Overview

The three-channel GRAPE 2 Doppler Monitor (fldigi version) is a key component of the HamSCI Personal Space Weather Station (PSWS).  It could be considered the 'next generation' of GRAPE receiver, released just prior to the April 8, 2024 North American solar Eclipse.   It is used for receiving, analyzing and recording of signals from frequency standard stations such as WWV/H and CHU. The PSWS project involves monitoring changes in the Earth's ionosphere through measurements of Doppler frequency shifts on a 24/7 basis. 

The Grape 2 could be considered the 'big brother' of the GRAPE PSWS family. It is capable of receiving three frequencies simultaneously, utilizing a GPS disciplined oscillator for making precise frequency measurements.  A complete GRAPE 2 PSWS system (as pictured above) consists of the following: Grape 2 Receiver and Logic PC boards, Teensy microcontroller, Raspberry Pi 4, external hard drive, power supply and two antennas, one for the GPS and one for the time standard frequencies. Ideally, every Grape 2 should have access to a reasonably fast (>100Mb/S) Internet connection for data uploads. There is a provision to buffer and transmit buffered data at a later time if the connection is lost. Data collected by the GRAPE 2 is intended to be uploaded on a daily basis to a HamSCI server.   The data collected by a Grape 2 can be used to generate plots of Doppler shift vs. UTC hour.  A sample plot from  April 8, 2024 (the date of the recent North American total solar eclipse) appears above.  (The solar eclipse's effect on the ionosphere is clearly visible between about 1800 and 2100 UTC.)

Specifications

Grape 2 User Manual

The Grape 2 User Manual Version 1.2 was sent out in March of 2024, as part of the original deployment. It can be found here on the HamSCI website.

Sourcing

Approximately 30 GRAPE 2s were manufactured and tested late in Q1, 2024. They were deployed in accordance with terms of the grants which funded the project: A map of the stations appears on this page. They were on line and uploading data during the April 8, 2024 North American total solar eclipse. It is HamSCI's expectation that all will be kept running, on a 24/7/365 basis, for years to come, studying the behavior of the ionosphere during Solar Cycle 25. Further, some GRAPE 2 installations included remote magnetometer boards, used to measure minute changes in the Earth's magnetic field. That data was sent to the same HamSCI server.

Occasionally, units are returned to HamSCI for redeployment.  If you are interested in hosting a grand-funded GRAPE 2, please send your contact info, including location (grid square and city/state/province) to [email protected].  Note that grantees are expected to have basic Linux experience, an HF (shortwave) antenna, and common computing peripherals (USB keyboard/mouse, monitor) and an Internet connection for daily data uploads. Of course, we can't guarantee availability but we are very interested in having as many systems running as possible.

Grape 2 Update - Disk Drive Swap - March/April, 2025

While some data was uploaded to HamSCI data collection servers on a daily basis (a very narrow band of digitized audio, centered 1 kHz below the three time station carriers received) a great deal more data (~3KHz bandwidth, ~10.4GB per day) was captured and stored locally on each Grape 2's hard drive.  The 4TB drives are filling up, so new drives are being provided to each Grape 2 host.  We ask that you follow this procedure to make the swap.  Questions are best raised to the HamSCI Grape Google Group.  Provisions have been made for hosts to ship the old drives to the University of Alabama, where the data will be extracted and uploaded to the PSWS Central Control System.

Further Information

• Support is available from the HamSCI-psws Google Group.  All are welcome to join, ask questions, assist others on their GRAPE journeys.
• HamSCI explains The Science Behind the Grape Doppler Monitor
• In mid-October, 2023, while an annular solar eclipse which transited North and South America, over 50 GRAPE 1 systems were in operation, uploading research-worthy data. The GRAPE project contributors from that time period are noted on the GRAPE 1 Recognition and Acknowledgement page.  
• The GRAPE 1 is just one module of the HamSCI Personal Space Weather Station (PSWS)  Learn more here:  Overview of the Personal Space Weather Station (PSWS)

Images of the Grape 2 under development at the bench of John Gibbons, N8OBJ:

Grape 2 Hosts

30 Grape Version 2s were deployed prior to the April 8, 2024 total solar eclipse over North America.  The host stations are shown on this map.

Credits

The Grape Version 2 was designed by John Gibbons, N8OBJ, Lab Director of the Sears Undergraduate Electrical Design Lab, Case Western Reserve University, Department of Electrical Engineering. Software applications were written by Bill Blackwell, AB1XB and Cuong Nguyen, KC3UAX. The remote magnetometer board was designed, built and provided to host stations by David Witten, KD0EAG. Dr. Nathaniel Frissell, W2NAF, was the Principal Investigator on National Science Foundation grant 2230345 ('Collaborative Research: CEDAR: Measuring Daily Ionospheric Variability and the 2023 & 2024 Solar Eclipse Ionospheric Impacts Using HamSCI HF Doppler Shift Receivers'). Their efforts were supported by additional NSF grants (2002278, 1922972, 1932997, 2230346) and these institutions:

17 October 2025:  Updated PSWS CCS URL - af8a

This page accompanies descriptions of the following PSWS components

• Grape 1 fldigi
• Grape 1 DRF

Design Documentation for the GRAPE 1 Low IF Receiver PC Board

​Grape V1.11 Block Diagram: PSWS_GrapeLowCostBlockDiagram.pdf

Grape V1.12 Schematic:  WWV_Radio_V1_12_sch.pdf

Additional design details are on this Mendeley site:  data.mendeley.com/datasets/nbbhy2yxmz.  It holds mostly 'low level' documentation, such as PC board manufacturing files (top, bottom traces, solder mask, lettering), PSWS File Name Requirements, Fldigi source code, the Python routines which make the Grape 1 PSWS 'run' on a daily basis, and more.   Some of the details are for earlier versions of hardware and software, so read carefully if you visit this site.

Building the GRAPE 1 PSWS

Building the a GRAPE 1 PSWS is not as easy as the old HealthKits used to be.  For starters, there is no kit of components.  The instructions are fairly complete, but they are not 'cookbook style'.  It will take some digging and planning on the part of the builder.  Fortunately, help is not far away:  Join the hamsci-psws Google group and you'll find many others who've 'been there, done that' and who can help you if you get stuck.  You can also navigate over to the Google group and 'search' on any topic or question you might have.  It's possible that the answer you are looking for will appear in the search results!

Note:  The Grape 1, like many open source projects, is a work in progress.  The Grape documentation was begun in 2022 and has been updated many times (for new hardware, new software) right up to today.  Here it is separated into the most current (Grape 1.12) and older documentation, which, while not correct in every detail, is still quite useful.  See note above on hamsci-psws Google group - the group members are a wonderful resource.

Grape V1.12: Bare PC Board Ordering Link from OSHPark.com:  oshpark.com/shared_projects/9Z2fhMYW

Grape V1.12: PC Board Bill of Material (BOM):  WWV_Radio_V1_12_bom.txt

Grape V1.12: PC Board BOM Components Order Link from DigiKey.com:  www.digikey.com/short/cqdvrhjf

Grape V1.12: How to Request a Node Number: See Step #65 in this document:  MakeGrape1OSImageV1_05.pdf

Grape V1.12: STL File for a 3D printed case to hold a Grape 1.12 receiver PC board, courtesy of John Hysell, K2HJ:  Grape Case rev2.1.stl (most resent mod as of 29 March, added opening for frequency selection jumper)

Grape V1.12: One Ham's Perspective on Building a Grape from scratch. This paper contains good explanations of the fldigi waterfall and the daily graph of Doppler shift and received signal strength: K4BSE_Grape 1.12 Document v1-2.pdf

Grape PSWS Fldigi System Component List: (GPSDO, Audio interface, Raspberry Pi, cabling, etc.): GrapeGen1_SuppliesList.pdf

Obtaining the Grape PSWS Raspberry Pi Image File:  Navigate to Zenodo, www.doi.org/10.5281/zenodo.8305995   You will find a very large file called Grape1_OSGen1E.img. Download the file and follow Installing the Gen1E Grape Image instructions (see below) to burn the image onto an SD Card.

Installing the Gen1E Grape 1 Image and Configuring the Raspberry Pi: A step by step procedure that covers everything from burning the image onto an SD card to setting up your Raspberry Pi on a wifi network to uploading data to the Grape1 fldigi data repository: MakeGrape1OSImageV1_05.pdf

Grape Build Instructions, Testing, System Assembly and Operation:   Hardware X Paper on Grape 1 (2022). NOTE:  This document was written for a previous hardware version, so the PC board component lists, schematics and file names are not accurate for the V1.12 PCB.  However, the majority of the instructions in Sections 5, 6 and 7 do apply to version 1.12. (An on-line version of the paper is available at doi.org/10.1016/j.ohx.2022.e00289 )

Credits

The Grape Version 1 was designed by John Gibbons, N8OBJ, Lab Director of the Sears Undergraduate Electrical Design Lab, Case Western Reserve University, Department of Electrical Engineering. Please see the Grape 1 Contributors page for acknowledgement of the entire Grape 1 team.

The HamSCI Personal Space Weather Station project is led The University of Scranton Department of Physics and Engineering W3USR, in collaboration with Case Western Reserve University W8EDU, the University of Alabama, the New Jersey Institute of Technology Center for Solar Terrestrial Physics K2MFF, the MIT Haystack Observatory, TAPR, additional collaborating universities and institutions, and volunteer members of the amateur radio and citizen science communities. HamSCI wishes to acknowledge National Science Foundation grants AGS-2002278, AGS-2230345, AGS-1932997, AGS-2230346, AGS-1932972 for support of the PSWS project.

