March 20-21, 2020
A Virtual Workshop Hosted by The University of Scranton

Come join HamSCI at its third annual workshop! Due to restrictions caused by the COVID-19 Coronavirus, this year's workshop will he held as a virtual, eletronic workshop.  The meeting will take place March 20-21, 2020 using Zoom Webinar Services hosted by The University of Scranton in Scranton, PA . The primary objective of the HamSCI workshop is to bring together the amateur radio community and professional scientists. The theme of the 2020 HamSCI Workshop is "The Auroral Connection: How does the aurora affect amateur radio, and what can we learn about the aurora from radio techniques?" Invited speakers include Dr. Elizabeth MacDonald, NASA Scientist and founder of Aurorasaurus, Dr. James LaBelle, Dartmouth Space Scientist and expert on radio aurora, and Dave Hallidy K2DH, an expert in ham radio auroral communication.

This workshop will also serve as a team meeting for the HamSCI Personal Space Weather Station project, an 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 ham radio community at large.

Participation and Registration

Participation in the 2020 HamSCI Workshop will be via Zoom Webinar. Registration and participation is free and open to all. To prepare and make sure you are ready to participate in the 2020 HamSCI Workshop, please visit the Zoom Website and create free account. You can then download the client software and test it by creating your own free test meeting. The Zoom client will work on Windows, Apple OS X, Linux, Android, iPad, and iPhone.

This meeting is being recorded and will be available later.

Community Participation Guidelines

All participants in the HamSCI workshop must adhere to the HamSCI Community Participation Guidelines. Those that do not follow these guidelines will be asked to leave.

Presenter Information

Oral presentations will be given in the same format as if they were at the in-person workshop. Please familiarize yourself with the Zoom teleconferencing software by creating a free Zoom account, downloading the client software, and testing it by creating your own free test meeting.

Posters and demonstrations will also be presented via Zoom, but there are special instructions to adapt the poster session to electronic format. If you are a Poster or Demonstration presenter, please click here for updated information.

Invited Speakers

Invited Talk: Tim Duffy, K3LR, “Let’s Push the Exploration of the Ionosphere to The Next Level”

Tim has been an active amateur radio operator for 47 years. He has hosted 132 different operators from around the world as part of the K3LR Multi-Multi DX radio sport contest efforts since 1992. He was the ARRL Atlantic Division Technical Achievement award winner in 1998. Tim has been the moderator of the Hamvention Antenna forum for 34 years. K3LR serves as chairman of Contest University (13 years), the Dayton Contest Dinner (27 years), chairman of the Top Band Dinner – as well as coordinator of the Contest Super Suite (34 years) in Dayton during the yearly Hamvention. He is founder and moderator of the popular RFI Reflector ([email protected]) since 1999. Tim serves on the board of directors of the World Wide Radio Operators Foundation (WWROF) as Chairman and is President Emeritus of the Radio Club of America (RCA). Tim is President of the Mercer County Amateur Radio Club (W3LIF). Tim was elected to the CQ Contest Hall of Fame in 2006. He was honored with the prestigious Barry Goldwater Amateur Radio service award by the RCA in 2010. K3LR was honored as Hamvention Amateur of the Year in 2015 by the Dayton Amateur Radio Association. Tim is the Chief Executive Officer and General Manager at DX Engineering. He is a graduate of the Pennsylvania State University.

Invited Talk: David Hallidy, K2DH, “Amateur Auroral Communications”

Dave is a retired microwave engineer, having been employed in the RF and Microwave field for most of his adult life. He has been a licensed amateur radio operator for 53 years, since the age of 16. For many years, Dave “chased DX”- that is, attempted to contact amateurs in as many foreign countries as possible and now has confirmed contacts with 330 “entities”. In 1983, he became interested in the frequencies above 30MHz, and has experimented with signal propagation on the HF, VHF, UHF and SHF amateur bands ever since. His interests today include Aurora, Meteor Scatter, MoonBounce, Tropospheric Ducting and other unusual modes of signal propagation unique to the VHF, UHF, and SHF bands. He first experienced Auroral signal propagation in 1985, while living in Texas. An intense Aurora occurred, affecting signals as far as South Texas. Not understanding the phenomenon, he was surprised to hear some of his fellow amateurs attempting to talk and use Morse code, but with highly distorted signals- the usual pure tones of radiotelegraphy were merely a broken hissing sound and voice signals sounded like people whispering. After a while he realized that this was due to distortion caused by reflection of the signals via the Auroral Curtain. During that event, he made contacts as far away as 1000 miles on the 144 and 432MHz amateur bands. After that, he was “hooked”- whenever there were reports of Aurora, he was there, attempting to make contacts with friends around the country. After moving back to New York State, where radio Aurora is more frequent due to the closer proximity to the Auroral Curtain, he has continued to experiment with making contacts on the higher frequencies. In 1989 during a particularly intense Auroral event, he successfully made an Auroral contact with a station in Northern Canada on the 902MHz band, where it had never been achieved before. Dave lives with his wife in Rochester, NY and can be reached by email at: [email protected].

Invited Talk: Dr. Elizabeth MacDonald, “Aurorasaurus: Citizen Science Observations of the Aurora”

Liz MacDonald's research has focused on experimental particle measurement techniques and data analysis in the magnetosphere and ionosphere for the last 15 years. Liz is currently a Co-Investigator (Co-I) on the Helium, Oxygen, Proton, and Electron Spectrometer on the NASA Van Allen Probes mission. At Los Alamos National Laboratory, Liz was the Principal Investigator (PI) for the Z-Plasma Spectrometer on the DOE Space and Atmospheric Burst Reporting System (SABRS) geosynchronous payload. Liz also led the Innovative Research and Integrated Sensing (IRIS) team. In the recent past Liz led the DoE-funded Technology Infusion Project entitled Modular Advanced Space Environment Instrumentation (from 2009-2011) and served as the PI for the Advanced Miniaturized Plasma Spectrometer on the DOE SABRS Validation Experiment payload (2007-2008). Liz has a blend of expertise in both instrument development and data analysis and interpretation that comes from sounding rocket and satellite instrumentation experience. This experience ranges over the complete cycle of instrument production, including design and modeling, integration and testing, calibration, satellite operations, and in situ scientific data analysis. General interests include instrument technology development, basic magnetospheric science, and space situational awareness national priorities. Specific research interests include wave-particle interactions and the effect of plasma on radiation belt dynamics, mapping, coupling, and transport between the ionosphere and the inner magnetosphere, and the impact of heavy ions on geomagnetic storm processes. Liz holds Masters and PhD degrees from the University of New Hampshire and a Bachelor's in Physics from the University of Washington (largely funded by a NASA Space Grant scholarship). Liz is the founder and leader of Aurorasaurus, a citizen science project for the study of the aurora.

