Max Millennium Program

Collaborating Ground Based Observatories

  • Alfred University
  • Baikal Solar Vacuum Telescope
  • Big Bear Solar Observatory
  • Brazilian Solar Spectroscope
  • Carl Sagan Observatory
  • Catania Astrophysical Observatory
  • Crimean Astrophysical Observatory
  • H-alpha Solar Telescope for Argentina (HASTA)
  • Hida Domeless Solar Telescope
  • Hiraiso Solar Terrestrial Research Center
  • Huairou Solar Station
  • Itapetinga Radio Observatory
  • IZMIRAN Heliophysical Laboratory
  • IZMIRAN Solar Radio Laboratory (LaRS)
  • Kanzelhöhe Solar Observatory
  • Kharkov Astronomical Observatory
  • Kitt Peak, NSO US
  • Kodaikanal Observatory
  • Larissa Observatory
  • Marshall Space Flight Center
  • Mauna Loa Solar Observatory
  • Mees Solar Observatory
  • Meudon Observatory
  • Mirror Coronagraph for Argentina
  • Mitaka Solar Observatory, NAO Japan
  • Nançay Radioheliograph
  • Nobeyama Radioheliograph
  • Norikura Solar Observatory, NAO Japan
  • Ondrejov Observatory
  • Oporto Radiospectrograph
  • Owens Valley Solar Array
  • PHOENIX Radio Spectrometer
  • Potsdam Solar Radio Astronomy Group
  • Prairie View Solar Observatory
  • RATAN 600 Radiotelescope
  • Sacramento Peak, NSO US
  • San Fernando Observatory
  • Siberian Solar Radio Telescope
  • Solar Optical Observing Network
  • Solar Radio Burst Locator
  • Trieste Solar Radio System
  • Udaipur Solar Observatory
  • All Ground Based Solar Observatories

    Alfred University 
    Contact: F. David Toot, Alfred University
    Type of Observation: Goals: Instrument Setup:
    H-alpha  high temporal and spatial resolution imaging. Study chromospheric response to electron precipitation at high time resolution Field of view 10x10 arcmin. H-alpha center line imaging at video cadence, using 0.6 A filter.
    Baikal Solar Vacuum Telescope 
    Contact: Natalia Firstova, ISTP
    Type of Observation: Goals: Instrument Setup:
    H-alpha polarization with high spatial and temporal resolution optical spectrograms (not filtergrams). Temporal, spatial and spectral distribution of impact polarization during solar flares in H alpha; Spectropolarimetric observations of pores, filigree with high spatial and spectral resolution BSVT - 760 mm aperture, 40 m focal length, spectrograph with two camera mirror (f1=9.5 m, f2=14m); spatial dispersion 0."24/pixel, 0."37/pixel, detector- CCD camera TEK 512*512
    Big Bear Solar Observatory
    Contact: Haimin Wang, NJIT
    Type of Observation: Goals: Instrument Setup:
    Magnetograms (vector), H-alpha high resolution imaging Obtain vector magnetic field measurements over entire active region with 0.5" image scale, and corresponding H-alpha coverage 10" center bench, video- magnetograph; 26" east bench, H-alpha center line
    Full-disk H-alpha Coverage of all active regions, filaments, etc. Singer Telescope,  Kodak MegaPlus CCD, about 1 arcsec per pixel
    High time resolution flare imaging in D3, H-alpha Obtain chromospheric diagnostics in H-alpha and D3, to study the chromospheric response to electron precipitation 10" east bench, fast (10 ms) He D3 observations of precipitation kernels (2.1 x 2.1 arcmin field of view); 26" benches, H-alpha center line, +0.6 A, and -0.6 A
    Brazilian Solar Spectroscope
    Contact: Francisco Fernandes, INPE
    Type of Observation: Goals: Instrument Setup:
    Broadband spectral radio observations Observations of radio emissions, in particular decimetric bursts and fine structures (type III, spikes, patches) as a diagnostics of the particle acceleration process and of  plasma emission. Full disk, high time and spectral resolutions, with 9 m diameter antenna, in the interval 200-2500 MHz, with rrequency resolution 3 MHz and time resolution: 10 - 1000 ms.