This page is an archival copy of the GRAPE PSWS page from the 2020-2023 era.  We suggest you visit the latest HamSCI PSWS pages for current information

The Grape* PSWS Project - A Distributed Array of Software Defined Receivers 

The HamSCI Personal Space Weather Station (PSWS) Project is making available, to the radio hobbyist and space physics communities, a distributed array of Low IF radio receivers. They are designed with a specific purpose in mind:  Recording changes in the Earth's ionosphere through measurements of Doppler frequency shifts observed by monitoring, on a 24/7 basis, frequency standard stations such as WWV/H and CHU.

Ham radio operators and other shortwave enthusiasts are encouraged to host Grape receivers at their stations from now until well after the total North American solar eclipse on April 8, 2024.  Hosting involves providing reliable power, space for an antenna and an Internet connection.  Other factors come into play, such as the need for visibility to the constellation of GPS satellites.

The science behind the Grape PSWS project is described below.  In short, the array of Grape PSWS receive signals from the frequency standard stations, make extremely accurate measurements of the received frequency, record and then upload the data.  Measurements accuracies are in the milliHertz range.  Space physicists and citizen scientists can then use those measurements to study the effects of solar phenomena (e.g., flares, CMEs and eclipses) on the ionosphere.   

*Why is it called 'Grape'?  Because it is the Great Radio Amateur Propagation Experiment, and because Grapes work best in 'bunches' - the more deployed to the field, the better!

Grape 1 fldigi and Grape 1 DRF:  Single-Channel Receivers

Grape 1s are designed for DIY enthusiasts. The single-frequency receiver portion is built by the user on a PC board using surface mount components. The user then has to obtain and assemble the system components, such as a GPS disciplined oscillator, a Raspberry Pi, USB audio interface, power supply, storage medium and antenna. All components are readily available and thoroughly documented. Note that Grapes are like any hardware/software based product; they have evolved  over time and there are multiple versions in use. 

1. The first Grape systems run a highly modified version of fldigi software.  Dozens are in use, collecting data on a 24/7/365 basis. Each system uploads data, once per day, to a server hosted by the WWV ARC. Grape fldigi data has been collected since 2019. Those Grapes provide valuable data and are expected to keep running throughout 2023 and 2024.  Construction and software details, along with information on initiating the data collection and uploading processes, are on the Grape 1 page. 
2. Grape 1 systems running GNU Radio software, collecting data in the Digital Radio Format, was released in September of 2023.  It is the first Grape model to upload data to the Personal Space Weather Station Central Control System.  Construction details are located on the Grape 1 page, while guides to the software, data collection methods and more are on the Grape 1 DRF documentation page.  

The Grape 2 Multi-Channel Receiver

The Grape 2 is more sophisticated 3-channel receiver. However, the extra complexity requires that the PC boards be commercially built. Over 30 Grape 2s were deployed prior to the April 8, 2024 total solar eclipse over North America.  Details, photos and a map of the host stations are on the Grape 2 web page.

Please note that the Grape Low IF radios are not general purpose receivers. They are designed to receive signals only on frequencies pertinent to the research.

How Can I Participate?

HamSCI strongly encourages anyone with interest and/or experience in the areas of shortwave radio reception, kit building, system assembly, single-board computer application to read through the details on the Grape 1 and 2 and decide which approach would be best for you.

1. Grape 1 sites require no registration beyond requesting a node number for uploading data to the a central server (data repository). Directions for obtaining a node number are on the Grape 1 page.
2. Approximately 30 Grape 2 sites were funded through research grants.  All have been deployed.  There are no plans for building additional units, though that could change in the future. 

All Grape participants should join the hamsci-grape Google Group.  All are welcome to participate in weekly Grape Zoom calls to share hints, hacks, and results.  Questions are always welcome - if you have a question, chances are that many others have the same question - the community is very welcoming in that regard.  (The Zoom calls are recorded and made available on the HamSCI YouTube channel.)

The Science Behind the Grape PSWS Project

The following is an abbreviated summary of the science behind the Grape PSWS network and how the Grape creates valuable data for scientific study.  It is recommended that the reader follow the links at the end of this section to gain a full understanding of the concepts described here.   Before diving in, it would be helpful to understand Doppler effect, and also to be aware of the HamSCI glossary.

Scientific Interests

The PSWS network has proven to be useful in the study of short-term (lasting hours to days) geophysical and solar events, such as traveling ionospheric disturbances, solar flares, solar eclipses and geomagnetic storms.  It does so by observing the bottom side of the ionosphere.  Data from PSWS member stations, often combined with observations from other scientific instruments, yields clues as to how and why those events impact HF (high-frequency, 3–30 MHz) radio wave propagation.  The data can also be used to improve mathematical models of the ionosphere, which should result in more accurate predictions of HF propagation (such as maps of the MUF and critical frequencies). 

Role of the Grape PSWS

HF Doppler sounding is an established means of observing the bottom side of the ionosphere. Its principle of operation is straightforward: A shift in signal path length causes a corresponding Doppler shift (Figure 1). The Grape receiver performs Doppler measurements by measuring the carrier freqency of frequency standard stations such as WWV/H (or CHU). Their transmit frequency accuracy and stability is less than one part in 10^13 - an incredibly small value.  Measurements of the WWV/H frequency at a distant receiver site is limited by a few factors, one of which is the receiver’s accuracy and stability, the other is the propagation path.  The former is well accounted for in the design of the PSWS, the latter is the primary measurement of interest.  In other words, those who study the PSWS measurements are not overly concerned about the absolute value of the receive frequency, but they are extremely interested in the variation of the received frequency over time (typical PSWS datasets are broken into 24 hour periods) (Figure 2).

Figure 1: A simplified illustration of the relationship between rate of change in ionospheric layer height and received frequency shift. Precision frequency standards are required at both beacon and receiver in order to make an effective comparison. Frequency variation is generally on the order of ±1 Hz. Multihop propagation (multiple reflections between ionosphere and ground), Pedersen modes (internal ionospheric reflections), asymmetric paths, and other factors impacting path length are not shown. Reproduced from Collins et al. (2022).

Figure 2:  Annotated frequency and amplitude plots of Node 1's 5 MHz data from 28 October 2021, with sunrise and sunset indicated by background shading. The filtered result is superimposed on the raw data. The day's sunrise peak is clearly visible. The horizontal axis is plotted in mean solar time, rather than UTC, in order to emphasize the effects of the 24-hour day/night cycle. A Doppler flash associated with an X-class solar flare is evident around 15:30 UTC. Reproduced from Collins et al. (2022).

For further information, please review these papers, presentations and posters.  More on this subject can be found in the Publications on this site.

• Grape Personal Space Weather Station Doppler Observations (peer reviewed paper)
• The potential of HamSCI Doppler Observations for inferring Solar Flare Effects on the Ionosphere (conference proceeding)
• HF Doppler Observations of Traveling Ionospheric Disturbances in a WWV Signal Received with a Network of Low Cost HamSCI Personal Space Weather Stations (poster and explanatory video)

Grape PSWS Project Sponsors and Supporters

17 October 2025:  Updated PSWS CCS URL - af8a

Ver 1.2  (10 May 2024 - Removed 'day of event' info.  Added doc on results analysis)

Updates:  Download the new document on TDOA Chirp Analysis  and see comments on Reporting Results

Background

The April 8, 2024 annular solar eclipse offered a unique opportunity to study an eclipse's influence on ionospheric dynamics, particularly on the layers of the ionosphere which are responsible for the propagation of radio waves in the HF (3-30 MHz) band. The science questions pertinent to this event:

• What is the observed change in effective F2 ionization layer height caused by the momentary blockage of solar radiation?
• Is symmetry observed in layer height changes when comparing 'before eclipse' and 'after eclipse' layer heights?   

General Methodology 

Over propagation paths that support transmission of multiple hops, test waveforms were used to measure HF signals' Time Difference of Arrival (TDOA) between multipath modes. For this event it was the 1- and 2- hop modes from the F2 layer that were of interest because:

• F2 layer height is most sensitive to sunlight variations,
• Simultaneous propagation of both modes frequently occurs on frequencies below 10 MHz, 
• TDOA information can be used to infer F2 layer height. 

The test waveforms consisted of very short pulses plus an audio chirp. They were reasonably simple to transmit, receive and analyze by amateur radio operators.  A full explanation (theory, methods, on-air validation) of the TDOA technique is here on the HamSCI site.  The last page of that document contains references for further exploration.

HamSCI recruited dozens of stations capable of transmitting, receiving and recording WAV or MP3 files on 40, 60, 75 and 160 meters using SSB signals during the eclipse, looking for pairs of stations operating across North America.  Pairs were located such that the stations were on opposite sides of the eclipse path, parallel to the eclipse path and at some distance from the eclipse path.   A sample of the pre-registrants is listed below.  