Invited Talk: Dr. James LaBelle, “Observing Radio Signals of Auroral Origin”

Jim LaBelle is an experimental space plasma physicist. He has been at Dartmouth since 1989. He earned his undergraduate degree in physics from Stanford University (1980), followed by masters and doctorate degrees in applied physics from Cornell University (1982 and 1985). He did post-doctoral work at the Max-Planck Institute for Extraterrestrial Physics in Garching, Germany (1985-7) and at Utah State University in Logan, Utah (1987-9). He is a member of the American Geophysical Union and the International Union of Radio Scientists. He has had visiting fellowships at the Max-Planck Institute for Extraterrestrial Physics (1997, 2000-2001) and at the University of Sydney (2008). In 2010, he was appointed to the inaugural Lois L. Rodgers Professorship at Dartmouth.

Science/Program Committee

• Dr. Nathaniel Frissell, W2NAF, University of Scranton, Chair
• Dr. Phil Erickson, W1PJE, MIT Haystack Observatory
• Dr. Cathryn Mitchell, M0IBG, University of Bath
• Dr. Elizabeth MacDonald, NASA Goddard Space Flight Center
• Mr. Bill Liles, NQ6Z, HamSCI Community

Local Organizing Committee (University of Scranton)

• Dr. Mohammad A. Maktoomi, Chair
• Dr. Declan Mulhall
• Ms. Laurie McCoy, Administrative Assistant
• Ms. Frani Mancuso, Executive Director of Conference & Event Services

Questions?

Please e-mail [email protected].

The 2020HamSCI Workshop is hosted by The University of Scranton. Financial support is provided by the United States National Science Foundation.

Come join HamSCI at its second annual workshop! The workshop will be held March 22-23, 2019 at Case Western Reserve University in Cleveland, OH and seeks to bring together the amateur radio community and professional scientists. Anyone interested in this workshop is invited to join.

Cost and Registration

• Friday Registration: $100 (Includes Breakfast, Lunch, and Banquet Ticket)
• Saturday Registration: $50 (Includes Breakfast, Lunch, and Dinner)
• Friday Banquet Ticket Only: $50

Call for Speakers

We are especially looking for speakers with presentations showing analysis of ionospheric observations, ideas and proposals for the design of the Personal Space Weather Station and instrumentation for the 2024 eclipse. We will also accept other presentations related to amateur radio and science. Presentations will be in the form of oral talks, posters, lightning talks, and demo room tables. Abstract and acceptance and presentation format will be chosen by the Science Program Committee. If you would like to present, please e-mail your abstract to Nathaniel Frissell, W2NAF, at [email protected] by February 10, 2019. Presenters will be notified by March 1, 2019.

In your abstract e-mail to [email protected], please include:

• Title of Presentation
• Name of Presenter
• Co-Author List with Call Signs and Affiliations
• Abstract, limited to 1 paragraph and 350 words
• Request of presentation or demo room table

You may request a poster presentation format. Due to time constraints requests for oral presentation slots are not guaranteed.

Program

This year’s theme will be “Ionospheric Effects and Sensing,” which includes the use of amateur radio techniques for the characterization and study of ionospheric phenomena such as traveling ionospheric disturbances, sporadic E, response to solar flares, geomagnetic storms, the 2024 total solar eclipse other space weather events. In order to facilitate this science, continued development of the HamSCI Personal Space Weather Station and discussion of integration of amateur radio into the collegiate curriculum will also take place. Featured speakers include well-known amateur radio author Ward Silver, N0AX, propagation specialist Carl Luetzelschwab, K9LA, and MIT Haystack Observatory Ionospheric Scientist Dr. Larisa Goncharenko. We will also accept presentations relating to amateur radio and science, particularly space and atmospheric science, space weather, and radio astronomy. 

On Saturday afternoon, after lunch, the conference proceedings will continue at CWRU's think[box], a student manufacturing facility and makerspace that is open to the public. Attendees will participate in tours of think[box] facilities; tours of the Case Amateur Radio Club, W8EDU; and an amateur radio licensing session. There will also betime available for breakout sessions and committee discussions. The conference will close on Saturday evening with a screening of Contact at CWRU Film Society. Tickets to the film are complimentary with a conference badge.

View Agenda, Videos, and Presentation PDFs

Friday Keynote: Tim Duffy, K3LR

Tim has been an active amateur radio operator for 47 years. He has hosted 132 different operators from around the world as part of the K3LR Multi-Multi DX radio sport contest efforts since 1992. He was the ARRL Atlantic Division Technical Achievement award winner in 1998. Tim has been the moderator of the Hamvention Antenna forum for 34 years. K3LR serves as chairman of Contest University (13 years), the Dayton Contest Dinner (27 years), chairman of the Top Band Dinner – as well as coordinator of the Contest Super Suite (34 years) in Dayton during the yearly Hamvention. He is founder and moderator of the popular RFI Reflector ([email protected]) since 1999. Tim serves on the board of directors of the World Wide Radio Operators Foundation (WWROF) as Chairman and is President Emeritus of the Radio Club of America (RCA). Tim is President of the Mercer County Amateur Radio Club (W3LIF). Tim was elected to the CQ Contest Hall of Fame in 2006. He was honored with the prestigious Barry Goldwater Amateur Radio service award by the RCA in 2010. K3LR was honored as Hamvention Amateur of the Year in 2015 by the Dayton Amateur Radio Association. Tim is the Chief Operating Officer and General Manager at DX Engineering. He is a graduate of the Pennsylvania State University

