URALN Codes

Position measurements of solar radio sources or inferred coronal holes at a discrete frequency, possibly including intensity and flux.

This code is used to report location of either coronal condensations observed above 500 MHz (approximate); for example, the "slowly" varying component, generally a = 1 or a = 2 (see definition below); or noise storms observed below 500 MHz (approximate), where total power observation of noise storm on the same frequency is not available, generally a = 1 or a = 3 (see definition below).

When total power observation is available, URANJ should be used.

Example:

Definition of symbols:

  • URALN comes from RAdio noise Location, code N

  • I I I I I = station indicator

  • Y = last digit of year
  • MM = month of year, 01 = January, 02 = February, etc
  • . DD = UT day of month

  • FFFFF = frequency in MHz

  • dd = UT day of month of data
  • / = filler
  • hh = UT hour of region location

  • HHT = UT time nearest beginning of observation period in hours and tenths of hours
  • a = type of observation reported, where
    • 1 = fan-beam, east-west scan using single group d e f f f for each source.
    • 2 = detailed pencil-beam measurements in heliographic coordinates-two groups (QXXYY b b b c c) for each source.
    • 3 = pencil-beam mapping on geocentric N-S-E-W grid; one group Qxxyy for each source
  • n = number of sources and (or) coronal holes reported
  • If a = 1 (fan-beam, east-west scan) use the following two groups:

  • d = noise source or inferred coronal hole and importance, where
    • 0 = noise source, importance 0 (least importance)
    • 1 = noise source, importance 1
    • 2 = noise source, importance 2
    • 3 = noise source, importance 3 (greatest importance)
    • 4 = inferred coronal hole, importance 1 (least importance)
    • 5 = inferred coronal hole, importance 2
    • 6 = inferred coronal hole, importance 3 (greatest importance)
  • e = location of noise source or deepest depression of inferred coronal hole east or west of scan center, where
    • 7 = east
    • 8 = west
  • f f f = distance of noise source or inferred coronal hole from scan center, in percent of photospheric radius

  • b b b = maximum intensity in tens of thousands of Kelvins(or, for sources at mm wavelengths, tens of Kelvins)
  • c c = flux enhancement from region in 10-22Wm-2Hz-1
  • If a = 2 (detailed pencil-beam measurements in heliographic coordinates) use the following two groups:

  • Q = quadrant (heliographic coordinates) containing the noise source, where
    • 1 = NE (northeast)
    • 2 = SE (southeast)
    • 3 = SW (southwest)
    • 4 = NW (northwest)
  • XX = distance to the central meridian in degrees (if above east or west limb, use 95)
  • YY = heliographic latitude in degrees

  • b b b = maximum intensity in tens of thousands of Kelvins(or, for sources at mm wavelengths, tens of Kelvins)
  • c c = flux enhancement from region in 10-22Wm-2Hz-1
  • If a = 3 (pencil-beam mapping on geocentric N-S-E-W grids) use the following group for each source:

  • Q = quadrant containing the noise source, where
    • 1 = NE (northeast)
    • 2 = SE (southeast)
    • 3 = SW (southwest)
    • 4 = NW (northwest)
  • XX = distance to east or west of N-S diameter in tenths of photospheric radius
  • YY = distance north or south of E-W diameter in tenths of photospheric radius

Note: / is to be used for data not available.