Operational Details (Manual method, transmit and receive)

• Dawn transition measurements:  Look for WA5FRF and others on 7250, at 1200 UTC on 8 Apr 2024.  
• Eclipse measurements:  Look for WA5FRF and others on 7250, at 1600 UTC on 8 Apr 2024
• If the frequency is busy, the group will slide up a few kHz.  If a major shift is needed, it will be announced on HamSCI's Google Group.  Other bands may come into play after the initial tests on 40 meters.  Connect to the day-of-event Zoom meeting for updates.
• Participating stations will be asked to work in pairs or small groups.   
• QSOs will established between at least two members of the group.  Others can simply listen, recording the chip audio, or they may choose to transmit their own chirp signals for others to receive/record, as in a 'roundtable' QSO.
• A chirp waveform will be transmitted from one station to another multiple times during the solar eclipse period.  (Use enough power to consistently maintain a good signal.)
• Options:  One station does the chirp transmitting (T), the other(s) the receiving/recording (R).  Even better would be to alternate:  Station A transmits, Station B receives.  Then, Station B transmits and Station A receives
• Multiple T/R sessions are needed throughout the eclipse period.  A station should be prepared to transmit a chirp signal every 6 to 10 minutes, over 2 or more hours - for at least an hour prior to maximum annularity near your QTH, and for at least an hour after.
• Save received files with callsign, date and time stamps in their names (eg W5XXX-14 Oct-1650Z.WAV)
• Help the HamSCI science team with the results analysis.  Here is a paper on a manual method for analyzing TDOA results: 2024-05-04 TDOA Chirp Analysis for NVIS.docx

Operating Tips - for Successful Transmitting and Receiving 

•   Pre-Event Checklist V4, authored by Steve Cerwin, WA5FRF
• Please review this PDF file, TDOA Operating Tips, authored by Steve Cerwin, WA5FRF.

Preparation - Before the Solar Eclipse (8 April 2024)

1. Please pre-register as a TDOA Event participant.  There is no obligation for pre-registration, but doing so helps the study authors gage interest and the geographic dispersion of interested parties.  You are welcome to identify the stations with whom you would like to operate during the TDOA Event.
2. Verify that your station can cleanly transmit and/or receive WAV or MP3 files.  A sound card interface (eg SignaLink, microHAM), or a radio which appears as an audio device over USB (eg Icom 7300, 7610, Elecraft K4 series, Kenwood TS-590SG) will work equally well.
3. For transmitting stations, create and test to be sure your computer (or HF transmitter) can load and play the Science Payload files noted in #4, below
4. If you will be participating in the HamSCI TDOA as a transmitting station during the upcoming eclipse, please generate this new personalized .wav file for your use.  This file has many modifications made from the previous file we used during the 2023 annular eclipse.  The changes were made to permit a more robust data recovery.  The link to create the new .wav file can be found by clicking on the README file at the bottom of:  https://github.com/jtm5/HamSCI_TDOA_SigGen
5. For receiving stations, prepare a directory on your shack computer for storing the recordings (which we will ask you to upload to the HamSCI/TDOA data repository after the eclipse).
6. Plan your solar eclipse operating around the time when the eclipse path is closest to your QTH.  NASA's Eclipse Explorer can provide detailed path information. 

Here you can listen to a test waveform (~18 seconds long) consisting of a 1 KHz 'calibration' tone, white noise, short pulses, ten repetitions of the 'chirp' signals, more white noise and another 1KHz calibration tone.  We suggest right clicking the appropriate link, and choosing 'Open in a new browser tab (or window) to listen or download.

Mac OS:   SEQP Test Signal_v5_Science-payload.wav

Windows OS:  SEQP Test Signal_v5_Science-payload.mp3

Interest List

​The following is a sampling of stations who expressed an interest in participating. 

Reporting Results

The research community uses various public databases to store data collected in these events.  They allow for open access, and long-term (many years') storage.  Once the database has been chosen and upload procedures established, they will be shared with all participants via email.  If you have questions about where or how to upload data, please contact Steve Cerwin or [email protected]

Scoring and Post-Event Recognition

Unlike other the other events to be held during the Festivals of Eclipse Ionospheric Science (add link), the TDOA Event is not a competition.  All participants will be acknowledged via listings on the HamSCI website.  There is the possibility that one or more participating stations will receive mention in future studies, presentations and research papers.  Regardless, everyone will earn the gratitude of the ionospheric science community.  Only through experimentation, data gathering, rigorous analysis and sharing of results can we make progress towards understanding the physical world in which we live and operate our stations.

Credits

• The TDOA Event stems from work originated by Steve Cerwin WA5FRF with assistance from the WWV/H Scientific Modulation Working Group.
• Code for generating the chirp file is courtesy of Aidan Montare KB3UMD and Dr. Kristina Collins KD8OXT
• Web page authored by Gary Mikitin AF8A

Overview

HamSCI will be present at the 2023 Dayton/Xenia Hamvention in order to further its goal of connecting the ham radio and scientific communities. Support for the 2023 HamSCI Hamvention activities comes from The University of Scranton, The Yasme Foundation, TAPR, The National Science Foundation, NASA, and volunteers like you. Per long standing tradition, HamSCI will be hosting booth  5008 (next to TAPR in Building 5, the Hertz Building, map below), hosting the HamSCI Forum and giving booth talks in the ARISS/YOTA area (map below). To help out, please sign up to volunteer at the booth.

Booth Volunteering

Volunteer Sign-Up

Lab Coats

HamSCI labcoats may be ordered from https://www.allheart.com/lab-coats. Please use custom logo code C_5163_Q5D and place the logo on the left chest. Put your whole name on Line 1, and your call sign on Line 2. Use block style lettering.

Recommended Styles for 2023

Note that allheart.com changes their available styles on a regular basis. The important thing is to pick a white lab coat that fits you and put the custom logo code C_5163_Q5D and place the logo on the left chest.

• https://www.allheart.com/allheart/basics-by-allheart/unisex/unisex-41-ipad-pocket-lab-coat/ah8004.html
• https://www.allheart.com/meta-labwear/meta-labwear/unisex/unisex-colored-40-lab-coat/6116.html

Sample Order - Information confirmed March, 2023

Natural Uniforms Unisex 41" Lab Coat
Item #: AH-8200---WHTLGE
Color: WHT White
Size: LGE
Personalization - Left Chest
  Embroidery Style: Block Style
  Thread Color: Black
  Letter Height: 1/2 inch (25 characters)
  Text Line #1: Dr. Nathaniel A. Frissell
  Custom Emblem: C_5163_Q5D
  Text Line #2: W2NAF

Exhibitor Badges

If you are volunteering at the booth or giving a talk, HamSCI will supply an exhibitor badge. These badges give you full access to the Hamvention, including the set-up and break-down times. However, these badges will not enter you in the prize drawings the way a normal Hamvention ticket will. Please coordinate requests for exhibitor badges with Gary Mikitin AF8A via [email protected].  

Group Photo - Please note the date/time change

A HamSCI group photo will be taken during the Hamvention on Saturday at 9:30 AM (1330 UTC) at the HamSCI booth. Wear your labcoats!

HamSCI Presentations, Talks and Demonstrations

Members of HamSCI will be presenting at many events throughout the Hamvention weekend, beginning Thursday evening.  Some talks will be at offsite events, while others will be held on the Hamvention grounds.  A complete list of talks, presenters and dates/times can be found on the HamSCI Hamvention 2023 page.

Questions?

If you have questions about HamSCI's 2023 Hamvention plans, please contact the HamSCI Team at [email protected].

Booth Location

HamSCI will be at Booth 5008, next to TAPR, in Building 5, the Hertz Building.

How to Check and Update Your KiwiSDR Firmware:

Do an admin login and go to the status tab - it lists the installed FW version.


The Update tab allows you to update and build the latest version.

Main workshop page: http://hamsci.org/hamsci2023
HamSCI Glossary

Friday, March 17, 2023

Saturday, March 18, 2023

Sunday, March 19, 2023

Presentation Files

Welcome amateur radio contesters, beacon enthusiasts and citizen scientists.  This is the Contest Information Page for the 2023 and 2024 HamSCI Solar Eclipse QSO Parties and the Gladstone Signal Spotting Challenges.  This page has links which will quickly take you to the FAQ pages, rules and the optional pre-registration form for both events.  They are part of the HamSCI Festivals of Eclipse Ionospheric Science.

Contest results from the 2023 and 2024 FoEIS events (GSSC, SEQP) have been tabulated and published: FoEIS Results

Solar Eclipse QSO Party (SEQP) (Next event:  April 8, 2024)

The SEQP is a typical ham radio contest for those who wish to makes tens, hundreds or even thousands of CW, SSB and digital mode QSOs on 160-6 meters during the 2023 and 2024 American solar eclipses.  Each QSO will become one of millions of data points which will help researchers answer science questions about ionospheric variability.

SEQP FAQs

SEQP Rules

Gladstone Signal Spotting Challenge (GSSC) (Next event:  April 8, 2024)

The GSSC is a unique event for those who enjoy operating beacons (CW and digital), and the 'propagation study modes' of WSPR and FST4W, both transmit and receive.  Signals generated and received during the GSSC will help researchers answer science questions about ionospheric variability. 

GSSC FAQs

GSSC Rules

HamSCI Festivals of Eclipse Ionospheric Science (FoEIS)

The SEQP and GSSC are part of the HamSCI Festivals of Eclipse Ionospheric Science.  Members of HamSCI, the Ham Radio Science Citizen Investigation, along with the ham radio community, will be creating data for researchers by transmitting, receiving and recording signals across the HF spectrum.  Upon analysis, the data should inform researchers how the ionosphere reacted to the eclipse.  The data will be compared to existing computer models of the ionosphere, potentially improving the accuracy of those models.  Researchers will also be looking at how the ionosphere’s refractive properties varied during the beginning and ending phases of the eclipses. Further details on the scientific basis of the FoEIS will be published here soon.  