    Carl Sagan Observatory
    Contact: Antonio Sanchez-Ibarra, USON
    Type of Observation: Goals: Instrument Setup:
    Active region, filaments and prominences at H-Alpha imaging and chromospheric plages with Calcium imaging. Obtain daily from 15 to 23 hrs UT continuous CCD high resolution video recording and live webcast of active regions, filaments, and prominences with 1/30 s temporal resolution and imaging of events in progress simultanously with H-Alpha and Calcium filters.   Twin aphocromatic refractors 16 cm with Coronado H-Alpha and Calcium filters and CCD video cameras.  
    Catania Astrophysical Observatory
    Contact: Francesca Zuccarello, Catania University
    Type of Observation: Goals: Instrument Setup:
    Full Disk H-alpha images; Full Disk WL images; High time resolution flare imaging in H-alphaTo obtain a good temporal coverage of the solar disk in photosphere and chromosphere; to study the global evolution of active regions, the dynamic of H-alpha filaments and the response of the low solar atmosphere to electron precipitation during a flare event; to study phenomena occurring before flares (precursors) in the framework of Space Weather researches. Cook refractor to make daily drawings of sunspot-groups from visual observation 150 - mm refractor (230 cm focal length) with an H-alpha Lyot filter (bandwidth of 0.25 or 0.5 Å), and a 1360 x 1200 Astromed TE4 CCD array with a dynamical range of 16 bits.
    Crimean Astrophysical Observatory
    Contact: Nataly Stepanian, CRAO
    Type of Observation: Goals: Instrument Setup:
    Full-disk magnetograms (line of sight) and Dopplergrams; optical spectra. Obtain daily full-disk solar magnetograms seen in chromosheric Na D1-D2 lines, and monitoring of the solar velocity and brightness with 30-second cadence; Obtain daily images of active regions in the HeI line 1083nm and spectra  in  the  range  390-1084 nm to study physical conditions in active regions before and after solar flares. Regular observations with magneto-optical filter in Na D1-D2 lines, spatial resolution 4.5 arcsec, time resolution 30 seconds; Echelle  spectrograph  for  spectral range 390-660 nm and spectrophotometer for infrared observations.
    High resolution  H-alpha imaging and polariimetry Study nature of linear polarization of H-alpha flare emission Spectral (and may be monochromatic) observations with linear polarization analyzer
    H-alpha Solar Telescope for Argentina (HASTA) 
    Contact: Marta Rovira, IAFE
    Type of Observation: Goals: Instrument Setup:
    Full disk H-alpha imaging  High temporal and spatial observations of flares, eruptive prominences and coronal mass ejections  1.5" spatial and 3 sec temporal resolution in H-alpha (6563 A) 
    Hida Domeless Solar Telescope
    Contact: Hiroki Kurokawa, Kyoto Univ.
    Type of Observation: Goals: Instrument Setup:
    High-resolution H-alpha and broad-band  optical imaging Study flare energy build-up processes: new flux emergence and magnetic shear developments.  Study flare trigger mechanism: new flux emergence, filament eruption High resolution imaging with the Domeless Solar telescope (DST) H-alpha 0.0,  H-alpha +0.8, H-alpha -0.8 images: 10 G-band sunspot images: 30s cadence
    High time resolution H-alpha imaging Study rapid developments of electron- bombarded footpoints of flare loops. High resolution imaging with the DST H-alpha -1.0 A and G-band images: 1/30s cadence
    Hiraiso Solar Terrestrial Research Center
    Contact: Maki Akioka, CRL
    Type of Observation: Goals: Instrument Setup:
    H-alpha full disk Doppler imaging Obtain full disk H alpha dopplergram with 2K by 2K CCD to observe the chromospheric dynamics and filament eruption at flare and CME. H alpha center, +0.7A, -0.7A and continuum images are taken every three minutes. Passband of Lyot filter is set at 0.25A. Close-up imaging of target active region with higher cadence is also available in parallel. 