Invited Talk: Carl Luetzelschwab, K9LA, "Ham Radio for Space Scientists"

Carl started his radio career as a shortwave listener in the late 1950s, and received his Novice license (WN9AVT) in October 1961. He selected K9LA in 1977. He enjoys propagation, DXing (he’s at the top of the Honor Roll), contesting (he was NCJ Editor from 2002-2007), playing with antennas and fixing/using vintage equipment. Carl is a graduate of Purdue University (BSEE 1969, MSEE 1972) and worked for Motorola and Magnavox/Raytheon as an RF design engineer (mostly designing solid-state RF power amplifiers). He retired in October 2013. He and his wife Vicky (AE9YL) reside in Fort Wayne and enjoy traveling, which has included DXpeditions to Syria, Market Reef and numerous trips to the Cayman Islands. Carl is currently the ARRL Central Division Vice Director. He has received the Bill Orr W6SAI Technical Writing Award, the YASME Foundation Excellence Award and the Indiana Radio Club Council Technical Excellence Award.

Invited Talk: Dr. Larisa Goncharenko, "Space Science for Ham Radio Operators"

Dr. Larisa Goncharenko is a research scientist at the Haystack Observatory, Massachusetts Institute of Technology. Her major areas of interest are ionospheric-thermospheric coupling, and the dynamics and electrodynamics of the ionosphere and thermosphere, with an emphasis on processes in the lower thermosphere and coupling with lower altitudes. Goncharenko's undergraduate and graduate education was in Physics (High Honors), 1988, at Kharkiv National Polytechnic University, Kharkiv, Ukraine. She has held research positions at Kharkiv National Polytechnic University (1988-1996) and Haystack Observatory, MIT (Visiting Scientist, 1994-1995; Postdoctoral Fellow, 1996-1997; Research Scientist, 1997 to present). Goncharenko's research in Ukraine was focused on ionospheric modification by HF heating facility (similar to those in Arecibo or EISCAT) and diagnostics of modifications with the Kharkov incoherent scatter radar. Her research at MIT includes experimental studies using multiple incoherent scatter radars, GPS TEC data, ionosondes, satellite data, and collaborations with multiple modeling groups. She is the recipient of the CEDAR Prize Lecture award (2012), NASA Group Achievement Award (2008), and an MIT Excellence Award (2003). She is the author or coauthor of more than 70 refereed publications.

Meeting Location and Parking

The Friday sessions and Saturday morning sessions will be held in the Premier Industrial Lecture Hall in the Dively Building on the CWRU campus. The Friday evening banquet will be held at Nighttown. On Saturday afternoon, proceedings will move to CWRU think[box] for workshops and demonstrations, as well as tours of the Case Amateur Radio Club, W8EDU. The conference will conclude with a screening of Contact at Strosacker Auditorium, presented by the CWRU Film Society.

Paid parking is available near each venue. Near Dively, participants are advised to park in the Ford Garage. Parking for Nighttown is available next to the restaurant.  When visiting think[box] and the other destinations on the Case quad (W8EDU, Film Society), attendees should park in the Veale Garage and enter think[box] through Veale Center.

Breakfasts, Lunches, and Friday Banquet

Breakfasts, lunches, and coffee breaks are included with registration for both Friday and Saturday. Special dietary needs can be specified when registering.

The Friday Banquet Dinner will be hosted at Nighttown, with keynote speaker Ward Silver N0AX. Banquet tickets are included with Friday registration. Separate/additional banquet tickets may be purchased for $50 each.

Nighttown
12383 Cedar Rd
Cleveland, OH 44106

Lodging

A block of hotel rooms has been reserved at the Cleveland Courtyard by Marriott, a short walk from the Dively Building. For the nights of March 21, 22, and 23, rooms are available at the CWRU nightly rate of $165. Participants may reserve a room by calling 1-800-MARRIOTT and identifiying themselves as part of the HamSCI group under CWRU. Reservations must be placed by March 1, 2019 in order to receive the discounted rate.

Other nearby hotel options include Glidden House, a short walk from the conference, and the Tudor Arms Hotel, a short drive.

Flight Information and Ground Transportation

Easy access to CWRU and the HamSCI meeting is available through the RTA Red Line, which connects directly to Cleveland Hopkins International Airport. If coming from the airport, take the Red Line to the Little Italy station.

Talk-In Frequencies

Every party should have a call-in frequency; if you have an HT, check in en route to ask directions or say hello.

• Primary Simplex: 146.55 MHz
• Secondary Simplex: 432.10 MHz
• Repeater: KD8LDE/R 442.28750 MHz + 131.8 Hz

Local Organizing Committee

• Ms. Kristina Collins, KD8OXT, Chair
• Dr. David Kazdan, AD8Y, Advisor
• Mr. Nathaniel Vishner, KB1QHX

Science/Program Committee

• Dr. Nathaniel Frissell, W2NAF, NJIT, Chair
• Dr. Phil Erickson, W1PJE, MIT Haystack Observatory
• Dr. Ethan Miller, K8GU, JHU/APL
• Mr. Bill Liles, NQ6Z, HamSCI Community

Questions?

If you have questions, please e-mail [email protected]. Logistics questions will be directed to Kristina Collins, KD8OXT (216-368-3579) and science/program questions will be directed to Nathaniel Frissell, W2NAF (973-787-4506).

The 2019 HamSCI Workshop is hosted by Case Western Reserve University in collaboration with the New Jersey Institute of Technology. Financial support is provided by the United States National Science Foundation.

