Max Millennium Program
Collaborating Ground Based Observatories

  • Aryabhatta Research Institute of Observational Sciences
  • Baikal Solar Vacuum Telescope
  • Big Bear Solar Observatory
  • Brazilian Solar Spectroscope
  • Callisto Solar Spectrometer
  • Carl Sagan Observatory
  • Catania Astrophysical Observatory
  • Crimean Astrophysical Observatory
  • Green Bank Solar Radio Burst Spectrometer
  • 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
  • Meudon Observatory
  • Mirror Coronagraph for Argentina
  • Mitaka Solar Observatory, NAO Japan
  • Nançay Radioheliograph
  • Nobeyama Radioheliograph
  • Norikura Solar Observatory, NAO Japan
  • Ondrejov Observatory
  • Ooty Radio Telescope
  • Oporto Radiospectrograph
  • Owens Valley Solar Array
  • PHOENIX Radio Spectrometer
  • Potsdam Solar Radio Astronomy Group
  • Prairie View Solar Observatory
  • RATAN 600 Radiotelescope
  • Rosse Solar-Terrestrial Observatory
  • Sacramento Peak, NSO US
  • San Fernando Observatory
  • Siberian Solar Radio Telescope
  • Solar Optical Observing Network
  • Solar Submillimeter-Wave Telescope
  • Trieste Solar Radio System
  • Udaipur Solar Observatory
  • Wilcox Solar Observatory
  • All Ground Based Solar Observatories







    Aryabhatta Res. Inst. of Observational Sciences
    		 Contact: Wahab Uddin, ARIES
    Type of Observation: Goals: Instrument Setup:
    High resolution H-alpha imaging Active region, flares and eruptive prominences Monitoring of active regions, filaments etc Active regions, flares, and filaments/prominences 15-cm Coude Solar Tower Telescope for H-alpha flare patrol and CCD, cadence ~ 100 millisec-30 sec during 0200-1100 UT
    H-alpha line center high resolution images at cadence of ~ 100 millisec-30 sec during 0200-1130 UT.



    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 and solar image in H-alpha center line ± 0.5Å. 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".17/pixel, detector  CCD camera: Princeton Instruments 512x512 pixel and FLIgrab 2084x2084 pixel.



    Big Bear Solar Observatory
    		 Contact: Haimin Wang, NJIT
    Type of Observation: Goals: Instrument Setup:
    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.



    Callisto Solar Spectrometers
    		 Contact: Christian Monstein, ETH
    Type of Observation: Goals: Instrument Setup:
    Meter wave and low decimeter wave full-disk observations
    		 Observations of signatures of flare shocks (Type II events) and electron beams escaping from the Sun on open magnetic field lines (Type III bursts), for predictions of CMEs heading toward Earth. The global CALLISTO network consists of identical programmable heterodyne receivers, connected through the internet.   It operates between 45 and 870 MHz using a modern, commercially available broadband cable-TV tuner CD1316 having a frequency resolution of 62.5 KHz.



    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: Paolo Romano, 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. A 150 - mm refractor (230 cm focal length) with an H-alpha Lyot filter (bandwidth of 0.25 or 0.5 Å), and an E2V 42-40 Front illuminated MPP mode CCD (2048x2048 pixels, pixel size 13.5 micron, 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



    Green Bank Solar Radio Burst Spectrometer*
    		Contact: Tim Bastian, NRAO
    Type of Observation:Goals:Instrument Setup:
    Full disk dynamic spectra of solar radio burstsPublicly-available research-quality dynamic spectra of flares
    		10 MHz to 1050 MHz with a time resolution of 1 s during  the time range from 12 to 24 hours UT