    Huairou Solar Observing Station
    Contact: Honqui Zhang, BAO
    Type of Observation: Goals: Instrument Setup:
    Vector magnetograms, Doppler  maps, H alpha images  Obtain vector magnetic field measurements and corresponding H-alpha images of target active regions FeI 5324 A vector magnetograms, 0.75 A from line center, typical temporal resolution 5 min and spatial resolution 2 arcsec. 
    Itapetinga Radio Observatory
    Contact: Emilia Correia or Pierre Kaufmann , CRAAM
    Type of Observation: Goals: Instrument Setup:
    High time resolution polarimetry, mm and IR Time variations of the  polarization degree in association to the fast structures present in the intensity profiles of bursts Instrument characteristics: frequency observation: 7 GHz, full Sun, sensitivity less than 0.5 sfu, 20 ms time resolution, circular polarization modes (R and L)
    IZMIRAN Heliophysical Laboratory
    Contact: Boris Ioshpa, IZMIRAN
    Type of Observation: Goals: Instrument Setup:
    Active region vector magnetograms and velocity maps Observe simultaneously the longitudial magnetic fields and radial velocity in the FeI 5253A line and  the radial velocity in nonmagnetic FeI 5567A line. Obtain some magnetic and velocity maps throughout the day with the rate one map per half hour - one hour (rate depends on size of region and number of maps), provide analyzed magnetogram data for extrapolations.  Longitudial magnetograph taken in Fe I (5253 A),  one magnetogram and velocity map (with the compensation of 5-min oscillations) every half hour;  tachometer in the nonmagnetic FeI 5567A line.
    IZMIRAN Solar Radio Laboratory (LaRS)
    Contact: Roman Gorgutsa or Alexander Gnezdilov, IZMIRAN
    Type of Observation: Goals: Instrument Setup:
    Broadband radio (meter) spectral observations and fixed frequency radio (meter and centimeter) observations. Daily patrol of meter solar radio bursts and noise storm dynamic spectra with high enough time and frequency resolution, supplemented by intensity measurements at fixed frequenies in meter and centimeter range. Digital solar meter radio spectrograph 25 - 270 MHz (the frecuency range is scanned 25 times per second) and fixed frequency radiometers 169 MHz, 204 MHz and 3000 MHz (time resolution 1 sec). Daily patrool observations 06 - 12 UT (07 -12 UT since November to March
    Kanzelhöhe Solar Observatory
    Contact: Wolfgang Otruba, KSO
    Type of Observation: Goals: Instrument Setup:
    Full-disk H-alpha imaging, NaD intensitygrams, magnetograms and white light photoheliograms Obtain full-disk H-alpha images in several spectral bands and full-disk magnetograms for monitoring the activity level of the Sun With the solar patrol telescope H-alpha images are obtained at a cadence of 1 minute. A tunable Lyot-filter (FWHM=0.07 nm), a high-speed 1K x 1K CCD camera (8 bit) and a high-resolution 2Kx2K CCD camera (14 bit) are used. Full-disk magnetograms and intensitygrams are obtained with the magneto-optical filter (MOF) operated in the Na-D line with a cadence of 1 image set per minute. Image size is 512 x 495 pixels (2 bytes). Additonally we obtain a daily sunspot drawing and a white light photoheliogram.
    Kharkov Astronomical Observatory
    Contact: Gennady Marchenko, Kharkov State U
    Type of Observation: Goals: Instrument Setup:
    Active region and flare in the He 10830 and Balmer continuum To obtain images in the He 10830 and Balmer continuum during of flare evolution. Full disk images with ~8" resolution in He 10830 and Balmer continuum and precontinuum; one image every 5-10 minutes.
