MS sprint contest
“ 144 MHz Meteorscatter Sprint Contest 2026 “
MMMonVHF[1], in cooperation with the magazines DUBUS[2] and Funk-Telegramm[3], invites you to take part in the 19th edition of the “144 MHz Meteorscatter Sprint Contest” during the maximum of the Perseids meteor shower (PER). Based on predictions from IMO[4] (the International Meteor Organisation), this maximum will occur on August 13, 2026, between 02:00 GMT and 04:00 GMT.
RULES:
Contestperiod:
August 12, 2026, 07.00 GMT – August 14, 2026, 07.00 GMT (end time last completed QSO).
Participation:
Class 1: QRP (< 1.5 kW ERP)
Class 2: QRO (>1.5 kW ERP)
Stations can participate in one class only. No difference between single- or multioperator stations or modes.
Exchange:
Full callsigns, reports (e.g. 26 or R26) and final rogers (RRRR)[5].
Scoring:
For each completed QSO you receive an amount of points that equals the distance between you and the station you completed with. A worked station only counts once, so no duplicates allowed.
Final scoring:
The total score is the sum of all points you received for all completed QSO’s together.
Logs:
Logs can be send via E-mail or regular mail. Your log has to be received before September 15, 2026. In case you have send your log by regular mail, the postmark will count. Logs received after that date will be considered as checklogs.
Logs via E-mail can be sent to: mssprint@mmmonvhf.de ; Subject: MSSprint “Call”
Logs via regular post can be sent to: A.F. Veldhuijsen, PA4EME,
Westlandstraat 9,
6137 KE Sittard,
The Netherlands.
Be sure you log contains at least the following:
- Your call, name, adress and class you want to participate in. Stations in Class 1 (QRP) have to state details about the equipment they used in form of used output power and antennagain. If no data about your station is given, you will be placed in Class 2. The power used for the calculation of the Effective Radiated Power will be the power measured at the output of your transceiver or active amplifier(s);
- The QSO list. As there are many logging programs available nearly every format is possible[6]. But make sure that the log will show at least: date, time (to be specific: end time), call, report send, report received, locator and distance (equals points).
With sending your log you also declare to have operated within the limits of your chosen Class, licence and local regulations when performing any activity that could impact your submitted score. Unsportsmanlike conduct can be ground for disqualification. Also you agree to have the log open to the public which might result in publishing your log on MMMonVHF or in the magazines DUBUS and/or Funk-Telegramm.
Reception of a log will be confirmed in the same way it was received.
Stories and pictures are welcome for the soapbox.
Conditions to be observed:
The use of DX-clusters and chat-channels during the contest is only allowed in such way that there is no exchange of reports or other data from which the status of the QSO can be extracted. Limited information on the cluster (e.g. 12:00 DK5EW PA4EME JN48MB<MS>JO20WX) or chat (e.g. 12:00 PA2DW 144.355 CQ for MS Sprint) is allowed.
Selfspotting exceeding more then once every 15 minutes will be considered as unsportsmanlike behaviour.
Winner of the contest:
The winner of the contest is the station with the highest amount of points. There will be a winner in each class. If two stations have the same amount of points, the position will have to be shared.
Special scoring for outside Europe stations:
There will be a seperate listing for stations outside Europe.
Certificate:
All stations will receive a digital certificate showing the Class and ranking achieved.
Results:
The results of the MS Sprint Contest will be published on October 1th 2026 online on MMMonVHF. They will appear in various magazines as well.
Additional notes:
[1] MMMonVHF (Make More Miles on VHF): www.mmmonvhf.de
[2] DUBUS - the serious magazine for VHF and up amateur radio: www.dubus.org
[3] Funk-Telegramm - Magazin für Funkamateure: www.funk-telegramm.de
[4] IMO – International Meteor Organisation: www.imo.net
[5] Operating Procedures for Meteor Scatter QSO’s: http://www.vhfdx.de/ms_howto.pdf
[5] Проведение MS QSO в 1 районе IARU: http://www.vhfdx.ru/ms/provedenie-ms-qso-v-1-rayone-iaru
[6] The “144 MHz Meteorscatter Sprint Contest” is supported by at least two software
programs:
- Arcom (Ham Office) : www.hamoffice.de
- Ucxlog : www.ucxlog.de
Other logging programs are allowed as well.