Switch to plain text editor More information about text formats Text format Web page addresses and e-mail addresses turn into links automatically. Convert [icon:%bundle:%icon] tags. Global tokens will be replaced with their respective token values (e.g. HamSCI or Publications). Lines and paragraphs break automatically. Image Files must be less than 512 MB. Allowed file types: png gif jpg jpeg. FILE Add a new file Files must be less than 512 MB. Allowed file types: txt. HIDDEN IMAGES Add a new file Files must be less than 512 MB. Allowed file types: png gif jpg jpeg. Vertical Tabs Menu settings Not in menu (active tab) URL path settings Alias: hamsci2019 Revision information New revision URL redirects 1 enabled redirect Authoring information By kd8oxt on 2018-12-01 23:56:35 -0500 Publishing options Published Provide a menu link Query Home Dashboard Content Structure Appearance People Modules Configuration Reports Help Log out Hello jwalker

8 December 2019: Data from the FFM is currently being processed.If you submitted data to the Festival of Frequency Measurement, and your callsign is omitted from the list below, contact [email protected]:
AA8K, AC6SL, AG7PQ, AJ4YA, K0ANS, K2LYV, K4BSE, K7JKM, K7KMQ, KA6WKE, KE0ARE, KG4ARN, KM4YMI, N1IRO, N1NAZ, N2MD, N7IVV, N7QNM, N7XZ, N8OBJ, N9MVO, NA0B, NU0C, VA3ROM, VE3OAT, VE3YX, VE6GRT, VE6IXD, VE7CNF, VK3ZAZ, W1KU, W3FAY, W6BM, W6MSU, W6OQI, W8EDU, W9INE, WA5FRF, WA7BNM, WB4HIR, WB6HYD, WV5L, WX4US, XE3I

Data is available at https://zenodo.org/record/3707210.

Introduction

Contact information:

https://groups.google.com/forum/#!forum/festival-of-frequency-measurement/join

David Kazdan: [email protected]

Research Questions

• How does WWV 5 MHz's HF propagation path vary over one UTC calendar day?
• How do various measurement techniques for understanding the path variation compare?

Objective

• Measure Doppler shifts caused by space weather's effects on the ionosphere.
• Use a specified measurement protocol available to amateur radio operators and other citizen-scientists.

Times

• (Control Day was 01 August 01 2019, 0000 – 2359 UTC)
• Centennial Day: 01 October 2019, 0000 – 2359 UTC

The Beacons

The NIST beacon station WWV in Fort Collins, Colorado, USA (and co-located WWVB) is shown here:

WWV broadcasts on 2.5, 5, 10, 15, 20, and 25 MHz.  This experiment will use only the 5 MHz transmissions. If you want to participate and cannot record the 5 MHz signal, use whichever WWV frequency you can and make sure the file is labeled appropriately.

The recordings in this experiment are expected to show formations of the D-layer at stations' local sunrise and other daily events of the ionosphere.  Space weather varies day to day and some features may be prominent.  We'll see what we get!

Procedures

1) Prepare Your Receiver, Computer, and Software (fldigi)

• Download fldigi, install it, verify that it's working correctly.  Find the "frequency analysis" module in the "op mode" pulldown menu.
• Set your receiver's mode to USB (upper sideband).  Tune an AM station's carrier to 1000 Hz audio by setting your receiver that much below the carrier frequency.  For 5 MHz WWV, tune to 4.999 MHz and listen for the 1000 Hz tone (musicians: 1000 Hz is musically below C two above middle C [i.e., C₆] if you want to check that way).
• Look for the 1000 Hz line on fldigi's waterfall.  Click the cursor there or use the offset frequency box at the bottom of fldigi's screen.  Look for "writing CSV file" on the lower line of fldigi, toward the left.
• Now, leave fldigi alone.  Every time you make a change or move that cursor, the CSV file ("comma-separated variables," the data file you're recording) will be erased and a new one started.  It's maddeningly easy to delete your work and fldigi does not make a backup.
• Robert, VA3ROM, has offered a batch file for automating the renaming.  It is for Windows.  It may be found at the end of this document; use it if you wish but do try it before the event.
• At the end of your recording period, close fldigi. The file "analysis.csv" should be in your /fldigi/temp/ directory.
• Try all this before the day of the event.

2) Collect the data: Make sure Windows cannot be shut down by an automatic update!

• Start as above. Now, leave fldigi alone.  Every time you make a change or move that cursor, the CSV file ("comma-separated variables," the data file you're recording) will be erased and a new one started.  It's maddeningly easy to delete your work and fldigi does not make a backup.
• At the end of your recording period, close fldigi. The file "analysis.csv" should be in your /fldigi/temp/ directory.
• Rename the file with your callsign and location.
• Again, try all this before the day of the event.

3) Rename the Data File

• You should finish with one data file named "analysis.csv". It should be about 2 MB.
• Rename it with your callsign and location and frequency: "AD8Y 41.49 -81.58 5 MHz.csv"
• Use the Maidenhead locator if you don't have latitude/longitude: "AD8Y EN91fl 5 MHz.csv"

4) Upload to Zenodo

Data Description

In the data description box, please include: "Festival of Frequency Measurement 1 October 2019

Data Notes

Also in the Data Description box, you may include your personal comments regarding your observations. The "Description" block accepts multiple lines.

• Your Name and Callsign
• Latitude and Longitude of the Recording
• Start time of the .csv file
• A description of station hardware configuration, including
  • Antenna type
  • Antenna pointing direction (if applicable)
  • Receiver type
  • Frequency reference type
  • Frequency measurement technique
• Any other information you believe would be necessary for proper scientific interpretation of your measurements

If you find it helpful, you may copy the following template and include it with your submission. Again, you are encouraged to include any other information you feel may be helpful.

Festival of Frequency Measurement Submission

—-

event: WWV Centennial

UTC date:

beacon frequency:

station name:

latitude and longitude and/or maidenhead grid square: 

city:

state or region:

Difficulties had:

Anything you know about the stability of your equipment:

soapbox:

Data License

Please license your data as:

• Open Source
• Creative Commons Attribution 4.0

----------------------------------------------------------------

VA3ROM batch file:

Page Contributors: WA9VNJ, N8UR, W8RKO, W2NAF, KD2JAO, KM4EGE, AD8Y, KB3UMD, VA3ROM

Last edit: 19 Septembr 2019

HamSCI at Hamvention 2017

Overview

HamSCI will be present at the 2019 Dayton Hamvention in order to further its goal of connecting the ham radio and scientific communities. Support for the 2018 HamSCI Hamvention activities comes from the  New Jersey Institute of Technology Center for Solar-Terrestrial Research, the Yasme Foundation, the National Science Foundation, and volunteers like you. This year, HamSCI will again host a booth in the "Ham Radio 2.0: Innovation and Discovery" row, host booth talks, demos, and the HamSCI Forum. To help out, please sign up to volunteer at the booth or offer to give a booth talk.