    Kitt Peak (U S National Solar Observatory)
    Contact: Jack Harvey, NSO
    Type of Observation: Goals: Instrument Setup:
    Full-disk magnetograms (line of sight), multichannel optical images. Obtain context observations  and high-resolution monitoring of active region magnetic development at chromospheric heights Regular full disk synoptic observations in the morning (1400-1700 UT -- photospheric and chromospheric magnetogram and 1083 nm spectroheliogram); high-rate chromospheric longitudinal magnetograms (rate depends on size of region)
    Multichannel Doppler He 10830 narrow-band spectroheliograms Put active filament observations in the context of what we know from other observations about the helicity of the region and the eruption. Scan in the red and blue wings of helium 10830 with a repeat rate of about 2 min for at least four hours per day
    Kodaikanal Observatory
    Contact: K. M. Hiremath, Indian Institute of Astrophysics
    Type of Observation: Goals: Instrument Setup:
    Flaring active region Monitor sunspot motion associated with flares; monitor chromospheric activity in H-alpha & Ca-IIK line Photoheliograph in white light at time resolution of every one hour with the help of 6 inch refraction telescope and spectroheliograph in H-alpha & Ca-IIK line center with 1 min time resolution
    Larissa Observatory
    Contact: Nick Stoikidis, Director
    Type of Observation: Goals: Instrument Setup:
    Flaring active region Monitor chromospheric activity in H-alpha & Ca-IIK line A refractor telescope f/15 with diameter of lens 16 cm and focal length 2400 mm, a Hale Ha filter (6563 A* with wings +- 0.5A* until +-1A* at red and blue) and a 1616 XTE CCD camera of Meade.
    Marshall Space Flight Center
    Contact: Mitzi Adams, MSFC
    Type of Observation: Goals: Instrument Setup:
    Magnetograms (vector) and high-resolution H-alpha images Provide shear analyses of vector magnetograms taken near 1300 UT to aid in target selection; Obtain vector magnetograms of target active region throughout day; provide analyzed magnetogram data for extrapolations, electric current calculations; provide co-aligned H-alpha coverage of active region Magnetograph--6x6 arcmin field of view with 3.2" resolution, taken in Fe I (5250.22 A), fastest cadence one magnetogram every 7 minutes (vector magnetograms and shear maps available on web). H-alpha, co-aligned with magnetograph, 1/2 A bandpass, 3 images per magnetograph image. Video rate recording is possible.
    Mauna Loa Solar Observatory
    Contact: Joan Burkepile, HAO
    Type of Observation: Goals: Instrument Setup:
    Full-disk H-alpha, Full-Limb H-alpha and white light Obtain coronal structure and large-scale eruptions/restructuring associated with flares/CMEs. Halpha disk and limb images (every 3 minutes between ~17:00 and 22:00) and white light coronal images (~1.1 to 2.7 Rsun every 3 minutes)
    Mees Solar Observatory
    Contact: Jeff Kuhn, IfA
    Type of Observation: Goals: Instrument Setup:
    Magnetograms (vector), Stokes Polarimetry Record the evolution of magnetic fields and structure.  IVM vector magnetic field movies (2 min. cadence, 0.5 arcsec pixels, 4.5 x 4.5 arcmin FOV) , Haleakala Stokes Polarimeter
    H-alpha multichannel imaging spectroscopy Spectral diagnostics of chromospheric heating. MCCD H-alpha imaging spectra, using the KPR01 program to study preflare and eruptive events if the major flare probability stays low, but switching to the JPW05 program if major flares are likely. These have similar spectral and spatial resolutions, but JPW05 uses a smaller FOV to gain higher cadence (10-20 sec)
    Full disk white light, full limb H-alpha coronagraph Image registration, large-scale eruptions. Small stand-alone telescope and camera.
    Meudon Observatory
    Contact: Jean-Marie Malherbe, Observatoire de Paris
    Type of Observation: Goals: Instrument Setup:
    Full disk H-alpha imaging and Doppler Obtain chromospheric context observations of active region development Full disk observations in H-alpha center line, +0.5 A and -0.5 A, with 1 min time resolution, 2" pixel size.