In the meantime, you may wish to view the contest and science results from the 2017 SEQP.

Optional Pre-Registration Form

We are asking participants to voluntarily pre-register with their names, callsigns, and locations to ensure we have good participation from stations near or under the eclipse path.  While all signals will have scientific value, those passing under the solar eclipse path (https://www.greatamericaneclipse.com/) will be of particular interest.  If we miss the chance to collect meaningful data in 2023 and 2024, it will be decades before North American hams and researchers get another opportunity!

Back to Pre-Registration Form information
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The Gladstone Signal Spotting Challenge is named for Philip Gladstone, N1DQ, the creator and maintainer of the PSKReporter.info website, also known as the Digimode Automatic Propagation Reporter.  Philip has made a tremendous contribution to Amateur Radio operating, citizen-science and ionospheric research through the data ('spots') which are collected and stored on PSKReporter.info.  This Wikipedia entry tells the story:  https://en.wikipedia.org/wiki/PSK_Reporter

The contest results for the 2023 and 2024 GSSC events have been tabulated and published:     GSSC 2023 Results       GSSC 2024 Results

The following is an introduction to the GSSC.  Please visit the full GSSC Rules for detailed explanations of station requirements, and the post-event entry event and scoring process.  These FAQs are a brief, informal recap of the actual GSSC rules.  In case of conflicts or questions, the GSSC Rules should be considered the definitive resource.  The GSSC is but one event within the Festivals of Eclipse Ionospheric Science.

What is the Gladstone Signal Spotting Challenge?

The Gladstone Signal Spotting Challenge is planned to be a fun, friendly competition with a serious purpose.  Amateur radio operators (hams) and short wave listeners will be operating beacons and setting up receiving sites using WSPR, FST4W, PSK31 and Morse Code (CW).  (These activities are commonly referred to as 'spot generation', 'spot collection' and the resulting data, 'spots'.)  The spots generated and collected by GSSC participants will be used in scientific studies exploring the Earthly ionosphere’s reaction to the 2023 and 2024 solar eclipses passing over North America.  The studies should lead to a better understanding of the interactions between the Sun, the ionosphere, and radio wave propagation.  That research should benefit hams, professional broadcasters, satellite operators, and many other users of the radio spectrum.  

When will the GSSC occur? (Download and open the ICS file below to add the event to your electronic calendar)

• April 8, 2024; 1400-2400 UTC; is the official 2024 GSSC event period.
• The GSSC will start a few hours before the eclipse begins its transit across the US mainland, so baseline data can be gathered (it is important to know how well the ionosphere is refracting high frequency (HF) signals prior to the eclipse)
• It will continue through the entire eclipse period, in order to study how high frequency (HF) propagation is affected by the eclipse (past experience suggests that ionospheric changes will be clearly visible in the data).
• It will conclude a few hours after the eclipse transits beyond the US mainland, in order to observe and study the after effects of the eclipse, such as ionospheric recovery.

You do not have to operate the full GSSC period, though that would be most welcome.  If you only have an hour or two, try to schedule your operating when the eclipse path is nearest to your QTH.  That will raise the odds that your signals will be affected by the eclipse.   Eclipse paths can be seen at https://www.greatamericaneclipse.com/.

GSSC 2024.ics

Geographically speaking, who should participate?

HF radio signals are rarely restricted to small geographic areas, so we welcome hams and radio enthusiasts from all over the world to set up WSPR and FST4W equipment (both transmitting and receiving) and also PSK31 and CW receivers (often called 'skimmers').   

What equipment is required?

Transmitting stations have many options (only a few are listed here, HamSCI is not recommending any specific method or vendor):

• Standard HF transceivers with audio/computer interfaces and appropriate software (such as WSJT-X)
• WSPR-only transmitters (https://www.zachtek.com/
• Raspberry Pi based gear (https://tapr.org/)
• Build-it yourself kits (https://qrp-labs.com/)

Receiving setups have many options (All require appropriate software, depending on the mode being received, e.g. WSJT-X, WSPRdaemon, fldigi, CW Skimmer)

• Standard HF transceivers with audio/computer interfaces
• Most off the shelf software defined radios (SDRs)
• Build-it yourself kits  (https://qrp-labs.com/)

Simple antennas, being minimally directive, are often best for these modes.  Verticals, dipoles, loops, installed indoors or out, will work well.  But - if all you have is a set of stacked beams hundreds of feet in the air - that's fine.  Please be sure to note your antenna system details in your post-event GSSC entry.

For receiving stations, a reliable Internet connection is highly desirable.  All spot collection software should be configured to forward the spot data, in real time, to one of the on-line aggregation sites, such as wsprnet.org or PSKReporter.info.  This relieves individual receiving stations from needing hardware and procedures to store and deliver the to spots to HamSCI researchers after the GSSC.

Where can I learn more about modes such as WSPR and FST4W?

The WSPR protocol is more than a decade old, yet is still widely used for propagation monitoring.  There are many web resources explaining WSPR and how to set up a WSPR station, perhaps the best place to start is at the WSJT-X software home page.  There are many YouTube sites to explore, one suggestion is linked here <https://www.youtube.com/watch?v=KYlaLT5HLkM>

WSJT-X contains a much newer protocol with exciting capabilities, FST4W.  The WSPR Daemon site http://wsprdaemon.org/presentations.html has many details on that mode.

The HamSCI site has a list of publications  https://hamsci.org/publications on propagation research, including the use of WSPR data.

The GSSC looks like fun, but I also want to participate in the Solar Eclipse QSO Party.

Feel free to enter both events!  For example, you may wish to operate WSPR or FST4W transmitters on one or more one of the WARC bands while you operate in the SEQP.  FT4/8 operators:  The 2024 GSSC scoring will not include FT4 or FT8 receptions or transmissions.  Operators who enjoy those modes are encouraged to enter the Solar Eclipse QSO Party (SEQP).

Further suggestions?

Whether you are new or an expert in the areas of spot generation or spot collection, there's no need to wait for the GSSC to put your station to use.  Explore your options, assemble and operate your equipment as soon as you are ready.  You'll work the bugs out of your system well before the eclipse events.  Even better, you'll contribute valuable spot information to the on-line databases as Solar Cycle 25 ramps up.  You can follow our Sun's activity at https://spaceweather.com/ and https://www.solarham.net/ .

The following is an informal introduction to the SEQP.  Please visit the full SEQP Rules for detailed explanations of all terms, links to useful sites, and just about everything needed to prepare for and operate in the SEQP.  The rules also contain details on after-contest scoring and log submission.  These FAQs are a brief, informal recap of the actual SEQP rules.  In case of any conflicts or questions, the SEQP rules should be considered the definitive resource.  The SEQP is but one event within the Festivals of Eclipse Ionospheric Science.

What is a Solar Eclipse QSO Party, and why is it being held?

The Solar Eclipse QSO Party is an opportunity for amateur radio operators (hams) to operate during the October, 2023 and April, 2024 eclipses, before, during and after they pass over North America.  Using various modes (CW, voice, and digital), two-way transmissions (QSOs) made during the SEQP will contribute to scientific studies focusing on the ionosphere’s reaction to the eclipse.  The studies should lead to a better understanding of the interactions between the Sun, the ionosphere, and radio wave propagation.  That research should benefit hams, professional broadcasters, satellite operators and many other users of radio spectrum.  

Results from the 2023 SEQP are available here 

Results from the 2024 SEQP are available here

When will the SEQP occur? (Download and open the ICS files below to add the events to your electronic calendar)

• October 14, 2023; 1200-2200 UTC; is the official 2023 SEQP event period.
• April 8, 2024; 1400-2400 UTC; is the official 2024 SEQP event period.
• The SEQPs both starts a few hours before the eclipses begins their transit across the US mainland, so baseline data can be gathered (it is important to know how well the ionosphere is reflecting and refracting high frequency (HF) signals prior to the eclipses)
• They continue through the entire eclipse period, in order to study how HF propagation is affected by the eclipse (past experience suggests that ionospheric changes will be visible in the data).
• They conclude a few hours after the eclipses transit beyond the US mainland, in order to observe and study the after effects of the eclipse (such as ionospheric recovery, if any).

You do not have to operate the full SEQP hour period, though that would be most welcome.  If you only have an hour or two, try to schedule your operating when the eclipse path is nearest to your QTH.  That will raise the odds that your signals will be affected by the eclipse.  Eclipse paths can be seen at https://www.greatamericaneclipse.com/.

GSSC 2023.ics

2024 SEQP.ics

Who should participate?

The 2023 and 2024 eclipses will be passing over the continental United States, so researchers are most interested in having hams in North America participate.  Of course, HF radio signals don’t generally restrict themselves to small geographic areas, so hams from all over the world are welcome to operate and enter the SEQP.

What equipment is required?

Almost any ham station can participate.  An HF radio and antenna(s), usable on one or more of the 160, 80, 40, 20, 15 10 and 6 meter bands.  

It is extremely helpful to have contest logging software on a computer in your station.  The software guides you through the QSO making process, and it records all of the QSO data needed to submit your results after the SEQP.  It is those results which scientists will gather, from you and thousands of other participants, to aid in their research.

What can I expect if I get on the air during the SEQP?

The SEQP, while technically an 'operating event', closely mirrors fits the definition of a ‘contest’.  It is a friendly competition where participants endeavor to make many contacts in a short period of time, over the widest possible area.  QSOs will be short, with specific information (callsigns, signal reports, stations locations) exchanged between stations.  If it is your first contest, the first few minutes can be a bit overwhelming, but listen in, learn the operating rhythm, and jump in!