Booth Volunteering

Please use sign up to volunteer at the booth using the SignUp.com. As a volunteer, we ask that you stand at the HamSCI booth and talk to booth vistors about HamSCI and your specific research interests. Feel free to bring demonstation items and materials and to talk about what you know best. The goal of HamSCI is to connect ham radio with scientific research. So, any topic that supports this goal is a good topic to talk about. The booth uniform are HamSCI labcoats, which can be purchased below. For questions regarding booth volunteering, please e-mail Bill Liles NQ6Z at [email protected] and George Lemaster WB5OYP at [email protected].

Volunteer Sign-Up

Lab Coats

HamSCI labcoats may be ordered from https://www.allheart.com/product.aspx?p=ah8200. 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.

Example Order

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, you may purchase an exhibitor badge for $20. 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. If you would like an exhibitor badge, please e-mail Bill Liles NQ6Z at [email protected] and George Lemaster WB5OYP at [email protected].

Group Photo

A HamSCI group photo will be taken during the Hamvention on Friday at 12:00 PM at the HamSCI booth. Wear your labcoats!

HamSCI Presentations

Booth Talks

Booth talks include both HamSCI and Ham Radio 2.0 Talks.

Friday Booth Talks

Friday, May 17, 2019	Group	Title	Presenter	Organization	Home QTH
10:00 AM	HR 2.0	Moonbounce Via the MIT Remote Linked EME Station	Marty Sullaway, NN1C		Waban, MA
11:00 AM		New Directions in Sporadic-E Research	Bill Engelke, AB4EJ	University of Alabama	Tuscaloosa, AL
12:00 PM	HR 2.0	Contesting with FT4 - Issues and Opportunities Going Forward	John Pescatore, K3TN		Ashton, MD
1:00 PM		The Third Source of F2 Region Variability	Carl Luetzelschwab, K9LA		Fort Wayne, IN
2:00 PM	HR 2.0	How Real-Time Scoreboards Change Contesting	Victor Androsov, VA2WA and Randy Thompson, K5ZD		Boucherville, QC, Canada and Uxbridge, MA
3:00 PM		RBN & WSPRNet Response to September 2017 Solar Flares and Storms	Nathaniel Frissell, W2NAF	New Jersey Institute of Technology	Newark, NJ

Saturday Booth Talks

Saturday, May 18, 2019	Group	Title	Presenter	Organization	Home QTH
10:00 AM	HR 2.0	Balloon Pico Races	William Brown, WB8ELK		Madison, AL
11:00 AM		The Polar Environment Atmospheric Research Laboratory (PEARL) and VY0ERC:  Atmospheric Science and Ham Radio at 80N	Pierre Fogal, VE3KTB	Polar Environment Atmospheric Research Laboratory (PEARL) / University of Toronto	Ellesmere Island, Canada
12:00 PM	HR 2.0	Youth Contesting Program in North America and Europe	Jocelyn Brault, KD8VRX, Bryant Rascoll, KG5HVO, and Philipp Springer, DK6SP		Liberty Township, OH, Montgomery, AL, and Erding, Germany
1:00 PM		Propagation on 630m and 2200m	Carl Luetzelschwab, K9LA		Fort Wayne, IN
2:00 PM	HR 2.0	SOTA and New Methods of Portable Operating	Paula Uscian, K9IR		Hoffman Estates, IL
3:00 PM		HF Satellite Observations of Field Day	Gareth Perry, KD2SAK	New Jersey Institute of Technology	Newark, NJ

Demonstrations

If you would like to give a demonstration, please e-mail Bill Liles NQ6Z at [email protected] and George Lemaster WB5OYP at [email protected].

Friday Demonstrations

Saturday Demonstrations

HamSCI Forum

Booth Location

HamSCI will be at Booth 4304 in the Ham Radio 2.0: Innovation and Discovery Area.

Questions?

If you have questions, please contact Nathaniel W2NAF at [email protected].

RBN-WSPRNet Daily Histograms

The RBN-WSPRNet Daily Histograms are used to monitor global high frequency (HF) ham radio communications in relation to space weather activity. The following data are shown:

• Panel (a) shows geomagnetic activity indices derived from ground-based magnetometer data, including the SYM-H index (black line) and Kp Index (colored stems).
• Panel (b) shows X-ray flux measurements made by the GOES satellites for monitoring solar flares.
• Panels (c) - (h) show density maps and histograms of ham radio spots/QSOs from the Reverse Beacon Network and WSPRNet. The data are located at the midpoint of the transmitter and receiver. Map bin sizes are 1˚ lat by 1˚ lon, and histogram bin sizes are 10 min by 250 km. When a user‐reported location is not available, a lookup to a public database such as http://qrz.com or http://hamcall.net is made. If location is not provided and a database lookup is not available, the spot is discarded.

HF Ham Radio Data

To monitor HF radio communications, we use data from two separate automated amateur radio monitoring networks, the Reverse Beacon Network (RBN) and the Weak Signal Propagation Reporting Network (WSPRNet). These networks operate continuously and are built, operated, and maintained on a volunteer basis by members of the amateur radio community. For a detailed analysis of a solar flare and geomagnetic storm event using this type of data, please see Frissell et al. (2019). RBN and WSPRNet data have been aggregated and provided by Bill Engelke, AB4EJ, University of Alabama DXDisplay. Visualizations by Nathaniel Frissell, W2NAF, NJIT CSTR.

