Solar Radio Data. Scientists monitor the structure of the solar corona, the outer most regions of the Sun's atmosphere, using radio waves -- the surface of the Sun is 6,000 degrees Kelvin, while the high corona can reach several million degrees Kelvin. Contact online >>
Solar Radio Data. Scientists monitor the structure of the solar corona, the outer most regions of the Sun''s atmosphere, using radio waves -- the surface of the Sun is 6,000 degrees Kelvin, while the high corona can reach several million degrees Kelvin.
Each observatory monitors solar radio emissions on 8 discrete fixed frequencies (245, 410, 610, 1415, 2695, 4995, 8800 and 15400 MHz) as well as low frequency spectral emissions in the VHF band. This document is only concerned with the 8 discrete frequencies.
Solar Radio Datasets. The structure of the solar corona, the outermost regions of the Sun''s atmosphere, can be monitored using radio waves (100''s of MHz to 10''s of GHz). Variations in the radio wave spectrum reveal characteristics of the corona and upper chromosphere in terms of altitude profile for the local plasma temperature, density and
Schmahl and Kundu (1995) find that the solar radio fluxes in the spectral range 1000-9400 MHz correlate well with the total solar irradiance. The intermediate frequencies (at 2800 and 3750 MHz) are produced mainly by free-free gyroresonance emission from sunspot structures, while 1000 and 9400 MHz flux are produced mainly by free-free processes
Solar-Geophysical Data Reports 54 Years of Space Weather Data. Solar
HF Radio: Weak or minor degradation of HF radio communication on sunlit side,
Outstanding Occurrences -- Solar radio emission bursts at fixed frequencies are
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The structure of the solar corona, the outermost regions of the Sun''s atmosphere, can be monitored using radio waves (100''s of MHz to 10''s of GHz). Variations in the radio wave spectrum reveal characteristics of the corona and upper chromosphere in terms of altitude profile for the local plasma temperature, density and magnetic field. Typically, the lower the frequency, the higher the height of origin.
NOAA NCEI has acquired these legacy data sets from multiple sources over many decades. The data presented here are provided, ''as is,'' and in most cases the linked documentation is the entirety of available information. In some cases, older data may also be found in theSpace Weather Legacy Print Publications.
Radio bursts are associated with solar flares. The signal arrival time delay at Earth of the different radio frequencies during burst events is due to the outward movement of the source. Large bursts last 10 to 20 minutes on average. Longer radio noise storms of persistent and variable high levels of radiation originate in sunspot groups, areas of large, intense magnetic fields.
Measurements taken at local noon at various solar radio observatories. Observatories include facilities in the Solar Electro-Optical Network (SEON, RSTN, SOON), Krakow, and Penticton. Date coverage and observed frequencies vary.
Daily mean radio flux densities for 55 different observatories (1949–1986) per the quarterly IAU Bulletin.
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The observed and predicted Solar Cycle is depicted in Sunspot Number in the top graph and F10.7cm Radio Flux in the bottom graph.
An updated version of the Solar Cycle prediction product is now available on NOAA''s Space Weather Prediction Testbed.
The mean forecast for the current solar cycle (Cycle 25) is given by the red line. This is based on an international panel that was convened in 2019 for this purpose. In February, 2023 the plot was modified to show the full range of the 2019 Panel prediction as the gray shaded region (similarly for the F10.7 cm plot). This takes into account expected uncertainties in the cycle start time and amplitude. Use the drop-down menu below each plot to display specific curves within this range.
These plots, like many on the SWPC website, are interactive.
Left clicking on the data and holding while you drag will define a zoom window.
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