The SEQP encourages operation on CW, SSB and all digital modes.  The basic idea is to have as many hams as possible make as many QSOs as possible, then collect their QSO data, carefully studying it for trends indicating how far, how strong and where HF signals propagated vs. the path of the eclipses. 

Is there a 'fun factor' to the SEQP?

Yes, absolutely!  Operating events are supposed to be ‘fun’.  One way to increase the fun factor of any contest is to calculate a score for all participates, based on the number of contacts made, their geographic reach, and how many receiving stations heard their signals.  The HamSCI Data Processing Team will gather all of the entries submitted on the SEQP website, visit propagation databases such as WSPRNET.org and PSKReporter.info, and assemble millions of data points into a research database.  From that database the HamSCI Data Processing Team will be able to assign everyone a score, which will then be published some months after the SEQP.

What if I am not interested in two-way QSOs, but I am a WSPR or FST4W enthusiast?

There is a solar eclipse event for those who are interested in transmitting and receiving WSPR and FST4W signals: The Gladstone Signal Spotting Challenge

Ideally, many WSPR and FST4W transmitters will be on the air for the entire SEQP, their transmissions logged by receivers worldwide (or as far as propagation allows), enabling researchers to search out propagation effects of the solar eclipses as they move across our planet. 

Version 1.25 (added 2024 Google entry form)

8 Apr 2024

The Gladstone Signal Spotting Challenge is named for Philip Gladstone, N1DQ, the creator and maintainer of the PSKReporter.info website, also known as the Digimode Automatic Propagation Reporter.  Philip has made a tremendous contribution to Amateur Radio operating, citizen-science and ionospheric research through the data ('spots') which are collected and stored on PSKReporter.info.  This Wikipedia entry tells the story:  https://en.wikipedia.org/wiki/PSK_Reporter

The first contest results for the GSSC have been tabulated and published:  GSSC 2023 Results

FT4/8 operators:  The 2024 GSSC scoring will not include FT4 or FT8 receptions or transmissions.  Operators who enjoy those modes are encouraged to enter the Solar Eclipse QSO Party (SEQP).

The following are the complete, detailed rules for the GSSC.  For a quick introduction to the GSSC, please visit the GSSC FAQ page.  The GSSC is one event within the HamSCI Festivals of Eclipse Ionospheric Science.

I) Dates and Times

14 Oct 2023 1200 – 2200 UTC (Partial eclipse began ~1500 UTC in Oregon ended ~1840 UTC in Texas) Event complete - Results available

8 Apr 2024 1400-2400 UTC (Partial eclipse begins ~1710 UTC in Texas and ends ~2040 UTC in Maine)

Participants are encouraged to operate before, during and after the eclipse passes over the continental US.  Doing so will create baseline data (pre- and post-eclipse), and eclipse influenced data (during annullarity or totality) for the research team.

II) Objective

To generate observations of propagation by  WSPRNet, PSKReporter and the Reverse Beacon Network, along with participants' event logs before, during, and after the eclipse on the amateur bands for the purpose of ionospheric sounding.  

III) Station Requirements - Receiving WSPR, FST4W, PSK or CW 

Reception reports for all of these modes will be useful to the scientific community in their propagation research efforts.

1. Bands of interest are 160, 80, 40, 30, 20, 17, 15, 12, 10, and 6 meters, reception of CW and all digital modes included.
2. A typical entrant will operate one CW Skimmer or PSK or WSPR or FST4W receiving node in a particular grid square.  
3. Entrants may operate multiple nodes in a given grid square, each on different band/mode combinations (e.g., 40m WSPR & 20m WSPR & 15m WSPR all in grid EN91gm).​
4. An entrant may choose to set up nodes in multiple grid squares.  If setting up multiple receiving nodes on a specific band/mode combination, those nodes must be separated by at least 100km in order to be useful to the science community (e.g., you may operate a 20m CW Skimmer site in grid EN91gn and another 20m CW skimmer site in grid EN90ha). 
5. Be sure the receive node data is properly configured (especially Reporter, 6-character Reporter Grid) when sending reports to the RBN/PSK/WSPR/FST4W reception report aggregation sites and in your event log.
6. WSPR nodes should monitor standard WSPR which uses 2 minute cycles (also known as 'WSPR-2' on wpsrnet.org).
7. Please register your node(s) and configure them for automatic uploads to the appropriate network: Reverse Beacon Network (RBN – http://www.reversebeacon.net/), PSKReporter (https://pskreporter.info/), WSPRNet (http://www.wsprnet.org).  This is the most effective way to pass GSSC reception information on to the HamSCI Data Processing team, and also, the best way to earn points and recognition for your efforts.
8. ​If you cannot register your receiving node(s) as suggested above, contact the GSSC Committee via the HamSCI mailing list prior to the event so we can discuss alternate arrangements for collecting your data.
9. Ionospheric science is advancing at a rapid rate.  New modes, such as FST4W-120, are gaining popularity and recognition for their ability to provide additional opportunities for research.  If you have access to a Kiwi software defined radio (SDR) and you can run WsprDaemon software, please consider setting the configuration for receiving FST4W-120 signals on the HF bands.   A bonus multiplier will be awarded for reception of FST4W-120 signals - see Bonus Multipliers below.
10. There are no provisions for mobile or rover operations.  Receivers should remain fixed in one location for the duration of the GSSC.

IV) Station Requirements - Transmitting WSPR, FST4W

WSPR transmissions are a well established method for generating propagation related data, useful to the science community.

1. WSPR and FST4W transmissions are encouraged on 160, 80, 40, 30, 20, 17, 15, 12, 10, and 6 meters. Operation on multiple bands is encouraged - the more data generated, the better.  Transmissions of FST4W-120 are also encouraged on these bands. A bonus multiplier will be awarded for transmitting FST4W-120 signals - see Bonus Multipliers below.
2. ​Use standard, legal WSPR and FST4W frequencies with a callsign which does not​ include a forward slash ( / ).
3. Whenever possible, configure your WSPR transmitter as follows:  Transmit (Tx) frequency to be either above or below 1500Hz, Type 1 messages, transmit percentage (Tx %) to 100%, 2 minute WSPR cycles.​ (While usual WSPR etiquette is not to transmit at 100%,  the GSSC is a time-limited event, designed for observing transient phenomena of scientific interest, thus 'the more, the better'.). The GSSC will be most successful if participants choose random frequencies.  One method for picking a random frequency is to visit a random number generator site for frequency selection.
4. Most users will want to transmit WSPR and/or FST4W using the latest stable release of WSJT-X, see K1JT's WSJT-X Page).  Stand-alone WSPR gear (such as hardware from Zach Tech, TAPR and others) will work as well.
5. WSPR reception reports will be automatically logged on WSPRNet (wsprnet.org).  The HamSCI Data Processing Team will download relevant WSPRNet data after the contest, so it is not necessary to submit reception reports from WSPRNet.org or any other WSPR aggregator to prove that your WSPR transmitter was 'on the air'.

V) Post-Event Entry Process

At the conclusion of the GSSC event, use the Google form at the bottom of this web page  to enter callsign/identifier, contact information, bonus point requests and comments.  

The HamSCI Research Team greatly appreciates all who contribute to the Gladstone Signal Spotting Challenge.  The Team would like to recognize all participants via postings on the HamSCI website and in other media.  ​Further, we may have questions for the participants as we work through the data analysis process.   Note: We will not share contact information with anyone outside the HamSCI Data Processing and Research teams.   We highly encourage all​ GSSC participants to complete the post-event entry process and receive a score and ranking once the results are tabulated.

Note:  if you choose to upload files to Zenodo (see Bonus Point Multipliers, below) do that first, note your DOI (Digital Object Identifier) and include that in the Comments section of the post-event Google form.

VI) Scoring and Post-Event Recognition

Scoring each participant's contribution in a highly technical and widely diverse event such as the GSSC is a challenge for the party organizers.  The HamSCI team has decided to list the relevant details about each submission, in the format shown below, as a way to recognize and thank those who contributed to the GSSC, and, ultimately, to the Festivals of Eclipse Ionospheric Science.

1. GSSC entries for transmit sites will be reported by three attributes:  Call, Reporter Grid, Frequency Band
   1. 'Call' must be be an amateur radio callsign (e.g. WR8ABC)
   2. 'Grid' must be the 6-character grid square where the transmitter is located
   3. 'Frequency Band' will be one of 160m, 80m, 40m, etc.​​

1. GSSC entries for receive sites will be reported by three attributes:  Reporter, Reporter Grid, Frequency Band
   1. ​'Reporter' may be be an amateur radio callsign (e.g. WR8ABC) or another textual identifier (e.g. OHSWLEN91)
   2. 'Reporter Grid' must be the 6-character grid square where the receiver is located
   3. 'Frequency Band' will be one of 160m, 80m, 40m, etc.

Some months after the event, after the HamSCI Data Processing Team has concluded their work, a chart, similar to that shown here, will be published to the HamSCI website. 

 

 

 

XI) Bonus Multipliers

All bonus multipliers will be verified by the HamSCI Data Processing Team, after the Gladstone Signal Spotting Challenge, as part of the final score calculation process.