Kp Index

The Planetary K (Kp) index is a quasi‐logarithmic scale from 0 to 9 that quantifies the level of geomagnetic disturbance (Menvielle & Berthelier, 1991). This index is calculated using observations from 13 midlatitude (±44°–60° magnetic latitude) ground magnetometers located in North America, Europe, and Australia. Hence, Kp is most indicative of geomagnetic conditions in these regions. At each station, fluctuations in the strength of the horizontal component of the magnetic field are observed over a 3‐hr interval. The resulting value is subsequently associated with an individual K value based on the geomagnetic latitude of the measurement station, such that a station near the equator requires less geomagnetic fluctuation than a station near the poles in order to record the same K value. Finally, the weighted mean of measurements from all Kp observatories allows calculation of a global Kp value. Kp was obtained from the NASA Goddard Space Flight Center OMNIWeb (King & Papitashvili, 2006).

SYM-H Index

The SYM‐H index is a measure of disturbances from background in the low‐latitude horizontal component of the magnetic field and is considered a high‐time resolution (1 min) version of the hourly disturbance storm time Dst index (Iyemori, 1990; Sckopke, 1966; Wanliss & Showalter, 2006). Observations from 6 out of 11 possible ground magnetometer stations evenly distributed in longitude and in the range of ±10°–50° magnetic latitude contribute to the SYM‐H index. SYM‐H monitors the intensity of the magnetospheric ring current. A negative SYM‐H value indicates an intensification of the ring current and is associated with geomagnetic storm activity. SYM‐H was obtained from the Kyoto World Data Center for Geomagnetism.

GOES X-Ray Flux

In addition to the two previously described indices, data from the Geostationary Operational Environmental Satellite (GOES) system is also used. This consists of observations from the GOES‐13 (GOES‐EAST, θ = −75°E) and GOES‐15 (GOES‐WEST, θ = −135°E) platforms. Each satellite carries an XRS providing 0.1–0.8 nm X‐ray irradiance observations (Chamberlin et al., 2009). A solar flare can cause sudden and unexpected fluctuations in solar X‐ray irradiance. GOES XRS measurements were retrieved from the NOAA National Center for Environmental Information (NCEI).

Software Acknowledgments

We acknowledge the use of the Free Open Source Software projects used in this analysis: Ubuntu Linux, python (van Rossum, 1995), matplotlib (Hunter, 2007), NumPy (Oliphant, 2007), SciPy (Jones et al., 2001), pandas (McKinney, 2010), xarray (Hoyer & Hamman, 2017), iPython (Pérez & Granger, 2007), and others (e.g., Millman & Aivazis, 2011).

References

Chamberlin, P. C., Woods, T. N., Eparvier, F. G., & Jones, A. R. ( 2009). Next generation X‐ray sensor (XRS) for the NOAA GOES‐R satellite series, Solar Physics and Space Weather Instrumentation III. San Diego, CA: Society of Photo‐Optical Instrumentation Engineers (SPIE). https://doi.org/10.1117/12.826807

Frissell, N. A., Vega, J. S., Markowitz, E., Gerrard, A. J., Engelke, W. D., Erickson, P. J., et al. ( 2019). High‐frequency communications response to solar activity in September 2017 as observed by amateur radio networks. Space Weather, 17, 118– 132. https://doi.org/10.1029/2018SW002008

Hoyer, S., & Hamman, J. ( 2017). xarray: N‐D labeled arrays and datasets in Python. Journal of Open Research Software, 5( 1), 10. https://doi.org/10.5334/jors.148

Hunter, J. D. ( 2007). Matplotlib: A 2D graphics environment. Computing in Science & Engineering, 9( 3), 90– 95. https://doi.org/10.1109/MCSE.2007.55

Iyemori, T. ( 1990). Storm‐time magnetospheric currents inferred from mid‐latitude geomagnetic field variations. Journal of Geomagnetism and Geoelectricity, 42( 11), 1249– 1265. https://doi.org/10.5636/jgg.42.1249

Jones, E., Oliphant, T., & Peterson, P. ( 2001). SciPy: Open source scientific tools for Python. Retrieved from http://www.scipy.org/

King, J., & Papitashvili, N. ( 2006). One minute and five minute solar wind data sets at the Earth's bow shock nose. Greenbelt, MD: NASA Goddard Space Flight Center/Space Physics Data Facility. http://omniweb.gsfc.nasa.gov/html/HROdocum.html

McKinney, W. ( 2010). Data structures for statistical computing in Python. In S. van der Walt & J. Millman (Eds.), Proceedings of the 9th Python in Science Conference (pp. 51– 56). Austin, TX: SciPy.org. https://conference.scipy.org/proceedings/scipy2010/pdfs/mckinney.pdf

Menvielle, M., & Berthelier, A. ( 1991). The K‐derived planetary indices: Description and availability. Reviews of Geophysics, 29( 3), 415– 432. https://doi.org/10.1029/91RG00994

Millman, K. J., & Aivazis, M. ( 2011). Python for scientists and engineers. Computing in Science & Engineering, 13( 2), 9– 12. https://doi.org/10.1109/MCSE.2011.36

Oliphant, T. E. ( 2007). Python for scientific computing. Computing in Science & Engineering, 9( 3), 10– 20. https://doi.org/10.1109/MCSE.2007.58

Pérez, F., & Granger, B. E. ( 2007). IPython: A system for interactive scientific computing. Computing in Science & Engineering, 9( 3), 21– 29. https://doi.org/10.1109/MCSE.2007.53

Rossum, G. ( 1995). Python tutorial (Technical Report CS‐R9526). Amsterdam: Centrum voor Wiskunde en Informatica, (CWI). https://ir.cwi.nl/pub/5007/05007D.pdf

Sckopke, N. ( 1966). A general relation between the energy of trapped particles and the disturbance field near the Earth. Journal of Geophysical Research, 71( 13), 3125– 3130. https://doi.org/10.1029/JZ071i013p03125

Wanliss, J. A., & Showalter, K. M. ( 2006). High‐resolution global storm index: Dst versus SYM‐H. Journal of Geophysical Research, 111, A02202. https://doi.org/10.1029/2005JA011034

Panel (a) shows geomagnetic activity indices derived from ground-based magnetometer data, including the SYM-H index (black line) and Kp Index (colored stems). Panel (b) shows X-ray flux measurements made by the GOES satellites for monitoring solar flares. Panels (c) - (h) show density maps and histograms of ham radio spots/QSOs from the Reverse Beacon Network and WSPRNet. The data are located at the midpoint of the transmitter and receiver. Map bin sizes are 1˚ lat by 1˚ lon, and histogram bin sizes are 10 min by 250 km. When a user‐reported location is not available, a lookup to a public database such as http://qrz.com or http://hamcall.net is made. If location is not provided and a database lookup is not available, the spot is discarded. Click here for a detailed explanation.