    Flare multichannel spectroscopy H-alpha line profile changes in 2D; study the dynamics of active regions and flares Solar Tower, multichannel spectrograph with 9 simultaneous 2D channels, at 0.25 A resolution, with 8' x 5' field of view, 0.5" pixel size, 1 minute time resolution
    H-alpha polarimetry Study impact linear polarization during solar flares in H alpha Stokes parameters integrated over the H alpha profile
    Mirror Coronagraph for Argentina 
    Contact: Guillermo Stenborg, MPAe
    Type of Observation: Goals: Instrument Setup:
    Full Limb coronal and flare imaging  High time resolution observations of transient phenomena, structure and evolution of prominences and streamers MICA observes the solar corona above the limb (from 1.05 to 2.0 solar radii from Sun center) in various spectral ranges (5303, 6374, 6563)
    Nançay Radioheliograph
    Contact: Nicole Vilmer, Meudon
    Type of Observation: Goals: Instrument Setup:
    Active region multi-channel imaging at dm-m wavelengths Obtain multi-frequency images of the low and middle corona (0.1-0.5 Rs above the photosphere) to identify structures, trace their evolution before flares, and identify sites of electron acceleration in non-flaring active regions. Daily imaging observations of the whole Sun at five frequencies in the range 150-450 MHz (standard setup: 164, 236.6, 327, 410, 435 MHz; change of frequencies and extension to up to ten frequencies possible).  Stokes Parameters I, V. 8 images/second. Spatial resolution between 0.3' and 6', depending on observed frequency and direction.
    Flare multichannel  imaging at sub-second time resolution Study non thermal energy release in solar flares, the sites of acceleration and the propagation of deka-keV electrons over an extended coronal height range ( 0.1-0.8 Rs above the photosphere), large-scale coronal shock waves and ejecta associated with CMEs. Provide observational constraints for particle injection into interplanetary space Same as above
    Mitaka Solar Observatory, National Astronomical Observatory Japan
    Contact: Takashi Sakurai or Yoshinori Suematsu, NAOJ
    Type of Observation: Goals: Instrument Setup:
    Magnetograms (vector),
    active region H-alpha images
    Obtain vector magnetic field measurements and corresponding H-alpha and white-light images of target active regions. The Solar Flare Telescope which is made of a video vector magnetograph and H-alpha and white light imagers. Its aligned field of view is 400"X300", with 0.66" pixel. Magnetograms are taken every 3 minutes. H-alpha images are taken every 30 seconds.
    Full disk H-alpha and white light imaging Detection of flares, sunspot evolution 10cm refractor with Kodak Megaplus 4.2 (white light, a few frames per day), 4cm refractor with a TV CCD camera (H-alpha, 1min cadence). Observing times: UT 23--08
    Norikura Solar Observatory, NAO Japan
    Contact: Kiyoshi Ichimoto, NAOJ
    Type of Observation: Goals: Instrument Setup:
    Full and partial limb imaging, optical spectroscopy and polarimetry Detection of coronal eruptions and flare-driven flows, spectroscopic diagnosis of the corona, polarimetry of disk and limb regions 10cm coronagraph (coronal green-line images and Dopplergrams), 25cm coronagraph and spectrograph, polarimeter (spectroheliograms and polarimetry). observing times: April to November, UT 22--07
    Nobeyama Radioheliograph
    Contact: Kiyoto Shibasaki, NRO
    Type of Observation: Goals: Instrument Setup:
    Full-disk  radio imaging Locate non-thermal electron acceleration sites and identify the acceleration machanism.  Search for phenomena in precursor phases just before impulsive onsets. Standard observing mode: Frequency/Polarization: 17 GHz/I and V, 34 GHz/I; temporal resolution: 1 sec; FOV/HPBW: Full disk/16 arc sec (17GHz), 8 arc sec(34GHz); PFI (5 arc min.) /10 arc sec (17 GHz); and high temproal resolution mode(during bursts): temporal resolution: 100 msec
    Ondrejov Observatory
    Contact: Petr Heinzel or  Karel Jiricka Ondrejov Obs
    Type of Observation: Goals: Instrument Setup:
