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Carrington, 1859

CARRINGTON, CHAPMAN AND OTHER GIANTS (Von HUMBOLDT, MAUNDER, CHREE AND BARTELS): HAVE WE ASSIMALATED ALL THEY TOLD US ABOUT SPACE WEATHER? Bruce T. Tsurutani* Jet Propulsion Laboratory California Institute of technology Pasadena, California 91109

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Carrington, 1859

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  1. CARRINGTON, CHAPMAN AND OTHER GIANTS (Von HUMBOLDT, MAUNDER, CHREE AND BARTELS): HAVE WE ASSIMALATED ALL THEY TOLD US ABOUT SPACE WEATHER? Bruce T. Tsurutani* Jet Propulsion Laboratory California Institute of technology Pasadena, California 91109 *Collaborators: W.D. Gonzalez, G.S. Lakhina, E. Echer and O.P. Verkhoglyadova

  2. CarringtonMNRS, 1859 Carrington, 1859

  3. “Description of a Singular Appearance seen in the Sun on September 1, 1859” By R.C. Carrington, Esq. (MNRA, 20, 13, 1859) “Mr. Carrington exhibited at the November meeting of the Society and pointed out that a moderate but very marked disturbance took place at about 11:20 AM, September 1st, of short duration; and that towards four hours after midnight there commenced a great magnetic storm, ……….” “While contemporary occurrence may deserve nothing, he would not have it supposed that he even leans towards hastily connecting them. “One swallow does not make a summer”. “ Carrington gave us gave us information to determine the average speed of the CME. It was not “politically correct” to relate solar and geomagnetic phenomena at the time (due to Lord Kelvin) . .

  4. The October 28 , 2003 “Halloween” AR

  5. The 1972 Event

  6. Big Solar Events • Some “big solar and interplanetary events” are the Carrington 1859 flare, the August 1972 event and the Halloween 2003 events. What do they have in common? • All flares were associated with magnetic ARs. • All took place after solar maximum. • See Svestka ASR, 1995

  7. > X10 flares N. Gopalswamy, personal comm., 2009

  8. Large flares tend to occur late in a solar cycle (Svestka ASR 1995; Gopalswamy, personal comm., 2009). How to explain the above: there might be more beta-gamma-delta regions (Kuenzel, AN, 1960; Sammis, Tang and Zirin, ApJ 2000) in this phase? (M. Wheatland, personal comm., 2009) A plus: the ARs would be closest to the equator (J. Harvey, personal comm., 2009).

  9. Total Energy from Solar/Stellar Flares September 1, 1859 Flare E = possibly 1032 ergs (K. Harvey, personal comm., 2001) Is This The Most Energetic Flare? August 1972 Flare E ≈ 1032 – 1033 ergs (Lin and Hudson, Sol. Phys., 50, 153, 1976) June 1, 1991 Flare E ≈ 1034 ergs (Kane, et al., Astro. J., 446, L47, 1995) What is the Maximum Flare energy? E = 1035 ergs? (See Schrijver, ASR, 2009)

  10. Is Solar Flare Energy the Most Important Parameter (for magnetic storms)? • Answer: not necessarily

  11. Gonzalez et al., GRL 1998 The most important quantity is the interplanetary electric field: E =V x B ~ V2 Max Vsw = 3000 km/s? Gopalswamy et al. JGR 2005 GoVnzalez et al. GRL, 2001

  12. The Sept 1-2 1859 Carrington Storm

  13. Low-latitude Auroras: The Magnetic Storm of 1-2 September 1859 D.S. Kimball (University of Alaska), 1960 “Red glows were reported as visible from within 23° of the geomagnetic equator in both north and south hemispheres during the display of September 1-2” D.S. Kimball, a colleague of S. Chapman wrote a comprehensive detailed report of the aurora during the Carrington storm (it is a GI/Univ. Alaska “internal report”).

  14. “Hand” measurements taken from a Grubb magnetometer. The magnetometer was “high technology” at the time and the manual for calibration does not have a sketch of it.

  15. From a plasmapause location of L=1.3 (auroral data: Kimball, 1960), we can estimate the magnetospheric electric field. The electric potential (Volland, 1973; Stern, 1975; Nishida, 1978) for charged particles is: Where and are radial distance and azimuthal angle measured counterclockwise from solar direction M – dipole moment - particle charge and magnetic moment Therefore: Modern day knowledge plus older observations allowed us to estimate the storm E field

  16. Extreme Magnetic Storm of September 1-2, 1859 • The storm was the most intense in recorded history. Auroras were seen from Hawaii and Santiago. • SYM-H is estimated to be ~ -1760 nT, consistent with the Colaba local noon response of ΔH = 1600 ± 10 nT • (In recent years we have only had the 1989 storm : Dst = -589 nT)

  17. Is this the most intense storm that has taken place? Ans: Most probably not. Maximum Magnetic Storm Intensity? Dst ~ -2500 nT (Vasyliunas, 2008)

  18. Have there been other recent events that might have surpassed the 1859 event under different conditions? Ans: Yes

  19. THE AUGUST 1972 SUPER FLARE/ICME • The ICME took only 14 hours to reach the Earth (Vsw = 2850 km/s. Vaisberg and Zastenker, 1976; Zastenker et al., 1978). The 1859 ICME took 17 hrs to reach 1 AU.