Visualizations by Nathaniel Frissell, W2NAF, NJIT CSTR. Kp was obtained from the NASA Goddard Space Flight Center OMNIWeb (King & Papitashvili, 2006). SYM‐H was obtained from the Kyoto World Data Center for Geomagnetism. GOES XRS measurements were retrieved from the NOAA National Center for Environmental Information (NCEI). RBN and WSPRNet data have been aggregated and provided by Bill Engelke, AB4EJ, University of Alabama DXDisplay.

This page is developed and maintained by Nathaniel Frissell W2NAF, Evan Markowitz KD2IZW, and Diego Sanchez KD2RLM.

Motivation

Since the beginning of the United States amateur radio service in 1912, amateur radio operators have made significant contributions to radio technology and the understanding of radio science.  This work must be continued today, as Part 97 of the FCC rules states that a primary purpose of the amateur radio service is the “Continuation and extension of the amateur's proven ability to contribute to the advancement of the radio art.”  Recent advances in the fields of computing, software defined radio, and signal processing provide unprecedented opportunities to meet this mandate, specifically in the field of radio science.  These opportunities are already beginning to be realized with the advent of systems such as the Reverse Beacon Network (RBN), the Weak Signal Propagation Reporting Network (WSPRNet), and PSKReporter.  In addition, enabling amateurs to make and contribute legitimate scientific observations will expose amateur radio to a wider community of people interested in science around the world.

What is HamSCI?

HamSCI, the Ham Radio Science Citizen Investigation, is a platform for the publicity and promotion of projects that are consistent with the following objectives:

• Advance scientific research and understanding through amateur radio activities.
• Encourage the development of new technologies to support this research.
• Provide educational opportunities for the amateur community and the general public.

HamSCI serves as a means for fostering collaborations between professional researchers and amateur radio operators. It assists in developing and maintaining standards and agreements between all people and organizations involved.

What is HamSCI's scientific focus?

HamSCI was started by ham-scientists who study upper atmospheric and space physics. These scientists recognized that projects such as the Reverse Beacon Network, WSPRNet, PSKReporter, DX Cluster, ClubLog, and more are generating big data sets that could provide useful observations of the Earth's ionosphere and related systems. Because of this, HamSCI's initial focus is on these fields of research. In the future, other researchers may join HamSCI and broaden its scope. For scientists, working with the amateur radio community is a way to access individually managed stations, available by the hundreds in dozens of countries, with receive and transmit capabilities across the electromagnetic spectrum, easily identified in areas of interest and deployed to remote locations, for free. You can read more about the utility of amateur radio as a teaching tool in this Eos article. 

Science Questions

• How does the ionosphere respond to inputs from space and from the neutral atmosphere?
• How does the ionosphere couple with the neutral atmosphere and with space?
• What are the sources of medium and large scale traveling ionospheric disturbances?
• What are the causes of Sporadic E?

Amateur Radio Questions

• How do disturbances such as solar flares, geomagnetic storms, and traveling ionospheric disturbances affect radio wave propagation?
• How does ionospheric science help amateur radio operators improve communications?
• How can I use my existing radio equipment to science initiatives?

What is a ham radio operator?

HamSCI is driven by data generated by the activities of ham radio operators (a.k.a. amateur radio operators). Ham radio operators are people who are interested in using radio as a hobby and have obtained a ham radio license from their state government. Ham radio is a very diverse hobby. Some operators enjoy talking to friends accross town, while others work to build stations that can communicate around the world. Ham radio operators can help with emergency communications and public service, or even help advance the boundaries of scientific knowledge.

Any interested person can become a ham radio operator. Amateur radio can introduce young people to an exciting career in the field of science and technology, or it can simply serve as a fun and productive hobby for anyone who would like to get involved. The American Radio Relay League is a great place to learn about how to become a ham radio operator.

Operating

One of the simplest ways to participate in HamSCI is simply to get on the radio! This is especially true if you enjoy operating HF CW or digital modes. Systems such as the Reverse Beacon Network, WSPRNet, and PSKReporter will automatically hear your transmissions and report back to their respective databases.

Participate in Receiving Networks

HamSCI scientists rely on data from systems such as the Reverse Beacon Network, WSPRNet, and PSKReporter. These systems rely on volunteers to install and operate receiving stations. Dense receiver coverage is needed globally, so installing a receiving node for one of these stations is a great way to help out!

Follow the ARRL: QST (Official Journal), QEX (Experimenter's Journal) and On the Air (new ham's magazine)

Learn more about ham radio operating by visiting the American Radio Relay League website.  Become an ARRL member to receive QST, along with the League's other publications.

To properly spec an oscillator, we need to establish several parameters. So we'll all be on the same page, I've outlined below the main ones.

[To the many of you who know more about this subject than I do, please forgive any oversimplification or bad examples!]

There are about five and one half specifications that define the performance of an oscillator in the frequency domain:

Accuracy

How close is the frequency or clock readout to an external reference (cesium frequency standard, or UTC time scale)?  This is a single number specified as a ratio (e.g., parts per billion) or as an absolute (e.g., +/- 0.001 Hz, or +/- 10 nanoseconds).

Short Term Stability

How much does the oscillator's frequency wobble around during measurement intervals of interest?  Short term stability is important for time interval measurements, where in effect it provides error bars around the measurement.

"Short term" doesn't have a specific cutoff, but it's usually thought of as measurement intervals of a day or less.  Short term stability is stated at a specific interval by a statistic called Allan Deviation. The measurement interval is called "tau" and saying "tau=10 seconds" means each reading is taken ten seconds apart).

