there a strong semiannual and universal
  time variation in occurrence and size of storms
  at solar minimum?
• What physical effects are the cause of the
  semiannual variation in Dst?
• What effects do Alfen waves in high speed streams
  have on storms?

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