More data on Perseids (007) by the International Meteor Organization (https://www.imo.net/resources/calendar/)
Perseids (007 PER) Active: July 17–August 24; Maximum: August 13, 02h to 04h UT (node at λ⊙ = 140 . â—¦0 − 140 . â—¦1), but see text; ZHR = 100; Radiant: α = 48â—¦ , δ = +58â—¦ ; Radiant drift: see Table 6; V∞ = 59 km/s; r = 2.2. Previous IMO observations (see WB pp. 32–36) found the timing of the mean or ‘traditional’ broad maximum varied between λ⊙ ≈ 139 . â—¦8 to 140 . â—¦3, equivalent to 2026 August 12, 21h − 09h UT. The orbital period of the parent comet 109P/Swift-Tuttle is about 130 years. The Perseids produced strong activity from a primary maximum throughout the 1990s. Enhanced activity was last observed in 2016 due to passages through separated dust trails. High activity well after the main peak has been reported during some recent returns in 2018, 2020 and 2021 about 0.7 to 1.5 days after the main maximum. Nothing similar was observed in 2022—2024. Maslov’s modelling indicates that the background (permanent) activity is expected to be notably lower than the usually quoted ZHR of 100 until 2026. Only in 2027 will the Earth pass sections of the stream that have been disturbed by Jupiter once more, which may then cause higher general rates again. Vaubaillon’s calculations show an approach to the 1079 dust trail in 2026. The trail is split into three parts. The Earth is expected to encounter one of these branches on August 12 at 16h53m UT (λ⊙ = 139 . â—¦859). Since it is a very old trail, no activity estimate is given. An encounter of a weak filament of 109P is listed in Table 5d of Jenniskens (2006). The calculated position is λ⊙ = 139 . â—¦97 ± 0 . â—¦2, corresponding to 2026 August 13, 01hUT (±5 h ). The expected ZHR of ≤ 43 is similar to the calculated filaments in 2013, 2014 and 2025 ((the latter still to come when this Calendar was written). Although the calculated filament occurs close to the main maximum and only shortly after the above mentioned 1079 trail passage, the trail and filament may become detectable if the background rate is lower. Since the trail and filament meteoroid size distribution may be different, it is advised to report also magnitude data for intervals of 30 minutes or less. New Moon on August 12 provides excellent conditions for all optical observations. With all the extra events seen after the nodal peak during some past returns it is recommended to include the nights around the main maximum in the observing program to record peculiarities. Mid-northern latitude sites are best for Perseid observing, as from here, the radiant has reached a reasonable elevation from 22h–23h local time onwards. Regrettably, the shower cannot be properly viewed from most of the southern hemisphere, or from latitudes north of about 60â—¦N.
![](<img%20src="https://public.tableau.com/static/images/BX/BXY8CPR3B/1_rss.png">)
“ 144 MHz Meteorscatter Sprint Contest 2026 “
MMMonVHF[1], in cooperation with the magazines DUBUS[2] and Funk-Telegramm[3], invites you to take part in the 19th edition of the “144 MHz Meteorscatter Sprint Contest” during the maximum of the Perseids meteor shower (PER). Based on predictions from IMO[4] (the International Meteor Organisation), this maximum will occur on August 13, 2026, between 02:00 GMT and 04:00 GMT.
RULES:
Contestperiod:
August 12, 2026, 07.00 GMT – August 14, 2026, 07.00 GMT (end time last completed QSO).
Participation:
Class 1: QRP (< 1.5 kW ERP)
Class 2: QRO (>1.5 kW ERP)
Stations can participate in one class only. No difference between single- or multioperator stations or modes.
Exchange:
Full callsigns, reports (e.g. 26 or R26) and final rogers (RRRR)[5].
Scoring:
For each completed QSO you receive an amount of points that equals the distance between you and the station you completed with. A worked station only counts once, so no duplicates allowed.
Final scoring:
The total score is the sum of all points you received for all completed QSO’s together.
Logs:
Logs can be send via E-mail or regular mail. Your log has to be received before September 15, 2026. In case you have send your log by regular mail, the postmark will count. Logs received after that date will be considered as checklogs.
Logs via E-mail can be sent to: mssprint@mmmonvhf.de ; Subject: MSSprint “Call”
Logs via regular post can be sent to: A.F. Veldhuijsen, PA4EME,
Westlandstraat 9,
6137 KE Sittard,
The Netherlands.
Be sure you log contains at least the following:
- Your call, name, adress and class you want to participate in. Stations in Class 1 (QRP) have to state details about the equipment they used in form of used output power and antennagain. If no data about your station is given, you will be placed in Class 2. The power used for the calculation of the Effective Radiated Power will be the power measured at the output of your transceiver or active amplifier(s);
- The QSO list. As there are many logging programs available nearly every format is possible[6]. But make sure that the log will show at least: date, time (to be specific: end time), call, report send, report received, locator and distance (equals points).
With sending your log you also declare to have operated within the limits of your chosen Class, licence and local regulations when performing any activity that could impact your submitted score. Unsportsmanlike conduct can be ground for disqualification. Also you agree to have the log open to the public which might result in publishing your log on MMMonVHF or in the magazines DUBUS and/or Funk-Telegramm.
