Virtual Solar Observatory
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1 Virtual Solar Observatory Adriana V. R. Silva CRAAM/Mackenzie Joaquim E. R. Costa DAS/INPE BRAVO Workshop 5-Feb-200
2 Summary Brazilian solar initiative The Virtual Solar Observatory (USA) Observatories and databases: ROI, SST Proposed applications: Magnetic field extrapolation Flare spectra modeling Solar atmosphere model
3 The Virtual Solar Observatory (USA) Browser query interface offers multiple search methods, including combinations GUI allows sorting by columns, viewing of thumbnails (where available) Gurman et al.
4 VSO Since 12/ Search by: Time Observable Instrument/Source/Provider Spectral range Nickname
5 Instruments 512-CHANNEL MAGNETOGRAPH 60-FT SHG BCS - Yohkoh BIG BEAR CDS CELIAS CERRO TOLOLO CFDT1 CFDT2 CHP COSTEP DPM EIT - SOHO EL TEIDE ERNE GOLF HXT - Yohkoh IMPACT LASCO SOHO LEARMONTH - GONG MAUNA LOA MK4 MOF/60 MOTH O-SPAN OVSA PLASTIC RHESSI S/WAVES SECCHI SOLAR FTS SPECTROMETER SPECTROHELIOGRAPH SPECTROMAGNETOGRAPH SUMER SWAN SXI-0 SXT - Yohkoh TENERIFE UDAIPUR UVCS VIRGO VSM
6 Search and Selection Search by data source and observatory or instrument
7 Search and Selection Or by physical observable
8 Search and Selection Or by wavelength or frequency
9 Search and Selection Or by nicknames, commonly used names for specific data types
10 Search and Selection Or by combination of search methods
11 Example Search by: Time interval (default) Nickname = EUV image (wavelength range) Physical Observable = Intensity
12 Search results Shopping cart: data request Delivery method (depends on data provider): or link
13 Multi-frequency data from different Observatories: 12, 22, 48, 212 & 405 GHz; Probe different heights in the atmosphere: emission at higher radio frequencies originate deeper than that at lower freqs. determine temperature and density of various layers of the solar atmosphere; Time profiles of flux density for flares; Flare spectra: emission mechanism, energetic particle population, magnetic field, etc; Maps/images: active regions, limb brightening, coronal holes, etc. The Brazilian Virtual Solar Observatory
14 Database
15 Database 12 GHz Radio Observatory of Itapetinga (ROI), in Atibaia, SP; Patrol telescope; Flux density of solar flares and position in heliographic coordinates daily from UT; Temporal resolution of 100 ms, spatial resolution of 30 arcsec, and sensitivity of 1 sfu; Real time international alert for microwave burst occurrence.
16 Burst location 12 GHz Measured flux density in the three antenna allows for location of the burst. Information used for pointing of other telescopes for burst observation.
17 SPUA Solar Patrol Un-phased Array Monitoring and alert of solar bursts at 12 GHz
18 Database 22 & 48 GHz ROI (Atibaia, SP) Observing campaigns Flux density of solar flares with 0.01 sfu sensitivity and temporal resolution of 1 ms.
19 Maps/Images 22 & 48 GHz Maps at both frequencies composed of raster scans Images of the solar chromosphere: observe bright active regions and dark coronal holes.
20 Database 212 & 405 GHz Submm Solar Telescope (SST), at CASLEO Obs. Argentina at 2500 m Since 1999 Flare observations and daily maps of the Sun 4 receivers at 212 GHz and 2 receivers at 405 GHz 5 ms temporal resolution
21 Solar maps 212 & 405 GHz (Silva et al. 2006) 4500 Solar maps at each frequency; Study: Quiet Sun s atmosphere Active regions Improve models of the atmosphere; Infer magnetic fields of AR.
22 Flare 212 & 405 GHz Time profile evolution Spectra emission mechanism Position (centroid) (Kaufmann et al. 2004)
23 S.A.G.U.I. Solar Analysis Graphical User Interface Software developed for data visualisation, extraction, and calibration. Data from ROI and SST.
24 Solar Maps
25 Applications
26 1) Magnetic field topology Extrapolation of cromospheric/coro nal magnetic field lines From photospheric line-of-sight magnetograms from MDI/SOHO.
27 2) Flare spectra Spectral analysis of microwave cm-mm solar bursts with gyrosynchrotron emission from general energy/pitch angle distributions. Thermal relativistic and nonthermal (simple or multi-power law) energy distribution is included. Radiation transfer is included in 3D topology of the magnetic field. (Simões and Costa 2006)
28 3) Model of the solar atmosphere Temperature and density distributions Based on 17 GHz maps from NoRH (Japan): measurement of the radius and limb brightening. Extend and improve the model including maps at 22, 48, 212, and 405 GHz. FAL-C Zirin Model FAL-C Zirin Model
29 The Brazilian Virtual Solar Observatory Database: Multi-frequency data from different observatories: 12, 22, 48, 212 & 405 GHz; Time profiles of flux density for flares; Maps/images of the Sun. Application: Magnetic field reconstruction; Flare spectra; Solar atmosphere model.
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