Sun Type III/2 Radio Burst
June 13, 2014, 2014 UT


The Sun radio emission burst was observed with these instruments.

Tektronix MDO4104-6 Spectrum Analyzer Video

Tektronix MDO4104-6 Spectrum Analyzer

  • The below Tektronix MDO4104-6 spectrum analyzer display shows the Sun radio emissions from 17.5 MHz to 24.0 MHz.
  • The Sun radio emission is the light blue to green-yellow color in the top blue spectrogram window.
  • Radio stations
    • The first set of strong vertical signals from the left edge are the 17.5 MHz to 17.9 MHz broadcasting stations.
    • The second set of strong signals from the left edge are the 17 meter (18.068 MHz to 18.168 MHz) amateur radio band.
    • Radio station WWV at 20.0 MHz is the white vertical line in the spectrogram just over one division left of center.
      • WWV distance is 1,511 km with a bearing of 105.3 degrees.
    • The strong set of signals just right of the center frequency is the 15 meter (21.0 MHz to 21.45 MHz) amateur radio band.
  • The short thin horizontal lines in the spectrogram are weak lighting or weak RFI bursts.
  • The antenna sensitivity peaks on the left side of the spectrogram.
    • This results in the background noise being a lighter blue color on the left side of the spectrogram.

Sun radio emissions

United States Frequency Allocations

United States Frequency Allocations

Sun Location

Antenna East-West Dipole and Sun position

The Sun was 52.55 degrees above the horizon when the solar radio emission occurred.

Tektronix MDO4104-6 Spectrum Analyzer Settings

  • Spectrum analyzer is the bottom window
    • 17.5 MHz start frequency
    • 20.75 MHz center frequency
    • 24.0 MHz stop frequency
    • 6.5 MHz frequency span
    • 6.5 MHz capture bandwidth
    • 1 kHz resolution bandwidth
    • 650 kHz per horizontal division
    • 5 dBm per vertical division
  • Spectrogram (waterfall) is the top window
    • Spectrogram bottom is the current spectrum trace shown at the bottom of the display.
    • Spectrogram top is the oldest spectrum, approximately 1 minute and 45 seconds after the current spectrum trace at the bottom.
    • 328 spectrums in the spectrogram.
    • 0.32 seconds per spectrum update rate.
    • 3.12 spectrums per second update rate.
    • Date and time in lower right corner is in UT.
  • Python 2.7.6 script taking screen captures every 12 seconds

Tektronix  MDO4104-6

Spectrum Analyzer Equipment

Icom IC-R75 Radio Receiver Strip Chart

  • Icom IC-R75 radio receiver with Radio-SkyPipe II strip chart recorder
    • Compare the spectrogram with the Icom IC-R75 strip chart.
    • Radio emission has a rapid onset and slower decay, the burst looks like a shark fin.
    • Multiple plateaus on trailing edge
Sun radio emissions

Radio Equipment

  • Icom IC-R75
    • 20.1MHz
    • LSB
    • AGC off
    • Preamp 2 on
  • Behringer XENYX 302USB 5-Input Mixer with XENYX Mic Preamp and USB/Audio Interface
    • The HP laptop does not have a line input, only mic input.
    • XENYX 302USB takes the IC-R75 back recorder jack [REC] signal and digitizing it.
    • The XENYX 302USB has its own Line gain control.
    • The XENYX 302USB has its own headphone gain control.
  • MFJ Enterprises MFJ-1040C Preselector
  • Radiowavz 15-DP11 15M dipole antenna with 1:1 Balum


SDR-IQ Receiver Video

RFSpace SDR-IQ Receiver

Sun radio emissions

Observing Information

  • OBS-Time: June 13, 2014, 2014 UT
  • OBS-Location: Camas, WA USA, 16.6 miles East-North-East from the center of Portland, OR, USA

Radio JOVE Data Archive Calendar

Verifying Solar Burst

NOAA/ National Weather Service
National Centers for Environmental Prediction
Space Weather Prediction Center
Solar Event Reports (Edited Events)

gt:Product: 20140613events.txt
:Created: 2014 Jun 14 1802 UT
:Date: 2014 06 13
# Prepared by the U.S. Dept. of Commerce, NOAA, Space Weather Prediction Center
# Please send comments and suggestions to SWPC.Webmaster@noaa.gov 
# Missing data: ////
# Updated every 30 minutes.
#                            Edited Events for 2014 Jun 13
#Event    Begin    Max       End  Obs  Q  Type  Loc/Frq   Particulars       Reg#
4110       2013   2017      2020  G15  5   XRA  1-8A      C9.0    2.3E-03   2087
4110       2014   2015      2025  HOL  2   FLA  S20E34    SF      ERU       2087
4110 +     2014   2014      2014  PAL  G   RBR  245       1300              2087
4110 +     2014   ////      2015  SAG  C   RSP  025-180   III/2             2087
4110 +     2014   2014      2014  PAL  G   RBR  410       460               2087

Obs   - The reporting observatory.
        CUL - Culgoora, Australia
        HOL - Holloman AFB, NM, USA    LEA - Learmonth, Australia
        PAL - Palahua, HI, USA         RAM - Ramey AFB, PR, USA
        SAG - Sagamore Hill, MA, USA   SVI - San Vito, Italy

Q     - Quality
        For radio bursts at fixed and sweep frequencies, and for storms, this 
        shows the quality of the data
                       C = Corrected report
                       G = Good 
                       U = Uncertain
        For optical flares, this shows the quality of observing conditions, 
        from 1 to 5, where:  1 = very poor and 5 = excellent
        X-ray events and SXI flare have a quality of 5 (meaning excellent).

Type  - Type of report, see http://www.swpc.noaa.gov/info/glossary.html
          BSL = Bright surge on the limb
          DSF = Filament disappearance
          EPL = Eruptive prominence on the limb
          FIL = Filament
          FLA = Optical flare observed in H-alpha 
          FOR = Forbush decrease (cosmic ray decrease))
          GLE = Ground-level event (cosmic ray increase)
          LPS = Loop prominence system
          PCA = Polar cap absorption
          RBR = Fixed-frequency radio burst
          RNS = Radio Noise Storm
          RSP = Sweep-frequency radio burst
          SPY = Spray
          XFL = SXI X-ray flare from GOES Solar X-ray Imager (SXI)
          XRA = X-ray event from SWPC's Primary or Secondary GOES spacecraft

	Type  II: Slow drift burst
	Type III: Fast drift burst
	Type  IV: Broadband smooth continuum burst 
	Type   V: Brief continuum burst, generally associated with Type III bursts
	Type  VI: Series of Type III bursts over a period of 10 minutes or more, 
	           with no period longer than 30 minutes without activity
	Type VII: Series of Type III and Type V bursts over a period of 10 minutes 
	           or more, with no period longer than 30 minutes without activity
	Type CTM: Broadband, long-lived, dekametric continuum
	Intensity is a relative scale 1=Minor, 2=Significant, 3=Major 


  • NASA WIND-WAVES: The Radio and Plasma Wave Investigation on the WIND Spacecraft
  • NASA STEREO (Solar TErrestrial RElations Observatory)