    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: Werner Pötzi, KSO
    Type of Observation: Goals: Instrument Setup:
    Full-disk H-alpha imaging
    Full-disk white light imaging
    Full-disk CaIIK imaging
    High time resolution H-alpha and CaIIK flare imaging    		 Obtain full-disk solar images in different wavelenghts (H-Alpha, CaIIK, Continuum) for monitioring the activity level of the Sun at high temporal coverage. With the solar patrol telescope images are taken in H-alpha
    (656.3nm, FWHM 0.07nm, Lyot filter), white light (545 nm, FWHM 10nm, interference filter) and  CaIIK (393.4nm, FWHM 0.3nm, Daystar filter). The H-alpha images are obtained at a cadence of 6 seconds, after processing only a 1 minute cadence is kept in the archive. In case of optical flares or X-ray flares above the level of C3 all images are kept. Once a day an overexposed set of H-alpha images is taken to get images of prominences for the Skalnate Pleso Observatory. The CaIIK images are obtained at a cadence of 6 seconds, after processing only a 1 minute cadence is kept in the archive. In case of X-ray flares above the level of C7 all images are kept. The white light images are obtained at a cadence of 1 minute, after processing onlya 5 minute cadence is kept in the archive. In case of X-ray flares above the level of M1 all images are kept. Additonally we obtain a daily sunspot drawing.



    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:
    Coronal magnetic field and plasma doppler and density.
    Chromospheric and photospheric imaging.

    		 Obtain coronal magnetic field and density structure; CME and alfven wave studies; precision photometry for irradiance studies Operate every day weather permitting 17UT to 0230 UT. Coronal magnetic field and alfven wave observations every day at varying cadences, Fe-XIII 1074.7 and 1079.8 nm and He-I 1083.0 nm full stokes polarimetry, every 3 minutes. 
    Broad-band white light polarization brightness of low corona.
    Chromosphere: 1)  He-I 1083.0 nm full disk and limb, 2) CaII-K Narrow Band core and wing full disk images;
    Photosphere:  Red and Blue continuum full disk images



    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)



    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



    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



    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



    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



    Ondrejov Observatory*
    		 Contact: Petr Heinzel or  Hana Meszarosova 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. 0.8-2.0 and 2.0-4.5 GHz radio dynamical spectra, each with 256 frequency channels and 10 ms time resolution.  Only flares are archived - for list and gif see our web page
    sunkl.asu.cas.cz/~radio



    Ooty Radio Telescope
    		 Contact: P. K. Manoharan, Radio Astronomy Centre
    Type of Observation: Goals: Instrument Setup:
    Interplanetary scintillation measurements and solar radio observations Measurements of solar wind density turbulence, its spectrum, and solar wind speed in 3D; track CMEs and CIRs to 1 au and beyond. Observation of interplanetary scintillations (IPS) at 327 MHz, and Callisto Solar Radio Spectrograph in frequency range of 40-900 MHz.



    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.



    Rosse Solar-Terrestrial Observatory*
    		 Contact: Peter T.Gallagher Trinity College Dublin
    Type of Observation: Goals: Instrument Setup:
    CALLISTO full-sun radio spectrograms Coordinated observations of Type IIs and Type IIIs with STEREO, SDO and RHESSI to study solar flares, CMEs, shocks, and particle acceleration. Daily observations using three CALLISTO spectrometers covering 10-500 MHz with 4-8 sweeps per second.
    AWESOME ionospheric spectrograms Sudden ionospheric disturbances (SIDs) - effects of solar flares and CMEs on Earth ionosphere Continuous monitoring of very low frequency (VLF) signals at 3-50 kHz with millisecond sampling. 



    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 Submillimeter-Wave Telescope*
    		Contact: Pierre Kaufmann, CRAAM
    Type of Observation:Goals:Instrument Setup:
    Full disk submillimeter radiometry at high time resolution.
    		Explore solar emission from the quiet sun, active regions, and solar flares in the submillimeter range.
    		 4 radiometers at 200 GHz and 2 radiometers at 400 GHz at El Leoncito in Argentina Andes; late in 2011 we are installing solar patrol polarimeters at 45 and 90 GHz, at the same site.

    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)



    Wilcox Solar Observatory*
    		 Contact: Todd Hoeksema, WSO
    Type of Observation: Goals: Instrument Setup:
    Full-disk line-of-sight low-resolution magnetograms
    Mean magnetic field of the Sun
    PFSS Coronal Field Model     		Synoptic observations of the large-scale magnetic field of the Sun Babcock solar magnetograph observes full disk with 3 arc minute resolution at least daily in FeI 5250, usually near 20 UT.

    * Updated 2011 or later