  20. MC: R. Lepping, private comm., 2005 4 major Bs intervals Tsurutani et al. JGR 1992

  21. 3 storm main phases Geomagnetic Quiet Storm main phase Removal of the radial and corotational delays indicate that the Pioneer 10 Bz features and geomagnetic activity at Earth line up.

  22. INTERPLANETARY EVENT OF 7-8 NOVEMBER, 2004: AR ASSOCIATION Two reverse waves 3 Forward Shocks Tsurutani et al., GRL, 2008

  23. CAN WE PREDICT WHEN THE NEXT ONE WILL OCCUR IN A STATISTICAL SENSE? Predictions of greater intensity magnetic storms requires either: 1) full understanding of the physical processes involved, or 2) good empirical statistics of the tail of the energy distributions. • The statistics for extreme events are poor. We are making progress on understanding physical limitations. Cannot predict tail distributions

  24. What Would the Consequences Be if a 1859-type ICME Hit Today?

  25. 1989 Storm Consequence

  26. ESW B Plasmasheet VSW Prompt Penetration Electric Fields(PPEFs) and Their Effects: A Global Scenario Positive Ionospheric Storm Initiation of the Magnetic Storm RC Negative Ionospheric Storm Tsurutani et al., JGR, 2004

  27. h (km) Quiet 300 106 Log N (cm-3) h (km) 300 106 Log N (cm-3) Creation of a new ionosphere: TEC enhancement Uplifted plasma moved to region of lower recombination time scales Solar photoionization creates a new ionosphere

  28. TheOct 30-31, 2003 Superstorm CHAMP GPS Dayside Ionospheric Superfountain Mannucci et al. GRL 2005 Mannucci et al. GRL, 2005 Mannucci et al. GRL 2005

  29. Satellite Drag With O+ ions being rapidly uplifted, one can expect corresponding uplift of neutrals by drag forces (ion-neutral drag). For the October 30-31 superstorm neutral densities at ~370 km altitude could be increased by up to 60% of the quiet time values and that at ~600 km by up to a factor of 7. Precipitation in the auroral zones lead to enhanced ionospheric heating and increased satellite drag (Thayer et al., GRL, 2008). These two effects should be modeled for an 1859 type storm.

  30. Effects During the Carrington Storm Arcing from exposed wires set fires. Unpowered telegraph lines carried signals (Loomis, Am. J. Sci., 1861) Everything was “low tech” at the time. Effects Today? Today one could certainly expect outages of major power grids (Severe Space Weather Events, NRC Workshop report, Nat. Acad. Press, 2008). MEO and GEO Satellites disabled, LEO satellites deorbited (Odenwald et al., ASR 2006). Loomis, Am. J. Sci., 1861

  31. Thank you very much for your attention.

  32. Some Reflection on Works Done by Von Humboldt, Maunder, Chree and Bartels • Recurrent (~27 day) geomagnetic activity: Maunder (1904) • Put on a sound mathematical basis: Chree (1912) • “Invisible” magnetically active regions, “M-regions”: Bartels (1934) • “Magnetisches Ungewitter”, Von Humboldt (1810)

  33. DECLINING PHASE OF SOLAR CYCLE Coronal hole

  34. THE SOLAR WIND DURING THE DECLINING PHASE OF THE SOLAR CYCLE HSSs Large polar coronal holes McComas et al. GRL 2003

  35. Nonlinear( ΔB/B ~ 1-2) Alfvén waves Tsurutani et al., Nonl.Proc. Geophys., 2005

  36. BS Bs HILDCAA Tsurutani and Gonzalez, PSS, 1987

  37. Chorus due to Injection of T┴/T|| > 1 Anisotropic 10-100 keV Electrons Tsurutani et al., Wave Inst. Spa Plas., 1979

  38. Chorus “element” duration ~ 0.1 to 0.5 s Burton and Holzer JGR 1968

  39. High-speed stream HILDCAA Tsurutani et al., JGR, 2006

  40. Relativistic ~400 keV electrons Chorus PC5s Tsurutani et al., JGR 2006

  41. >30 keV electrons 2.5 Mev electrons Chorus Kasahara et al. GRL 2008

  42. 2-6 MeV electron peak occurrence occurs in solar cycle declining phase when HSSs dominate D. Baker, 2006

  43. The energy input into the magnetosphere can be higher during the declining phase of the solar cycle than during solar maximum ~25 day HILDCAAs CIR storm “recovery” phases can last ~25 days Tsurutani et al., JGR, 1995

  44. Kozyra et al. 2006

  45. Our scientific “giants” could not have envisaged the long chain of physical connections: M-regions, high speed solar wind streams, embedded Alfvén waves, magnetic reconnection at Earth, nightside plasma injections, chorus and PC5 wave generation, relativistic electron acceleration, NOx production, and Ozone destruction.

  46. THE END

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