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
(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.
United States Frequency Allocations
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
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
- AGC off
- Preamp 2 on
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
15-DP11 15M dipole antenna with 1:1 Balum
SDR-IQ Receiver Video
- 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)
: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 STEREO / WAVES
NASA WIND-WAVES: The Radio and Plasma Wave Investigation on the WIND Spacecraft
NASA STEREO (Solar TErrestrial RElations Observatory)
NASA STEREO / WAVES data