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7/29/2019 Plasma bubbles and scintillation over Brazil
1/21
CAWSES Activities
in BrazilJean-Pierre Raulin
CRAAM/EE/UPM
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Credits/Contributors
CRAAM/EE/UPM Center for RadioAstronomy
Astrophysics Mackenzie Engineering School
Presbyterian Mackenzie University
SAVNET - South America VLF Network
INPE National Institute for Space Research
EMBRACE INPE Space Weather program
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Space Weather-Dynamics of Space Environment (Solar flare,
CME and solar winds)
- Sources from BELOW (Convections and waveenergy propagations)
- South Americas singularity
1. Equatorial Ionospheric Anomaly and plasma bubbles
2. South Atlantic Magnetic Anomaly
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Solar radiation and high energy particles
(Solar flare, CME and solar winds)
EIT on SOHO LASCO-C3 on SOHO
CME: Coronal Mass Ejection
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Troposphericconvections
Plasma bubbles inthe ionosphere
Convections and wave energy propagations
Troposphere
Stratosphere
ThermosphereMesosphere
Upward Gravity wavepropagation
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Equatorial Anomaly and Plasma bubbles
TIMED/GUVI
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Geomagnetic Field intensity over
South America
Courtesy of National Observatory,
Brazil
SAMA region:
from 26,000 to 23,000 nT
in the last 100 years,
12 % of decrease
Figure: Protons and electron flux greater than 0.5 MeV in low
Earth orbit measured by the NASA/SAMPEX satellite.
SAMPEX (Solar Anomalous and Magnetospheric Particle
Explorer) (Source: www.aero.org)
South Atlantic Geomagnetic Anomaly
http://www.aero.org/http://www.aero.org/7/29/2019 Plasma bubbles and scintillation over Brazil
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1. Solar (flare and long-term) radiation, CMEOccurrence Monitoring, SEP events
Important for satellite operation
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Using Radio telescopes
Itapetinga Radio Telescope
(Atibaia) 21-90 GHz
SPUA - 12 GHz
7 GHz
1.2, 1.7, 2.8, 5.6 GHz
Brazililan Decimetric Arrray (Cachoeira Paulista)
BSS 1000-2500MHz
SPECMM 1-40 GHz
INPE/MACKENZIE
BDA
SST 212 & 405 GHzSolar Polarimeters
45 & 90 GHz
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All B4 (and higher events) are detected - Lowest detected solar flare B 2.7 2.7 10-7 W/m2
1 hour
Indirectly from their ionospheric impacts
10 examples of solar flares detected in the low ionosphere (phase measurements) and compared to GOES X-rays
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LONG-TERM SOLAR FORCINGof THE IONOSPHERE
Indirect solar Lyman- monitoring using the VLF technique
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7 8 MARCH 2011 SPE events
CARPET event
Solar Neutrons
SEP event effect in
the ionosphere ?
CARPET Muon detector
excesses
> 9.5 GeV primariy protons at
the top of the atmosphere
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2. Solar wind monitoring by Cosmicray (Muon) (Forbush decrease)
To get Information of:
Solar CME and high density solar wind
approach to the earth
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Cosmic ray monitoring by Mon detectorat So Martinho da Serra (29 S, 53 W), RS,
Brazil
Intensity deficitconfined in a cone
To predict Magneticstorm in 6-8 hours
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3. Ionospheric scintillation and TEC
Monitoring by GNSS receivers
To provide information for Telecommunications,
GNSS positioning system application
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Plasma bubbles and scintillation over Brazil
Equatorial Plasma Bubbles
Scintilation
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Spatial variability of TEC over Brazil
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SUPIM Ionospheric modelConstelao de satlites
GPS This simulation were
obtained from the SUPIM,a co-development of theAeronomy Division of theCEA/INPE with theUniversity of Sheffield andwith the computationalimprovements by theComputer Lab for SpaceWeather at the SSO/INPE
and by the Computer Labfor Mathematical and
Science at the ETE/INPE.
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EMBRACE:
INPE Space Weatherprogram
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Estudo e Monitoramento do
Clima Espacial (EMBRACE)
-http://www inpe br/climaespa
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EMBRACE: Data Collection and Flow
Santa Maria
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