1. Upload PDF file(s) of antenna and station design characteristics (1.10 multiplier). 
   1. Antennas: Type, location, orientation, E and H plane patterns, height above ground
   2. Station:  Block diagram, including equipment information (manufacturer/model, transmitter power), software names and version numbers
2. ​Photograph(s) of station equipment and/or of the operating site (1.05 multiplier for the first photograph, more photos will not result in more multipliers)
3. Receiving or transmitting FST4W-120 signals (1.25 multiplier specifically for FST4W-120 reports )
4. Email the above files to [email protected]
5. Upload any other files you believe would be useful to research for purposes to the public HamSCI zenodo.org community. You will be provided a DOI (digital object identifier) which you can then include on your post-event GSSC Google form to associate your GSSC entry with your bonus files.
6. Bonus multipliers should be claimed on the GSSC post-event report form. 

Zenodo files will be uploaded under Zenodo's 'open access' policy.  Data files and entry forms will likely be transferred to Zenodo in the future - under the same 'open access' policy.

Station design characteristics and photographs may be used by the HamSCI Research Team to further their understanding of how and why signals propagated across the US before, during and after the eclipse.

 

2024 GSSC Google Entry Form

 

Data from the 2023 MW Recordings Event are available on Zenodo.  The complete story is here:  2023 MW Recordings

Contest results from the 2023 and 2024 FoEIS events (GSSC, SEQP) have been tabulated and published: FoEIS Results

The HamSCI Festivals of Eclipse Ionospheric Science will occur October 14, 2023 and April 8, 2024 during spectacular North American solar eclipses.

​The Festivals will consist of multiple events, each with a goal of increasing our understanding of sun-ionosphere-earth relationships.

​Participants will include volunteer amateur radio operators, short wave listeners and science researchers from multiple US universities.

♦ HamSCI FoEIS Contests (Non-WARC Bands, 6-160 meters)

• The Solar Eclipse QSO Party (SEQP) using CW, FT4/8, SSB and other digital modes
• The Gladstone Signal Spotting Challenge (GSSC) using CW, WSPR and FST4W modes
• The HamSCI FoEIS Contest Info Page has all of the details

♦ Additional Events Taking Place Across the Radio Spectrum

• Medium Wave (MW) Recordings Event - Making IQ recordings (using software defined radios) of medium wave broadcast stations for future studies of eclipse-influenced ionospheric dynamics

• ​VLF Reception Exercise (Definition in progress - please check back at a later date)

• 2017 Eclipse HamSCI Home Page
• 2017 Solar Eclipse QSOParty (SEQP) Results
• 2017 SEQP Data Archive
• National Contest Journal NCJ Solar-Eclipse Wrap-Up
• Geophysical Research Letters Peer-Reviewed Science Article

​Participating Universities

• The University of Scranton (W3USR) (Lead Institution)
• Case WesternReserve University (W8EDU)
• New Jersey Institute of Technology (K2MFF)
• The University of Alabama
• Dartmouth College
• Montclair State University
• Rice University (W5YG)

Media Hits

Version 1.07 (removed mention of PA, NV, AZ, SD QSO Parties from Section X)

3 Dec 2022 / 25 Jul 2023 / 26 Sep 2023 / 6 Oct 2023 / 14 Oct 2023 / 27 Feb 2024 / 5 Apr 2024

The following are the complete, detailed rules for the SEQP.  For a quick introduction to the SEQP, please visit the SEQP FAQ page.  The SEQP is one event within the Festivals of Eclipse Ionospheric Science.

Log submission links are in Section X, below.

Both N1MM+ and N3FJP logging programs officially support the SEQP.

I) Dates and Times

8 Apr 2024 1400-2400 UTC (Partial eclipse begins ~1710 UTC in Texas and ends ~2040 UTC in Maine)

Participants are encouraged to operate before, during and after the eclipse passes over the continental US.  Doing so will create baseline data (pre- and post-eclipse), and eclipse influenced data (during annullarity or totality) for the research team.

II) Objective

To generate observations of propagation by the Reverse Beacon Network and PSKReporter event logs before, during, and after the eclipse on the amateur bands for the purpose of ionospheric sounding.

The Solar Eclipse QSO Party (SEQP) is unique among ham radio competitions as it awards points for two-way QSOs (ham to ham contacts via radio) and bonus points for reception reports from skimmers, RBN nodes and the like.  

Please be aware that the SEQP is one of many events to be held during the HamSCI Festivals of Eclipse Ionospheric Science.  You are welcome to participate in more than one event.  Each event has its own 'rules' page, accessible from the 'Festival' link above.

III) Station Requirements

1. All transmitting and receiving equipment used to make two-way QSOs must be located within a 500-meter diameter circle.
2. Remote operation is permitted for two-way QSOs if the physical location of the remote stations meets the 500-meter diameter circle rule above, all station and operator licensing requirements are met for the remote location, and all category limitations in these rules are met.
3. Portable operation, from a fixed location (such as POTA, SOTA, Field Day style setups, operated by individuals or groups) are welcome and encouraged (see bonus points below).
4. There are no provisions for mobile or rover operations.  Transmitters and receivers should be fixed in one location for the duration of the SEQP.

IV) Categories (to be listed separately in the results)

1. Single-operator (only one transmitted signal, emitted for the purpose of making two-way QSOs, is permitted at any time)
2. Multi-operator (one or more transmitters) (only one transmitted signal per band and mode, emitted for the purpose of making two-way QSOs, is permitted at any time)
3. Checklog  Checklogs will not be scored, but submissions will be eligible for an SEQP Participation Certificate.  
4. ​There are no restrictions on transmitter power (please be reasonable, don't run a kilowatt on FT8!), spotting assistance, or band changes.
5. There are no band specific or mode specific categories.  All entries will default to 'Mixed Mode' and 'All Bands'.

V) Bands, Frequencies and Modes for Two-Way QSOs

160, 80, 40, 20, 15, 10, and 6 meter bands, using these modes: CW, SSB, digital (all varieties)

Reminder:  By international agreements, the 60, 30, 17, and 12 meter bands may not be used for two-way contest QSOs.

We anticipate plenty of activity. On CW and SSB, tune for stations calling 'CQ SEQP' near 'the 38s' (just a starting point - use any legal frequency) (CW +/-10kHz from 3538, 7038, 14038, etc.  SSB +/-25kHz 3838, 7238, 14328, 21338, 28338).  Activity on digital modes will be close to the usual activity centers but - please - spread out!  With many stations active, assist the receiving decoder stations to make quick and accurate measurements by leaving some space between signals.  You can find band planning information at 

• http://www.arrl.org/band-plan
• https://sumterdigitalgroup.com/digital-modes/frequencies/
• http://wsprnet.org/drupal/node/218

VI) Exchange for Two-Way QSOs

Accurate Signal Report, 4-Character Grid Square.

Example Exchange: 

• W1AW:  CQ CQ SEQP de W1AW W1AW
• N0AX:   N0AX
• W1AW: N0AX 579 FN31
• N0AX:  589 EM48
• Optional:  Either station's callsign may be inserted at any time during an SEQP QSO.  Use your judgment to balance efficiency (short QSOs) against accuracy (knowing for sure who you worked).
• If you miss any of the information, simply ask for a repeat (on SSB), or send AGN? (on CW).  Be sure to log what you receive.

Notes

1. On CW, call “CQ CQ TEST DE [your call] [your call] K” using a single code speed during the transmission.  Repetition of CQ and/or TEST as shown, as well as repetition of your callsign, maximizes the ability of the automated receivers to decode and spot your transmission. Please see Getting Spotted by the RBN for tips on getting spotted while calling CQ during the SEQP.
2.  To determine your grid square, visit this Amateur Radio Grid Square Locator Tool.
3. Signal Report
   • CW/Phone: The strength (S) value of RS(T) signal reports should represent the approximate peak S meter reading.  (Readings greater than S9 should be sent as S9.)
   • Digital: The preferred digital signal report is the SNR in dB as provided by the digital mode software. Alternatively, give the operator-determined RSQ (Readability - Strength - Quality) value. Note that N1MM+'s FT8 integration should automatically place SNR values into the Snt and Rcv signal report entry boxes, though you can do so manually if desired. (Researchers will assume any CW or digital signal report not in three-digit RST/RSQ format is an SNR [dB] value.)

VII) Transmitting Digital Modes

1. Many software authors publish guides to using their programs with FT8.  

   • Contesting software, such as  N1MM+ , interfaced with WSJT, is the best solution for operating FT8 in the SEQP, in part because it generates Cabrillo files.