    Active region and flare high cadence optical spectroscopy Chromospheric response to particle-beams precipitation at high temporal resolution, heating and flows at different chromospheric layers Multiline optical spectrograph, range from Ca II H+K up to H-alpha. Video mode: CCD video-cadence (25 frames/sec) spectra in H-alpha, D3 (or H-beta) and Ca II 8542 lines plus 0.5 A H-alpha video cadence filtrograms. Full spectrum mode: 5 cameras covering many chromospheric and photospheric lines, time resolution down to a few sec (on film) plus video H-alpha 0.5 A slit-jaw filtergrams. Both modes can run simultaneously
    Whole-Sun radio spectra and flux measurements Energy release signatures in flares with emphasis on spikes and type III bursts, shock waves, and particle beam acceleration. Analysis of effects of particle beams' bombardment of solar atmosphere layers and the study of these layers' responses in comparison with optical (H-alpha) and X-ray observations Daily single frequency flux at 3 GHz with 10 ms time resolution.  Spectra 0.8-2.0 and 2.0-4.4 GHz, each with 256 frequency channels and 100 ms time resolution.  Only flares are archived - for list and gif see our web page
    Oporto Radiospectrograph
    Contact: A. S. de Magalhaes, U Porto
    Type of Observation: Goals: Instrument Setup:
    Radio dynamic multichannel observations of flares Obtain measurements of non-thermal electrons in noise storms, electron beams and accelerated at shock waves Spectral resolution of 1 MHz and a time resolution of  60 ms, within the band 150 to 650 MHz
    Owens Valley Solar Array
    Contact: Dale Gary, NJIT or Kjell Nelin, OVRO
    Type of Observation: Goals: Instrument Setup:
    Active region multi- channel imaging and polaarimetry Obtain coronal temperature, emission measure, and magnetic field measurements (with ~ 15" resolution) daily, 43 frequencies, 1-18 GHz, dual polarization, 12 s time resolution, 10 baselines
    Flare multifrequency imaging Determine radio emission mechanism, coronal flare location, radio spectral diagnostics of electron energy distribution and ambient plasma parameters If flare-triggering available: auto-switch to 10-12 frequencies, 1-18 GHz, Stokes I, 2 s time resolution, 10 baselines. If no flare-triggering: use same sequence as for active regions (12 s time resolution)
    PHOENIX Radio Spectrometer
    Contact: Arnold Benz, ETH, Zurich
    Type of Observation: Goals: Instrument Setup:
    Full-disk, high time resolution, broadband spectral radiopolarimetric observations Coherent radio emissions of energy release (e.g. spikes) and of propagating and trapped electrons.  Diagnostics of the acceleration process and of the plasma of propagation and trapping. Daily 0430 - 1600 UT: 200 - 800 MHz; Daily 1630 - 1900 UT: 0.9 - 4.0 GHz
    Potsdam Solar Radio Astronomy Group
    Contact: Gottfried Mann or Henry Aurass, AIP
    Type of Observation: Goals: Instrument Setup:
    High resolution and full-disk H-alpha images Whole sun radio spectra (meter-decimeter range) with sweep spectrographs, selected ranges with multichannel polarimeters. Coronal plasma physics, shock waves and particle acceleration, flares and CMEs, flare dynamics, magnetic field evolution and nonthermal electron injection. 4 sweep spectrographs 40-100, 100-170, 200-400 and 400-800 MHz using 4 different aerials (crossed log.per. Yagi, 10.5m and 2x7.5m diameter paraboloids). Time res. 0.1 s. 2 multichannel receivers (in special obs. periods): 693-740 MHz, 48 1 MHz channels, 10ms time res. 326-346 MHz, 180 Channels, 20ms time res. flux and circ. pol. degree. Observing time interval: winter about 8-14 UT. summer about 4-18 UT.
    Prairie View Solar Observatory
    Contact: Tian-Sen Huang, Prairie View A&M Univ.
    Type of Observation: Goals: Instrument Setup:
    High resolution and full-disk H-alpha images Coordinated observation of solar active regions designated as targets for the HESSI mission. Comparative study of flaring events and their relation to the magnetic signature of active regions. High resolution H-alpha images: 6 by 8 arcmin images of a solar area of interest are obtained with a 35-cm Gregorian vacuum telescope, Daystar H-alpha filter and ST-7 CCD camera. Full disk H-alpha images (under construction): recorded on a 1024 by 1024 CCD camera.
    RATAN 600 Radiotelescope
    Contact: Vladimir Bogod,  Special Astrophysical Observ.