Reception of a log will be confirmed in the same way it was received.
Stories and pictures are welcome for the soapbox.
Conditions to be observed:
The use of DX-clusters and chat-channels during the contest is only allowed in such way that there is no exchange of reports or other data from which the status of the QSO can be extracted. Limited information on the cluster (e.g. 12:00 DK5EW PA4EME JN48MB<MS>JO20WX) or chat (e.g. 12:00 PA2DW 144.355 CQ for MS Sprint) is allowed.
Selfspotting exceeding more then once every 15 minutes will be considered as unsportsmanlike behaviour.
Winner of the contest:
The winner of the contest is the station with the highest amount of points. There will be a winner in each class. If two stations have the same amount of points, the position will have to be shared.
Special scoring for outside Europe stations:
There will be a seperate listing for stations outside Europe.
Certificate:
All stations will receive a digital certificate showing the Class and ranking achieved.
Results:
The results of the MS Sprint Contest will be published on October 1th 2026 online on MMMonVHF. They will appear in various magazines as well.
Additional notes:
[1] MMMonVHF (Make More Miles on VHF): www.mmmonvhf.de
[2] DUBUS - the serious magazine for VHF and up amateur radio: www.dubus.org
[3] Funk-Telegramm - Magazin für Funkamateure: www.funk-telegramm.de
[4] IMO – International Meteor Organisation: www.imo.net
[5] Operating Procedures for Meteor Scatter QSO’s: http://www.vhfdx.de/ms_howto.pdf
[5] Проведение MS QSO в 1 районе IARU: http://www.vhfdx.ru/ms/provedenie-ms-qso-v-1-rayone-iaru
[6] The “144 MHz Meteorscatter Sprint Contest” is supported by at least two software
programs:
- Arcom (Ham Office) : www.hamoffice.de
- Ucxlog : www.ucxlog.de
Other logging programs are allowed as well.
More data on Perseids (007) by the International Meteor Organization (https://www.imo.net/resources/calendar/)
Perseids (007 PER) Active: July 17–August 24; Maximum: August 13, 02h to 04h UT (node at λ⊙ = 140 . â—¦0 − 140 . â—¦1), but see text; ZHR = 100; Radiant: α = 48â—¦ , δ = +58â—¦ ; Radiant drift: see Table 6; V∞ = 59 km/s; r = 2.2. Previous IMO observations (see WB pp. 32–36) found the timing of the mean or ‘traditional’ broad maximum varied between λ⊙ ≈ 139 . â—¦8 to 140 . â—¦3, equivalent to 2026 August 12, 21h − 09h UT. The orbital period of the parent comet 109P/Swift-Tuttle is about 130 years. The Perseids produced strong activity from a primary maximum throughout the 1990s. Enhanced activity was last observed in 2016 due to passages through separated dust trails. High activity well after the main peak has been reported during some recent returns in 2018, 2020 and 2021 about 0.7 to 1.5 days after the main maximum. Nothing similar was observed in 2022—2024. Maslov’s modelling indicates that the background (permanent) activity is expected to be notably lower than the usually quoted ZHR of 100 until 2026. Only in 2027 will the Earth pass sections of the stream that have been disturbed by Jupiter once more, which may then cause higher general rates again. Vaubaillon’s calculations show an approach to the 1079 dust trail in 2026. The trail is split into three parts. The Earth is expected to encounter one of these branches on August 12 at 16h53m UT (λ⊙ = 139 . â—¦859). Since it is a very old trail, no activity estimate is given. An encounter of a weak filament of 109P is listed in Table 5d of Jenniskens (2006). The calculated position is λ⊙ = 139 . â—¦97 ± 0 . â—¦2, corresponding to 2026 August 13, 01hUT (±5 h ). The expected ZHR of ≤ 43 is similar to the calculated filaments in 2013, 2014 and 2025 ((the latter still to come when this Calendar was written). Although the calculated filament occurs close to the main maximum and only shortly after the above mentioned 1079 trail passage, the trail and filament may become detectable if the background rate is lower. Since the trail and filament meteoroid size distribution may be different, it is advised to report also magnitude data for intervals of 30 minutes or less. New Moon on August 12 provides excellent conditions for all optical observations. With all the extra events seen after the nodal peak during some past returns it is recommended to include the nights around the main maximum in the observing program to record peculiarities. Mid-northern latitude sites are best for Perseid observing, as from here, the radiant has reached a reasonable elevation from 22h–23h local time onwards. Regrettably, the shower cannot be properly viewed from most of the southern hemisphere, or from latitudes north of about 60â—¦N.