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Signatures of July 14, 2000 on Satellites and Ground-Based Experiment

Signatures of July 14, 2000 on Satellites and Ground-Based Experiment. By Dr. A. Mahrous Helwan University - EGYPT. Our Collaborators. AGASA (Japan). Chacaltaya (Bolivia). What are Cosmic Rays ?. LHC at CERN (7 TeV) Protons. What is the Maximum Energy. 3R s.

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Signatures of July 14, 2000 on Satellites and Ground-Based Experiment

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  1. Signatures of July 14, 2000 on Satellites and Ground-Based Experiment By Dr. A. Mahrous Helwan University - EGYPT

  2. Our Collaborators AGASA (Japan) Chacaltaya (Bolivia)

  3. What are Cosmic Rays ? LHC at CERN (7 TeV) Protons

  4. What is the Maximum Energy 3Rs • The simulation shows that UHE photons with energies between 1019 and 1020.5eV start cascading in the Sun's magnetic field within three times radius of the Sun. • If we are trying to detect such cascading particles on the Earth with air shower arrays, these showers originated by a bunch of secondary particles developed in the Sun’s magnetic field should be detected within a solid angle: •  = 3Rs2 / 4D2S-E , Rs: Sun’s radius •  6.12  10-4 sr from the Sun's position. This means that the energy of the primary particles could reach1027 eV DS-E  FOR MORE INFO... Mahrous, A. & Inoue, N., Development of electromagnetic cascading in the Sun's magnetic field Astronomy and Astrophysics, v.386, p.308-312 (2002)

  5. Composition & Energy Spectrum GZK Low Energy CR : • SCR are dominant for energies < 1 GeV • - GCR are changing with Solar Activity Gamma High Energy CR : • The spectrum is almost a power low with index –3 • Slight steeping at 3x1015 eV (knee) • -Slight flattening at 3x1018 eV (ankle) • - Above 1020 eV, the flux is uncertain. The possible scenarios predicting Z-burst photons are dominant. Protons

  6. Possible Sources

  7. Air Shower Phenomena NCR + Nair 0 +  + K 0  2  = 8.4 x 10-17 s  +   = 2.6 x 10-8 s  + Nair e+ + e- “ Pair Creation” e + Nair e +  “Bremsstrahlung” FOR MORE INFO... Takeda,M., Sakaki,N, Mahrous,A., AGAS group “Energy determination in the Akeno Giant Air Shower Array experiment, Astroparticle Physics, Volume 19, Issue 4, p. 447-462 (2003).

  8. Cherenkov Detectors

  9. Super Kamiocande

  10. Variations of GCR Intesity

  11. 1- Pressure Variation • Pressure »» atmospheric density »» absorption of CR FOR MORE INFO... Mahrous,A. Inoue,N.,” Variation Of Forbush-Decrease Amplitude With Some Shock Parameters”, 35th COSPAR Scientific Assembly. Held 18 - 25 July 2004, in Paris, France., p.1910.

  12. 2- GEOMAGNETIC CUTOFF RIGIDITY • Pcut(,) : Geomagnetic cutoff • rigidity in GeV • Angle between incoming particle velocity and geomagnetic east-west direction •  Geomagnetic latitude Chacaltaya 12 GeV

  13. 3- Forbush Decrease Depression in the counting rate of cosmic rays. FD >> 30% & recov. Several days A : Amplitude of Forbush decrease Mechanism : The energetic solar phenomena>>disturbance in interplanetary magnetic field>>reduction in low energy CR intensity which detected on the Earth.

  14. Chacaltaya Experiment Purpose: Detection of Cosmic Rays with primary energy greater than 1014 eV Location:  Latitude= 16o 21´ South, Longitude=  68o 08´, Altitude= 5300 m   Area: The experiment covering a circular area of 50 m radius Working theory: The detection of CR depends on Air Shower phenomena

  15. Types of Detectors Construction of the density detector Distribution of different types of detectors at Mt.Chacaltaya experiment 40 scintillation detectors of area (0.25m2) & 4 detectors of area (1.0m2) used for detecting the electromagnetic and muonic components, with counting rate every 10 seconds.