   • Desktop logging packages, such as Ham Radio Deluxe, also work well with FT8 and other digital modes.  However, it will take a few extra steps to generate a log for uploading to the SEQP Scoring Robot.  (You will need to selectively export your SEQP QSOs as ADIF for the date and time you were operating in the SEQP.)
2. PSK Reporter Spotting:  Many digital mode packages such as the open-source fldigi program and Ham Radio Deluxe/Digital Master 780 have options for automatically sending spots to PSKReporter.  Please enable this option to send additional data to PSKReporter.
3. Operate normally, call CQ, answer CQs - same as you would when not involved in a contest or QSO party.
4. Make sure your software is configured with your station location in the 4-character grid square format. This is especially important if you are operating portably.  See the Amateur Radio Grid Square Locator Tool.
5. When using WSJT, it is important to do two things:
   1. ​Enable PSKReporter in the Reporting tab.  This will send received signal data to the PSKReporter website, where it will be saved for later retrieval by the HamSCI data analysts.
   2. Enter an antenna description on the Frequency tab.  This field must have some information, even something simple, like 'dipole' or 'mag loop', in order for PSKReporter to accept received signal data.
6. Use an Internet connection for time sync and spotting if possible. Smart phone hotspots and public WIFI may provide Internet in portable locations.
7. Use CAT radio control if possible, to accurately record QSO frequencies.
8. In your Cabrillo soapbox, please note the type and version number of software used e.g. WSJT-X 2.5.4 or fldigi 4.1.23
9. ​Optionally sign SEQP to attract other participating operators (e.g., "KV4PC SEQP 73").​

VIII) Scoring

Score = (QSO Points x Multipliers) + Bonus Points

1. QSO Points: CW and Digital QSOs, 2 points each; SSB QSOs, 1 point each
2. Multipliers: 4-character grid squares, counted once per band.
3. The same station may be worked for QSO points on all SEQP bands and modes (e.g. N4BB contacts KD8GMH three times, on 40m CW, 20m SSB and 10m FT8).
4. Duplicate contacts (second, third, fourth, etc. QSOs with a station previously worked on a given band and mode) are allowed after 10 minutes have elapsed since the previous QSO with that station (ie K8MAD may contact N4FCG for QSO points on 40m CW at 2130z, 2152z, and again at 2215z). Note: N1MM+ logging software will correctly accept and score duplicate QSOs as follows:
   1. If you work a station that is truly a duplicate (same callsign, band, mode) within 10 minutes, N1MM+ will warn you with a red DUPLICATE message and refuse to log the QSO.
   2. If you work a 'legal duplicate' per Rule #4, N1MM+ will warn you with a red DUPLICATE message but it WILL allow you to log the QSO.
5. Bonus points earned (see Bonus Points section)

The final score, including bonus points, will be calculated by the HamSCI Data Processing Team.  Claimed Scores are not required to be accurate.

 IX) Bonus Points

Zenodo files will be uploaded under Zenodo's 'open access' policy.  Logs and entry forms will likely be transferred to Zenodo in the future - under the same 'open access' policy.

XI) Logging Requirements

Logs should be in the Cabrillo format (http://www.arrl.net/cabrillo-format-tutorial).  All modern logging programs are capable of generating a Cabrillo format log.  Required fields:

Frequency, Mode, Date, Time (UTC, not local), Sent Call, Sent Signal Report, Sent Grid, Received Call, Received Signal Report, Received Grid

Example QSOs (or click here for full example log):

QSO:  7030 CW 2017-07-20 2241 K2MFF             579  FN20 N3AO              599  EM97 
QSO:  1816 PH 2017-07-20 2243 K2MFF             59   FN20 KC2LRC            59   FN13 
QSO:  3590 RY 2017-07-20 2249 K2MFF             599  FN20 W1AW              599  FN31 
QSO: 14070 PK 2017-07-20 2305 K2MFF             30   FN20 AD0AE             24   CM97 

• Use the following mode codes should appear in the log.  N1MM+ should automatically generate logs with the correct codes.

• Include station power level, 6-character grid square, antenna type, equipment list, and extra comments in the Cabrillo file soapbox. Please use the example below to allow easy and accurate post-event processing. Note that although 4-character grid squares are used in the contest exchange, we ask for 6-character grids in the soapbox and log header.

Example soapbox:

SOAPBOX: power=100 W, grid=FN20vt, antenna=dipole, equipment=IC7410
SOAPBOX: comments=Totality was beautiful!

• Use any software that supports the Solar Eclipse QSO Party. The N1MM+ contest logger natively supports the SEQP as log type "ECLIPSE". 
• News Flash:  N3FJP Logger now supports the SEQP:  N3FJP VHF Contest Log 6.6.8 - updated to also support the Solar Eclipse QSO Party.  While the SEQP includes HF, the existing grid exchange in the VHF software was the best fit for SEQP's inclusion.  Just click Settings > Setup and select Solar Eclipse QSO Party. 
• Any logging software that supports the ARRL VHF contest exchange format (signal report and grid square) can also be used, though you will have to edit your Cabrillo file, changing the contest name to ECLIPSE-QSO

Figure: "New Log in Database" dialog box from the N1MM+ contest logging program. Select log type "ECLIPSE", choose "SINGLE-OP" or "MULTI-OP", put your four-character grid square in the Sent Exchange box, and include station data in the soapbox.  Be sure the 'Mode' selection is set to SSB+CW+Digital if you plan to operate any digital modes.

​

• HamSCI workshop presentations and discussions are expected be consistent with the bullet points stated in the section below entitled “HamSCI and the Scientific Method.”
• All HamSCI activity is expected to be conducted in a respectful and considerate manner. Discussions should never consist of personal attacks or crude language.
• Members are expected to act in an ethical manner, which excludes the practices of plagiarizing, misusing, misrepresenting, or stealing data or ideas.
• Presentations and discussions are expected to be of direct interest to the HamSCI community.
• Commercial endorsements, unrelated / inappropriate event advertisements, or other similar material should not be presented.

HamSCI Use of the Scientific Method

• The scientific method is a core strategy for HamSCI activities.  This implies that research findings, especially those containing potentially unusual or novel results, should first undergo the rigors of this technique before widespread community acceptance.  Discussions may therefore potentially include direct questions and suggestions from the professional research community, along with reference comparisons to previously published material in the open refereed scientific literature.  
• HamSCI workshop participants should always be willing to engage in scientific discussions in a spirit of open curiosity and knowledge advancement.  We emphasize that such interactions may include questions on findings, and these are not a sign of disrespect but, rather, of community interest in particular observations or implications.  The scientific method’s practices are a time-tested and vital method for producing a robust finding and avoiding incorrect conclusions based on misleading or potentially biased/flawed results.
• Questions may also be posed about specific methodologies and equipment characteristics, and these are equally important to the HamSCI method and should be treated with an equally open spirit.  Investigations in this area may require follow-up data collection or coordinated measurement activities in partnership with the collective.
• Members who violate the guidelines above may have their HamSCI participation privileges revoked at the discretion of the HamSCI Workshop Science/Program Committee.

Non-Discrimination, Anti-Harassment, Sexual Harassment, and Sexual Misconduct Policies

All participants of the 2023 HamSCI Workshop, which is hosted by The University of Scranton, are expected to treat each other with respect and follow The University of Scranton's current Non-Discrimination and Anti-Harassment Policy and Sexual Harassment and Sexual Misconduct Policy that are available from the University’s Office of Equity and Diversity website (https://www.scranton.edu/equity-diversity/). Participants who wish to report a violation of these policies may contact the HamSCI Workshop Science/Program Committee Chair, Dr. Nathaniel Frissell at [email protected]. Dr. Frissell is a full-time employee of The University of Scranton who will report the complaint to the University’s Title IX Coordinator and Office of Equity and Diversity. Alternatively, the University’s Title IX/Equity and Diversity Coordinator, Elizabeth Garcia, Esq., may be contacted directly at [email protected] or (570) 941-6645.

March 17-18, 2023
A Hybrid In-Person and Virtual Workshop

Come join HamSCI at its sixth annual workshop March 17-18, 2023 at The University of Scranton. The primary objective of the HamSCI workshop is to bring together the amateur radio community and professional scientists. The theme of the 2023 HamSCI Workshop is Forging Amateur-Professional Bonds.

This workshop will also serve as a team meeting for the HamSCI Personal Space Weather Station project, a NSF-funded project to develop a citizen science instrument for studying space weather from your backyard. The PSWS is led by the University of Scranton, and includes participation from TAPR, Case Western Reserve University/W8EDU, the University of Alabama, the New Jersey Institute of Technology CSTR, MIT Haystack Observatory, Dartmouth College, and the amateur radio community at large.

The 2023 HamSCI workshop is organized by The University of Scranton with generous financial support provided by the United States National Science Foundation and ARDC. HamSCI is an officially recognized NASA Citizen Science project.

Invited Speakers

Invited Scientist Tutorial: Dr. Joseph Huba, “Modeling the Ionosphere with SAMI3”

Abstract: SAMI3 (Sami3 is Also a Model of the Ionosphere) is a global, comprehensive model of the ionosphere/plasmasphere system. It is based on the SAMI2 model developed at the Naval Research Laboratory (Huba et al., 2000). SAMI3 models the plasma and chemical evolution of seven ion species (H, He, N, O, N, NO and O). The ion temperature equation is solved for three ion species (H, He and O) as well as the electron temperature equation. Ion inertia is included in the ion momentum equation for motion along the geomagnetic field. The neutral composition and temperature can be specified by empirical models (e.g, NRLMSISE00, HWM14) or by first-principle atmosphere models (e.g., TIEGCM, WACCM-X, HIAMCM). SAMI3 uses a nonorthogonal, nonuniform, fixed grid. The grid is designed to optimize the numerical mesh so that the spatial resolution decreases with increasing altitude. SAMI3 can use an untilted or tilted dipole model of earth’s magnetic field, or an IGRF field model based on the Richmond apex model. A general overview of ionospheric physics and the SAMI3 model will be presented, as well as several applications of the code.

Bio: Dr. Joseph Huba completed his PhD in theoretical plasma physics at the University of Maryland in 1975. Following his graduation, he joined the Naval Research Laboratory as an NRC post-doc and eventually became a staff member. Between 1995 and 2018, he headed the Space Plasma Physics Section, part of the Beam Physics Branch at the Naval Research Laboratory. He is now a Vice President of Syntek Technologies whose clients include the US Federal government. Dr. Huba’s main research interests include boundaries and wave phenomena in plasmas, physical processes governing the Earth’s upper atmosphere, and approaches to modeling these systems. Over the last two decades he has been dedicated to writing advanced computer codes to simulate these systems, which incorporate algorithms capable of simulating their sheer complexity. Dr. Huba is a Fellow of the American Physical Society and the American Geophysical Union.

