Notice! The experiment protocol described on this page is tentative! Please e-mail comments to email@example.com.
- How does the 2017 Total Solar Eclipse affect HF propagation paths?
- How much of the ionosphere is affected by a solar eclipse?
- For how long is the ionosphere affected by a solar eclipse?
- Observe changes in HF propagation caused by the eclipse by making recordings of large portions of the HF band from multiple locations, most importantly across the North American continent.
- Provide wideband recordings of HF spectra to support SEQP log/RBN/PSKReporter/WSPR data.
- 21 August 2017, 1400 – 2200 UTC
Please priortize recording of frequencies that correspond with Solar Eclipse QSO Party (SEQP) operation, especially the lower frequencies, as these should see the largest eclipse effect. This consists of the standard HF contest bands (see table below). In addition, we welcome observations from as much of the LF, MF, and HF spectrum as possible. The capabilities of different HF receivers vary widely, and some modern HF SDRs are capable of multiple slice receivers. Note that it is possible to simulteously make wideband recordings and act as a RBN skimmer node. See N6TV's How-To Guide for Running a Combined CW-RTTY Red Pitaya Skimmer for instructions on how send SDR data streams to multiple programs simultaneously.
|160 m||1.800 - 2.000 MHz|
|80 m||3.500 - 4.000 MHz|
|40 m||7.000 - 7.300 MHz|
|20 m||14.000 - 14.350 MHz|
|15 m||21.000 - 21.450 MHz|
|10 m||28.000 - 29.700 MHz|
You may use any radio and software that is capable of generating IQ recordings of HF spectrum that can be properly time-stamped and frequency-stamped. We recommend using MIT Haystack's Digital RF software for this purpose, as it is will record observations to the proper IQ format and provide the required time- and frequency- stamping.
We encourage you to make the most careful measurements possible. If you are capable of stabilizing your receiver with a high-stability frequency reference or provide amplitude calibration characteristics for your system, please do so. You may describe your methodology in the Zenodo Data Description box and upload supporting documents if necessary (such as block or antenna pattern diagrams).
Uploading to Zenodo
Please submit the following items:
- IQ File for each band recorded (Will be encapsulated in a HDF5 file if using MIT's Digital RF)
- Supporting data files (i.e. any files needed to help interpret the raw data, such as a block diagram of the recieve station)
Use the <Callsign>_wideband_<start_freq>_<stop_freq>kHz_<YYYYMMDD>_<HHMM>UT.<ext> filename convention for uploaded where HHMM is the UT start time of that particular file. Examples:
- K2MFF_wideband_3500_3692kHz_20170821_1400UT.hd5 (for a HDF5 IQ recording of 3500-3692 kHz made at K2MFF on 21 Aug 2017 starting at 1400 UT)
- K2MFF_wideband_supporting_20170821_1400UT.pdf (for a PDF of supporting material to help in interpretting the data)
In the data description box, please include:
- Your Name and Callsign
- Latitude and Longitude of the Recording(s)
- A description of station hardware configuration, including
- Antenna type
- Antenna pointing direction (if applicable)
- Receiver type
- Any other information you believe would be necessary for proper scientific interpretation of your measurements
In the Notes box, you may include your personal comments regarding your observations.
Please license your data as:
- Open Source
- Creative Commons Attribution 4.0
Page Contributors: W2NAF
24 July 2017