  16. Distribution of burst detectors A photo and scheme diagram of neutron monitor at Mt. Chacaltaya The burst detector is a scintillation detector covered with 15 cm of lead. We have 32 detectors with area (0.25m2), which used for detecting the hadronic components and Muons The Type: 12NM64 Neutron Monitor It is used for detecting the neutron component with counting rate 1 minute

  17. This is the effect of CR on electronic devices ! Monitor system of Chacaltaya experiment

  18. Event of July 14, 2000

  19. What is going on the Sun ? What we detect on the Earth ?

  20. Chacaltaya Results The sequence of the plots is the deviation from the average of DD, NM and counting rate of BD. FIRST DECREASE >> July 13 (9:20 UT) Deviations of –2% & –5% for DD&NM Continued for 6h for DD & 13h for NM. SECOND DECREASE >> July 15 at (13:30 UT) Deviation of –6% & –10% for DD and NM Continued for 18h for DD and 17h for NM. STABILITYin the counting rate of NM during that second decrease for about 4h, which is called two-step FD.It is indicated with a small red circle and enlarged in the outer circle in the same figure. The counting rate of all the detectors returned to the normal state in July 19.

  21. SOHO Satellite Results The figure shows the CME observed by SOHO/LASCO coronagraph during that flare. The produced and largest flare occurred on the Sun in 2000 July 14, at (10:54 UT) was associated with a full-halo CME. The expansion speed of the loop-like structure (indicated with arrows) was about 2000 km/s, this means that the arrival time ofsuch CME to the Earth will be about 1.5 days, which will be verified from WIND satellite results in the next slide. 2000 km/s CME observed by C2 coronagraph of SOHO/LASCO in July 14, 2000 at 10:54 UT

  22. GOES Results The sequence of the plots is : (A) Proton flux in 7 channels covering the range “0.6~500 MeV”, (B) Plot of X-ray flux in (Watts/m2 in two wavelength bands, Xl=0.54 A and Xs=18 A. (C) The four magnetic field components: “Hp”parallel to the satellite spin axis, “He”parallel to the satellite-Earth center line and points earthward. “Hn”perpendicular to both Hp and He “Ht” is the transverse component. -Solar proton events occurred in July 14 at (10:40 UT), reached a peak at (16:10 UT), and ended in July 16 at (04:00 UT). -Occurrence of X-class X-ray flare in July 14, 2000 observed in both of the two-wavelength bands at (11:00 UT). -A large disturbance occurred in the magnetic field components, which varied from positive 200 to negative 200 nT in July 15 at (19:00 UT).

  23. WIND Satellite Results • THE DETECTED SHOCKS : • S1 >> Date : July 13 at (09:13 UT) • V: 600 km/s • P: 10 P cc-1 • - S2 >> Date : July 13 at (10:12 UT) • V: 650 km/s • P: 15 P cc-1 • - S3 >> Date: July 14 at (15:32 UT) • NO DATA (detector saturation) • - S4 >> Date : July 15 at (14:15 UT) • V: 950 km/s • P: 50 P cc-1

  24. How can we understand Chacaltaya results ? FIRST DECREASE>> July 13 (9:20 UT) SECOND DECREASE>> July 15 at (13:30 UT) STABILITYin the counting rate of NM during that second decrease for about 4h, FIRST DECREASE >> S1&S2 SECOND DECREASE >> S4 STABILITY >> E1

  25. why we have one-step FD in July 13 and two-step FD in July 15 detected by NM ? July 15 July 13 Assuming the produced shock and its driver ejecta are moving towards the Earth. In case of theone-step FD observed in 2000 July 13, the position of the Earth was at the point “A”, at which,only the shock is passing through the Earth. In that case, the passing cosmic rays will suffer only one-step attenuation due to shock. On the other hand, as the case of thetwo-step FD detected in 2000 July 15, the position of the Earth could be at the point “B”, at which,both the shock and its driver ejecta is passing through the Earth. As the result, cosmic ray intensity will be reduced by two different levels of attenuation, one from the shock, and the other from the ejecta. Moreover, the time difference between such two levels of attenuation actually represents the thickness of the ejecta itself.

  26. Future of CR

  27. EUSO Mission

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