Invited Amateur Radio Tutorial: Mr. Jesse Alexander WB2IFS, “The Ham Radio Project: Exploring the Electromagnetic Spectrum”

Abstract: The National Radio Astronomy Observatory (NRAO) recently received funding from ARDC for a new 2-year project designed to teach young adults about the electromagnetic spectrum while sharing the excitement of amateur (ham) radio among BIPOC and LGBTQIA+ students. The project goals are to: Introduce students to the Electromagnetic Spectrum and radio technologies; develop a scalable, shareable curriculum via SuperKnova; provide hands-on activities to deepen subject knowledge, and support student attainment of Technician and General Class Amateur Radio Licenses.

Bio: Jesse Alexander WB2IFS/3 is an amateur radio operator leading the project's efforts to introduce young people to the wonder of the Electromagnetic Spectrum through hands-on ham radio based experiences. Jesse has been a licensed amateur radio operator since 1975, when he got hooked on amateur radio as a teenager reading ARRL's QST magazines at the Montclair Public Library in NJ. The stories about hams communicating with each other from Antarctic science stations and small Caribbean islands, chatting in Morse code through satellites, bouncing signals off the moon (Earth-Moon-Earth), and providing life-saving support during natural disasters filled him with wonder and curiosity! Jesse has more than 30 years of experience in technical writing, designing for people and companies involved in IT, wireless communications, and telecommunications, and is an award-winning poet, trainer, and entrepreneur. Jesse holds a B.S. and M.Eng. in Electrical Engineering from Howard University. He is a senior member of IEEE, ARES/RACES, ARRL/OTC, OMIK/ARC, and FISTS, and a life member of Alpha Phi Alpha Fraternity, Inc.

Keynote Speaker: Dr. Patricia Reiff W5TAR, “Forging Amateur-Professional Bonds”

Abstract: Amateurs have played an important role in scientific research for many centuries. Up until the time of automated computerized telescope searches, virtually all comets were discovered by amateurs. As David Levy (of comet Shoemaker-Levy fame) said, "Amateurs have time to observe and enjoy the sky. Professionals have to submit proposals, take data, and write papers." Amateurs have long held associations with professional scientists in the realms of botany, ornithology, and even fossil and meteorite hunting. Ham Radio operators have worked closely with meteorologists as stormspotters and to provide communication in times of severe weather or other emergencies. It is a very natural outgrowth that Ham Radio amateurs team up with space physicists and aeronomers who study the ionosphere and its dependences on solar disturbances, in the general term of "space weather". Stanford first created VHF SID ionospheric monitors for amateurs and schools, and the "Radio Jove" program from Goddard has enlisted amateurs in monitoring solar and Jovian radio emissions. Ham beacons using Joe Taylor's compression algorithms now are used to track amateur balloons that have sailed four more times around the Earth. Amateurs team up with college students to provide communication with Cubesats. We are entering a new era of amateur radio providing important information on the structure and variability of the ionosphere, especially during eclipses. Several HamSCI talks and posters were shown at the recent Chicago AGU meeting, and we look to this group to lead the way for future uses of ham radio in "real" scientific research. talks and posters were shown at the recent Chicago AGU meeting, and we look to this group to lead the way for future uses of ham radio in "real" scientific research.

Bio: Dr. Patricia Reiff W5TAR is a Professor in the Department of Physics and Astronomy at Rice University and was the founding Director of the Rice Space Institute. Dr. Reiff is highly regarded in both professional space science and amateur radio fields. She is a Fellow of the American Geophysical Union and has been involved in space plasma physics research for more than 50 years, with interests in magnetospheric reconnection, convection, plasma particle acceleration mechanisms, and solar wind control of the magnetosphere and ionosphere. She was a Co-I on the Dynamics Explorer, Polar, IMAGE, and Cluster Missions. She is a Co-I and Education/Public Outreach (EPO) lead for the MMS (Magnetospheric Multiscale Mission), and has served as Director for public education projects for over 30 years.  Her “Space Update” software has been used by over a million visitors at over 15 museums and distributed to 400,000 educators and learners. Dr. Reiff is also the developer and instructor of Rice University course PHYS 501: Physics of Ham Radio and trustee of the W5YG Rice University Amateur Radio Club. She has taught ham radio to new licensees as young as 8.

 

W3USR Special Event Station

The HamSCI Workshop will feature a real, working special event amateur radio station using the callsign W3USR! In-person participants are encouraged to stop by the station and guest operate or learn about how an amateur radio station works. We are grateful to the Murgas Amateur Radio Club K3YTL for organizing and running the W3USR Special Event Station. QSL information will be available here and on QRZ.com at a later date.

Amateur Radio Licensing and Exams

Although an amateur radio license is not a prerequisite to participate in HamSCI, we encourage participants to pursue a license. Getting a Technician Class license requires passage of a 35 question multiple choice test with a public question pool. Hamstudy.org provides free practice tests and materials and access to real online exam sessions. The ARRL also has an excellent selection of license study materials. You can also earn your amateur radio license at the HamSCI Workshop! An in-person Volunteer Examiner (VE) session will be held during the Saturday afternoon session. Please review the ARRL's "What to bring to an exam session" prior to the session. We are grateful to the Scranton Pocono Amateur Radio Club K3CSG (SPARK) for running this session.

Amateur Radio Through the Ages Exhibit

Amateur Radio Through the Ages Exhibit is an exhibit of historical amateur radios, QSL cards, QST magazines, and radio accessories on display at the University of Scranton Loyola Science Center / Hope Horn Gallery during the Spring 2023 semester. This exhibit is presented by the Murgas Amateur Radio Club K3YTL, The University of Scranton Amateur Radio Club W3USR, and The University of Scranton Department of Physics and Engineering, especially Tom Mayka W3TRM, Bill Gallagher WA3RA, Herb Krumich K2LNS, Ian Kellman K3IK, Phil Galasso K2PG, Elaine Kollar K3VQR, Dave Kirby N3SRO, Dr. Darlene Miller-Lanning, and Dr. Nathaniel Frissell W2NAF.

Friday Night Banquet and Door Prizes

The HamSCI Workshop Banquet will be help Friday, March 17, 2023 at the Historic Radisson Lackawanna Station Hotel and will feature keynote speaker Dr. Patricia Reiff, W5TAR. Thanks to a very generous donation from DXEngineering, this year we will have door prizes at the banquet! Door prizes include an Icom IC-7300 and ten $100 gift certificates to DXEngineering. Thank you, DXEngineering!

Logistics

Registration

In-Person Participation

In-person registration is now closed. However, you can still join us virtually! Please see below.

Virtual Participation

For those who cannot attend in-person, we offer a virtual participation option. Virtual participation will be via the Zoom platform. All oral presentations, tutorials, and the banquet keynote will be available via this platform. These presentations will be available for viewing after the workshop as well. Virtual participation is free of charge.

Location

The 2023 HamSCI Workshop will be held in the Loyola Science Center on The University of Scranton Campus.

Parking

Parking is provided free of charge during this event on the 4th floor and roof of the University of Scranton Parking Pavilion. Participants without University of Scranton parking permits must park on the 4th floor or the roof of the parking pavilion.

Lodging

Lodging will be available at the Radisson Lackawanna Station Hotel Scranton and the Hilton Scranton & Conference Center. Both hotels are in walking distance to the workshop.

• For reservations at the Radisson Lackawanna Station Hotel Scranton, please call 570-342-8300 or 866-715-7836 and say that you are reserving for the HamSCI Workshop. The rate of US$109/night + 13% tax is valid the nights of March 16 - 19, 2023.

Transportation

The University of Scranton and the HamSCI Workshop 2023 is located only 15 minutes from the Wilkes-Barre/Scranton (AVP) International Airport.

Participation Guidelines

All participants in the HamSCI Workshop 2023 are expected to treat each other with respect and follow the HamSCI Workshop 2023 Participation Guidelines, which include The University of Scranton's Non-Discrimination, Anti-Harassment, Sexual Harassment, and Sexual Misconduct Policies. In-person participants and presenters will be required to sign and abide by the The University of Scranton HamSCI Workshop 2023 Waiver.

Science/Program Committee

• Dr. Nathaniel Frissell, W2NAF, The University of Scranton, Chair
• Mr. Jesse Alexander, WB2IFS, National Radio Astronomy Observatory
• Dr. Kristina Collins, KD8OXT, Case Western Reserve University
• Dr. Philip Erickson, W1PJE, MIT Haystack Observatory
• Mr. Bill Liles, NQ6Z, HamSCI Community
• Ms. Veronica Romanek, KD2UHN, The University of Scranton

Local Organizing Committee

• Dr. Nathaniel Frissell, W2NAF, The University of Scranton, Chair
• Ms. Salisa Brown, The University of Scranton
• Prof. Rachel Frissell, W2RUF, The University of Scranton
• Ms. Frani Mancuso, The University of Scranton
• Ms. Veronica Romanek, KD2UHN, The University of Scranton
• Dr. Christine Zakzewski, The University of Scranton

Questions?

Please e-mail [email protected].

The 2023 HamSCI workshop is organized by The University of Scranton with generous financial support provided by the United States National Science Foundation (NSF) and Amateur Radio Digital Communications (ARDC). HamSCI is an officially recognized NASA Citizen Science project.