LOW FREQUENCY ARRAY LOFAR INTERPLANETARY SCINTILLATION IPS SCINTILLATION

LOW FREQUENCY ARRAY (LOFAR) INTERPLANETARY SCINTILLATION (IPS) SCINTILLATION INDEX (AND GLEVELS) FOR THE FIRST TIME. OYUKI CHANG (1), AND MARIO M. BISI (1), AND RICHARD A. FALLOWS (2). (1) RAL SPACE, UK RESEARCH AND INNOVATION – SCIENCE & TECHNOLOGY FACILITIES COUNCIL – RUTHERFORD APPLETON LABORATORY, HARWELL CAMPUS, OXFORDSHIRE, OX 11 0 QX, UK (2) ASTRON – THE NETHERLANDS INSTITUTE FOR RADIO ASTRONOMY, POSTBUS 2, 7990 AA DWINGELOO, THE NETHERLANDS

© 2019 RAL Space Worldwide IPS Stations (WIPSS) Network Pushchino 111 MHz 70, 000 ㎡ High-Band Tiles 110 to ~250 MHz. ISEE Multi-Station 327 MHz 2000 ㎡ × 3, 3500 ㎡ MEXART 140 MHz、10, 000 ㎡ Mexico Low-Band Dipoles ~10 to 90 MHz. Japan Russia UK/Europe – EISCAT/LOFAR WIPSS India Ooty 327 MHz、 16, 000 ㎡ South Korea MWA 80 -300 MHz (USA-Australia)

INTERPLANETARY SCINTILLATION INDEX (M)

G-LEVEL

THE LOW FREQUENCY ARRAY (LOFAR)

FILTERING THE INSTRUMENTS AND SOURCES

M-INDEX VALUES BY INSTRUMENT

M INDEX VALUES PER DAY

THE EFFECT OF THE SIGNAL/NOISE RATIO

SUMMARY • THE M INDEX AND G-LEVELS FROM LOFAR WERE CALCULATED FOR THE FIRST TIME. • AN AUTOMATIC FILTER FOR GOOD SPECTRA HAVE TO BE CREATED. • M INDEX DEPENDENCE: INSTRUMENT (S/N RATIO), SOURCE SIZE, FREQUENCY AND ELONGATION. • G LEVEL IS TOO SENSITIVE TO THE INSTRUMENT AND CAN’T BE COMBINED EASILY. • MODULATION OF M INDEX (G LEVEL) IS NOT SIMPLE FOR SPACE WEATHER PROPOSES.

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M-INDEX TIME RESOLUTION 3 C 299 28/10/2016 3 C 298 27/10/2016

FILTERING SPECTRA - 3 C 287

FILTERING SPECTRA – CS 002 HBA 0

FILTERING SPECTRA - 3 C 267 IONOSPHERE?

FILTERING SPECTRA - 3 C 273

FILTERING SPECTRA – CS 002 HBA 0

FILTERING SPECTRA - 3 C 208

FILTERING SPECTRA - 3 C 286