Space Weather using ground instrumentation

1. Space Weather using ground instrumentation Jean-Pierre Raulin Centro de Radioastronomia e Astrofísica Mackenzie, Universidade Presbiteriana Mackenzie, Escola de Engenharia, São Paulo, SP, Brazil Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

2. Space Weather Flares CMEs/Flares CMEs/Coronal Holes Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

3. Solar Flare Radio Emission at Very High Frequencies New Instruments are required in the GHz, THz to Infra-Red and Visible Ranges SST Models 2 systems operating at CASLEO and at CRAAM 45 & 90 GHz Patrol polarimeters SST 212 & 405 GHz SOLAR-T 3 & 7 THz Mid-IR GBO Ready to fly Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

4. 13/03/2012 solar event: 30 THz burst + WL + high-enery X-rays 30 THz WL FERMI 975-2000 keV FERMI 538-975 keV Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

5. Are the 30 THz impulsive component and WL part of the same emission process? - ~ 1 MeV electrons - deposit their energy between the surfave and the temperature minimum region ? Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

6. Ionospheric Disturbances Photons and/or energetic particles  ionization excesses  changes of the electrical conductivity VLF propagation anomalies  VLF phase and amplitude changes Solar: quiescent, Ly-, X-rays (flares), particles (SEPs); Non-Solar: X-rays, GRB, flares from SGR 70 – 90 km TGF Localized particle precipitation Few Mm Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

7. SAVNETCRAAM/EE 11 VLF tracking receiver stations deployed in Brazil, Peru , Argentina e México. 6 years of operation since 2007 • Long-term and transient solar activity (Ly- ; solar flares) • D Region absorption models • mesospheric disturbances (T, NO, O3) • Physics of the lower ionospheric (C/D) regions • Atmos. Physics (TGFs) • Subionospheric radio propagation modeling • Search for seismic-EM effects • Detection of Remote astrophysical objects Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

8. Solar Flare Detection Receivers Transmitters Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

9. Solar Flare Detection For this period of solar activity, the towest detected solar flare B 2.7  2.7 10-7 W/m2  all  B 4 Class events are detected with 100 % probability. Lowest SXR flare detected so far  B1.8 1 hour Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

10. Solar Flare Detection The minimum detectable soft X-ray flux is correlated with the averaged Lyman- flux : the higher the solar activity the higher Px Real-time monitoring of solar flares CASLEO, San Juan, Argentina 2 hours Valuable information for institutional, national or international Space Weather centers Lyman- solar radiation maintains the quiet ionospheric D-region (Nicolet & Aikin 1960) Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

11. THE IONOSPHERI C REGION C D daytime Mechtly et al., 1968, JATP nighttime E ~ 90 min. duration C region at ~ 65 km Origin: Cosmic rays ?? Origin: Ly- on O2 O on CO4- and NO3-  O2- and O  ozone + electron reservoir Indirect monitoring of the Lyman- solar radiation Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

12. SGR J1550-5418 on 2009, January 22 The same technique is used to study remote objects of great astrophysical importance. The fact that the nighttime ionosphere can be disturbed by moderate cosmic X-ray bursts, and not only by giant ones, indicates that the frequency of detection of such events could be improved, for example by increasing the coverage of existing VLF receiving networks, and performing a systematic search. The VLF detection of high-energy astrophysical bursts appears as an interesting observational diagnostic that complements their detection in space, in particular when space observations are not available, for example during Earth’s occultation or above the South Atlantic Anomaly region, or suffer from saturation. Simple burst Complex burst NPM-EACF NPM-ROI 20 ms VLF data Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria

13. The Embrace Network MCT / INPE / CEA – LAC – DSS - Programa EMBRACE

14. The Embrace Network BOA BLM 2014 MAN SLZ 2014 AFT EUS CBA PAL 2014 CGR CXB TCM JAT SMS CXP RGA SJC ECF MCT / INPE / CEA / DAE - IONO - Clezio Marcos De Nardin - clezio.denardin@.inpe.br

15. TEC Map over South America 1 map every 10 minutes MCT / INPE / CEA / DAE - IONO - Clezio Marcos De Nardin - clezio.denardin@.inpe.br

16. CONCLUSIONS For a better understanding of the (solar) flaring processes a complete description of the solar flare spectra are needed, sub-THz, THz, IR bands. The lower ionosphere plasma is a medium very sensitive to external and internal forcing: radiation, energetic particle fluxes, atmospheric variability, upper propagating waves. The VLF technique which uses very simple and cheap instrumental facilities has shown to be a very suitable tool to study many aspects of the Space Weather dynamics, as long-term and transient solar phenomena. The same technique can also be used to study remote objects of great astrophysical importance. The VLF detection of high-energy astrophysical bursts appears as an interesting observational diagnostic that complements their detection in space, in particular when space observations are not available, for example during Earth’s occultation or above the South Atlantic Anomaly region, or suffer from saturation. Existing arrays: combine the data; Extend existing arrays; Develop new arrays During SAVNET conception, fabrication, installation and operation (IHY and ISWI), many students were involved. Therefore, it is a great opportunity for under- and graduated (M, D) students to perform relevant researches in Space Sciences. Improving Space Weather Forecasting in the Next Decade, 51st Session of the Scientific and Technical Subcommittee of the Committee on the Peaceful Uses of Outer Space (COPUOS), 10-11 February 2014, Vienna, Austria