    Type of Observation: Goals: Instrument Setup:
    Active region radio spectra with 1D imaging and polarimetry Obtain the data about temperature, emission measure, magnetic field in active region (before, during and after flare), the study of the appearence of new magnetic flux using fine polarization measurements Daily - 35 frequencies, 0.955-16.4 GHz, V and I Stokes parameters, 3 azimuths [near 8-00UT, near 9-00 UT (meridian time) and near 10-00 UT]; special alert program - several azimuths (up to 20 with interval 8-9 minutes of time) at the same equipment.
    Sacramento Peak Observatory
    Contact: Dick Altrock, NSO
    Type of Observation: Goals: Instrument Setup:
    Active region coronal emission line imaging Obtain coronal temperature Daily observations of the corona above the limb with the Emission Line Coronal Photometer in Fe XIV, Fe X and Ca XV
    San Fernando Observatory
    Contact: Gary Chapman, CSUN
    Type of Observation: Goals: Instrument Setup:
    Active region imaging Obtain vector magnetic field measurements in photosphere Vector magnetic fields measured with the VSSHG
    Siberian Solar Radio Telescope
    Contact: Alexander Altyntsev or G. Ya. Smolkov, SSRT
    Type of Observation: Goals: Instrument Setup:
    Full disk radio imaging and polarimetry Obtain microwave images of the full Sun and to determine temporal evolution of coronal temperature and distribution of circular polarization in the active region before the flare. Daily images at about 0650 UT (local noon at longitude 102 E), 5.72 GHz, Stokes I and V, 21" spatial resolution.
    Flare high time resolution imaging Study of the fragmented energy release in solar flares. Diagnostics of plasma parameters in flare loops. During flares: One dimensional scans of the full Sun disk  with time resolution down to 14 ms (Stokes I and V). Two dimensional images of flare region with time resolution down to fractions of min.
    Solar Optical Observing Network
    Contact: Alan L. Kiplinger, NOAA/SEC
    Type of Observation: Goals: Instrument Setup:
    Full disk and active region images in H-alpha and white light. Record solar flares, from a network of four observatories around the world. Monitoring of up to six active regions at a cadence of 30 seconds (large scale) to 30 minutes (full disk). The large scale field of view is 6.4' x 6.4'; both large-scale and full-disk images are 512x512 pixels.
    Solar Radio Burst Locator
    Contact: Brian L. Dougherty, Caltech
    Type of Observation: Goals: Instrument Setup:
    Full disk microwave radio monitoring of position and spectra. Locate microwave bursts on the Sun and determine their spectra. Continuous daily monitoring at 245 MHz, 410 MHz, 610 MHz, and throughout 1-18 GHz. The instrument consists of a single 2 meter dish with a log-spiral feed for broadband reception, with a dual-frequency Yagi attached for observations at the lower frequencies.
    Trieste Solar Radio System
    Contact: Mauro Messerotti, TSRS
    Type of Observation: Goals: Instrument Setup:
    Full-disk, high time resolution, multichannel
    radio polarimetry
    Analyze radio signatures of energy release fragmentation in flares, e.g. spikes, and radio signatures of flare-accelerated electron beams, such as type III bursts.  Interpret the relevant radio diagnostics of the coronal plasma, in the attempt to characterize by the former the acceleration processes and by the latter the propagation environment. Daily, 6 frequencies (237, 327, 408, 610, 1420, 2695 MHz), circular polarization, 1 ms time resolution, no spatial resolution, two separate multichannel radiopolarimeters
    Udaipur Solar Observatory
    Contact: Ashok Ambastha, USO
    Type of Observation: Goals: Instrument Setup:
    Full disk H-alpha imaging Monitoring of active regions, filaments etc 15-cm Razdow H-alpha patrol telescope and CCD, cadence ~ 5-10 minutes during 0400-1100 UT
    Active region and euptive prominences Active regions, flares, and filaments H-alpha line center high resolution images at cadence of 15-20 sec
    Full disk magnetograms synoptic observations GONG instrument at 256x256 pixels each hour (to be upgraded to 1024x1024 pixels and cadence 1 minute)