I) Dates and Times

See the chart on the HamSCI MSQP Home Page for the six major showers that HamSCI will be investigating. The next will be the Eta Auqariids, May 5-7, 2026

II) Operating Bands and Mode

HamSCI is interested in both 6 and 10 meter MS propagation. While 6 meters is the most popular MS band, 10 meters, a band having both HF and VHF characteristics, lends itself to novel research opportunities.

This event is open to both Two-Way (transmit/receive) and Monitor (receive only) stations, fixed in position (no mobiles or rovers).
The event will use both the 6 and 10 meter bands. (50.260 and 28.145 MHz are popular MS operating frequencies.)
If your station can operate both 6 and 10 meters - please operate on both, alternating bands at 20 minute intervals (xx:00, xx:20, xx:40)
MSK144 is the only mode for this event.
Be sure the receive node software (most likely, the WSJT-X suite) is properly configured, especially your 6-character Maidenhead Grid Square, for sending reports to the PSKReporter. The data sent to, and collected by, PSKReporter will be critical to the research efforts underlying this event.

III) Valid Exchange

A valid 2-way MS QSO is defined as follows:

Each station transmits and receives callsigns, grid squares and/or signal reports and acknowledges the other station’s information (typically by sending ‘R’ or ‘RRR’ or ‘RR 73’)
There is no time limit when making a QSO. Whether 15 seconds, 5 minutes or 15 minutes - multiple retries are common with the MSK144 mode.
There is no penalty for 'dupes' (duplicate QSOs), meaning it is possible for one station to work another station 2, 3 or even 5 times during the operating period, on the same or a different band.

IV) Collection of WAV Files - Very important to the science objectives!

After the event concludes - all entrants - transmitters and monitors - please consider uploading your WAV file decodes to HamSCI's data repository at zenodo.org. Complete instructions are available at the MSQP GitHub Site. In brief...

Zenodo.org is a permanent, publicly accessible scientific data repository funded by the European Union via CERN
HamSCI's plan for the WAV files: Develop an 'ping algorithm' - a method of identifying MSK144 decodes via meteor scatter vs. other propagation modes, such as sporadic E, tropo or simple F layer refraction. If we are successful, we will run all of the WAV files through the algorithm, classifying the MSK144 decodes according to propagation method. Then, we can examine the decodes according to our science objectives.
Uploading to Zenodo requires a user account/login ID/password. There is no cost, no obligation, and perhaps best of all, no spam once your account is active!
Be sure to locate the WAV file directory on your computer, and ZIP all of your MSQP WAV files (those covering the shower time period during which you are operating) into one file - that simplifies the upload process
Note that the instructions mention the HamSCI Community on Zenodo. Please follow that step - so we have everyone's data consolidated under the HamSCI name
Save your login credentials in a safe place - you can use them again after future MSQPs, and for other research campaigns sponsored by HamSCI
If you have questions on any aspect of the MSQP, including the entry and WAV file upload process, please email us: hamsci@hamsci.org

Thank you, in advance, for taking this important step in the name of citizen science and radio wave propagation research!

V) MSQP Leader Board

***UNDER DEVELOPMENT - Target date, July, 2026***

HamSCI will be creating a 'Leader Board', likely to be based on the number and quality of WAV file decides submitted after each event (submissions should be made to Zenodo.org, see Section VIII below.

The HamSCI Research Team greatly appreciates all who contribute to the Meteor Scatter QSO Party. The Team would like to recognize all participants via postings on the HamSCI website and in other media.

VI) Science Objectives

Generate research-worthy data resulting from 6 and 10 meter meteor scatter operation. The data will be used by the research community in an attempt to answer science questions, such as:

What factors influence meteor scatter propagation?
- What are the similarities and differences between HF and VHF meteor scatter propagation?
- How does propagation change between the various sporadic sources and minor showers with their different speeds and radiant geometries?
- How does propagation change with radiant geometries, trail direction, meteoroid size, and speed?
What is the typical duration of useful meteor scatter propagation?
- How does this duration vary with operating frequency, transmitter–receiver distance, and meteor velocity?
What is the minimum size of an amateur radio station needed to work meteor scatter operations?
- What defines a 'successful' MS station? Power levels? Antenna type (directionality, gain, elevation, height, polarization)? System ERP (effective radiated power)?
- Does the definition of a 'successful' station (judged by both the number of contacts and the contact distances) vary between HF and VHF bands? If so, what are the differences?
How can meteor scatter communication be distinguished from other propagation modes?
- What percentage of reported meteor scatter QSOs are actually meteor scatter?
- What percentage are due to other modes (e.g., tropospheric, F-layer, E-layer, auroral)?
How do optical and radar meteor observations compare with amateur radio observations?

The target communities include: Seasoned meteor scatter operators, meteor scatter 'rookies' (those who are new to the mode), researchers with an interest in radio wave propagation. Data sources will include participant's log files (ADIF format), 'spotting' databases, such as PSKReporter.info and operators' WAV files from MSK144 decodes.

This is Version 4.0 of the MSQP Operating Rules and Guidelines, dated 3 May 2026