Originally constructed in 1995, the Global Oscillation Network Group (GONG) is a network of six identical ground-based solar telescopes distributed around the Earth in order to obtain continuous observations of the Sun. Those sites are located in Big Bear, California (BB); Mauna Loa, Hawaii (ML); Learmonth, Australia (LE); Udaipur, India (UD); El Teide, Spain (TD); and Cerro Tololo, Chile (CT). Additionally, there are three engineering/testbed sites in Boulder, Colorado (TC, TE, and TS). Owned by the National Science Foundation, GONG is operated and maintained by the National Solar Observatory (NSO) with significant funding from NOAA’s Space Weather Prediction Center (SWPC). Each minute, weather permitting, the GONG network observes the Sun at two spectral wavelengths: 676.78nm (a Ni I absorption line) and 656.28nm (the H-alpha absorption line).

Originally constructed in 1995, the Global Oscillation Network Group (GONG) is a network of six identical ground-based solar telescopes distributed around the Earth in order to obtain continuous observations of the Sun. Those sites are located in Big Bear, California (BB); Mauna Loa, Hawaii (ML); Learmonth, Australia (LE); Udaipur, India (UD); El Teide, Spain (TD); and Cerro Tololo, Chile (CT). Additionally, there are three engineering/testbed sites in Boulder, Colorado (TC, TE, and TS). Owned by the National Science Foundation, GONG is operated and maintained by the National Solar Observatory (NSO) with significant funding from NOAA’s Space Weather Prediction Center (SWPC). Each minute, weather permitting, the GONG network observes the Sun at two spectral wavelengths: 676.78nm (a Ni I absorption line) and 656.28nm (the H-alpha absorption line).

Originally constructed in 1995, the Global Oscillation Network Group (GONG) is a network of six identical ground-based solar telescopes distributed around the Earth in order to obtain continuous observations of the Sun. Those sites are located in Big Bear, California (BB); Mauna Loa, Hawaii (ML); Learmonth, Australia (LE); Udaipur, India (UD); El Teide, Spain (TD); and Cerro Tololo, Chile (CT). Additionally, there are three engineering/testbed sites in Boulder, Colorado (TC, TE, and TS). Owned by the National Science Foundation, GONG is operated and maintained by the National Solar Observatory (NSO) with significant funding from NOAA’s Space Weather Prediction Center (SWPC). Each minute, weather permitting, the GONG network observes the Sun at two spectral wavelengths: 676.78nm (a Ni I absorption line) and 656.28nm (the H-alpha absorption line).

This archived Paleoclimatology Study is available from the NOAA National Centers for Environmental Information (NCEI), under the World Data Service (WDS) for Paleoclimatology. The associated NCEI study type is Climate Reconstruction. The data include parameters of climate reconstructions|tree ring with a geographic location of North Pacific Ocean. The time period coverage is from 385 to -38 in calendar years before present (BP). See metadata information for parameter and study location details. Please cite this study when using the data.

This data file consists of Kp indices, Ap indices, Cp indices, C9 indices, sunspot number, and 10.7 cm flux. The most often requested parameter of this file are the Kp indices. These planetary indices are derived from the K indices ( a quasi-logarithmic three-hourly measure of magnetic activity ranging from 0 for the least disturbed periods to 9 for the most disturbed) from 12 observatories located between 46 degrees north geomagneticlatitude and 63 degrees south geomagnetic latitude.

The Magnetometer Instrument Engineering Telemetry Data file contains data used to support the generation of the Magnetometer Level 1b product, and monitor and evaluate the health and performance of the two magnetometers. This data is transmitted to the ground in raw digital counts, and subsequently converted into physical units by the ground system. Some of the data pertains to the temperature of components of the magnetometers. This includes temperatures for the electronics and sensors. Other telemetry includes reference voltages and temperature dependent scale factors and offsets relating raw observed counts to magnetic field units (nanoteslas) for the two magnetometers. The Magnetometer Calibration Data file contains raw observation counts and data acquisition status from the inboard and outbound magnetometers for a one second interval during a calibration maneuver. Nominally, this file contains ten observation samples acquired at one-tenth of a second intervals.

Geomagnetic variation data with 2.5 minute resolution

The geomagnetic aa indices are the continuation of the series beginning in the year 1868. A full description of these indices is given in the International Association of Geomagnetism and Aeronomy (IAGA) Bulletin No 33, which contains them for the years 1868-1967. Descriptions are also given (especially comparisons with am, ap, or Ci indices) in two short papers [Ann. Geoph., 27, 62-70, 1971 and J. Geophys. Res., 77, 6870-6874, 1972]. The aa values form 1968-1975 are contained in the IAGA Bulletin 39. From 1976 onward they are included in IAGA Bulletin 32. Revised aa values for the years 1969-1976 have been distributed in 1979 to the recipients of IAGA Bulletin 32 in the form of loose sheets to be inserted in the Bulletin 39 (1968-1975) and 32f (1976). A graph of these values 1868 - 1979 is published in the 426 Part I issue of Solar-Geophysical Data (SGD) (page 137). Revised aa values for 1968-1977 appear in the 411 Part II February 1977 SGD. Briefly, such three-hourly indices as these, computed from K indices of two antipodal observatories (invariant magnetic latitude 50 degrees), provide a quantitative characterization of the magnetic activity, which is homogeneous through the whole series. Half-daily and daily values give an estimation of the activity level very close to that obtained with "am" indices. Values are in gammas and correspond to the activity level at an invariant magnetic latitude of 50 degrees. The aa indices are computed for: N = daily values for the Northern Hemisphere, S = daily values for the Southern Hemisphere, M = half-daily values of aa indices for the Greenwich day. Letters C and K refer to a classification of the quiet days of the month (C = really quiet, K = quiet but with slightly disturbed three-hourly intervals). The letters on the left refer to the 24-hour Greenwich day, on the right to a period of 48 hours centered on the Greenwich noon. The three-hourly indices aa are available from the appropriate World Data Centers in digital form using the format described in IAGA Bulletin 33.

This file is comprised of the variation one minute values of the geomagnetic components X, Y and Z. These data were calculated by the Air Force Geophysics Laboratory magnetometer network during the years 1978-1983. The values are variation values and should not be used in looking at absolute values of the geomagnetic components.

The NOAA National Centers for Environmental Information (formerly National Geophysical Data Center) receives, on a monthly basis, Q indices from Sodankyla. These data are available from July 1957 to the present. Sodankyla indices are the most complete records of Q indices that NCEI has. The archive also contains Q indices from 15 other observatories. The Q index is a measure of geomagnetic activity assigned by high latitude (geomagnetic latitude > 58 degrees) geomagnetic observatories for each 15 minute interval. The index is designed to study auroral and ionospheric phenomena over a time scale smaller than that possible with KP. The Q scale is loosely logarithmic, with possible values from 0 to 11.