Long Term Stability

How constant is the oscillator's frequency over periods of days, weeks, or longer?  Long term stability has two main components: drift, or aging, and flicker noise floor.  Most oscillators exhibit drift, or aging -- a gradual change of rate over ong time periods.  All crystal and rubidium oscillators drift; cesium beam standards do not.  Long term stability is usually considered to include averaging times of a day or more.  It is also stated as Allan Deviation, and where appropriate by an aging rate, such as "1x10e-10/day".  The flicker noise floor is usually masked by drift, but is apparent in measurements of cesium beam frequency standards because they do not drift, but even then it only shows up at tau of several hundred thousand seconds.

Allan Deviation

I mentioned Allan Deviation above.  What is it?  ADEV is a statistic similar to standard deviation but modified to better reflect the noise types exhibited by oscillators.  It is dimensionless and is usually stated in the form "2.5 x 10e-8".  Smaller is better!  ADEV varies with measurement interval ("tau"), and is often plotted on a log-log graph with stability on the Y axis (lower is better) and tau on the X axis.  From the slope of the curve, one can determine the noise processes at work n each segment of the graph.

Drift is apparent in ADEV graphs by a "bathtub" shaped curve where stability improves out to a few hundred or thousand seconds, flattens for a bit, and then goes up at longer averages as the drift becomes apparent.  I've attached a sample ADEV graph so you can see what they look like.

Temperature Stability ("tempco")

Every resonator is a thermometer, and one of the challenges in crystal oscillator design is to prevent temperature changes from impacting the oscillation frequency.  This is why we have TCXOs (temperature compensated crystal oscillator) and OCXOs (oven controlled crystal oscillator).  Tempco is usually specified as parts per degree over a temperature range.

Phase Noise

How much unwanted phase modulation does the oscillator output carry? This is an important specification in RF systems because excessive phase noise increases the noise floor and impairs signal recovery by the receiver.  On the transmit side, broadband phase noise can cause interference to nearby receivers.

Phase noise is specified as dB down from the carrier (dBc) of the single sideband noise, normalized to 1 Hz bandwidth, at a given offset from the carrier -- e.g., 130 dBc/Hz @ 1 kHz offset.  It is often plotted on a log-log graph.  Various noise processes are shown by the slope of the PN plot.  Most oscillators have a PN curve that drops at slope 1 to 2 from the carrier out to some point where the noise floor is reached and the PN remains constant from that offset outward.  The closest offset usually measured is between 1 and 100 Hz, depending on the quality of the oscillator, and in the HF/VHF range region is usually measured out to 100 kHz or 1 MHz offset.Phase noise is really a short term stability at very short tau, and you can derive phase noise from an ADEV graph.  PN is usually used for offsets of more than 1 Hz (which equals tau of 1 second), and ADEV for longer tau.  I've also attached a sample phase noise graph.

Fun fact: phase noise increases by a minimum of 20log(N) with frequency multiplication.  Double the frequency, increase the PN by 6 dB; multiply by 10 and add 20 dB to the noise.  This is why phase noise is a major hassle in microwave systems.

Jitter

This is the 1/2 parameter mentioned above, because it is a different way of defining phase noise.  It tries to reduce to one number the noise performance of an oscillator across a wide range of offset frequencies. Jitter is widely used in telecom clock specifications and is usually specified in femtoseconds or picoseconds of bit edge displacement.  It's really another way of describing phase noise, and can be calculated from a phase noise plot.  The gotcha is that you need to know the bandwidth over which the phase noise is integrated, and that's often not clearly stated in the data sheet.

Page Courtesy of John Ackermann N8UR

This is a how to page for Gqrx an "open source software defined radio receiver".  Gqrx has many bells and whistles, one of which is the ability to listen to "raw" IQ files, speficially, "raw" IQ files from RRI.  This page is desinged to help set-up and listen to "raw" RRI IQ files using Gqrx.

Currenlty, Gqrx is available for Linux, and some instances of Mac OS.  Information about that can be found here.  This instructions and screen captures shown here are from Ubutu 18.04 LTS.  These instructions will be very similar - if not identical - for a Mac Gqrx install.  Gqrx may be downloaded directrly from the site, or it may be installed through the normal Linux APT software.  Gqrx user support is provided via a Gqrx Google group.

As you will see, Gqrx has lots of options and settings.  Here we are only concerned with playing "raw" I/Q files assoicated with RRI's dataset.

Gqrx Startup

When starting up Gqrx (assuming that your install went smoothly) you should see something similar to the following screen-grab.

Receiver settings

The raw I/Q files do not contain any metadata. RRI's settings related to the data file must be manually entered into Gqrx.  To do this, click on Configure I/O devices icon on the left side of the toolbar at the top of the window, as shown (the incon looks like a piece of computer hardware).  Then enter the important information contained in the file name of the RRI raw file into the Configure I/O devices window.  For example, here we have entered information for an RRI data file that was recorded at 7.025 MHz.  Under Device String, the field freq=7025e3 (7025 kHz = 7.025 MHz) and rate=625e2 (625E2 Hz = 62.5 kHz) are the only fields that have been changed.  Under LNB LO enter the tuned frequency RRI was at, in this example LNB LO = 7.025000 MHz.  Ensure the Audio Output settings are correct so that you'll be able to hear the audio.

Selecting an RRI raw IQ file to play

Next, to load up an RRI raw IQ file, click on the Record and play I/Q data icon on the top toolbar (the icon looks liek a screen with a voltage trace).  In the Record and play I/Q data window, be sure to set your path to the audio file correctly.  When this is done, you see all of the files in the *.raw format.  You will then be able to select the file you want to play.

Playing an RRI raw IQ file

To play the selected file, hit Play in the I/Q recording and replay tool.  Ensure that Mode in the Receiver Options panel to the right is set on Raw I/Q.  Then select the Start DSP processing icon in the top toolbar (the icon looks like a traditional 'play' button).  The raw IQ audio file should start playing.  You should see a waterfall plot similar to the one shown below.  Notice that the  I/Q recording and replay tool has a timer and a slider which allows you to locate and reposition your place in the audio file.

If you have any comments, questions, or suggestions, please do not hesitate to contact Gareth Perry

Main workshop page: http://hamsci.org/hamsci2019

2019 HamSCI Workshop Report [PDF]

Friday, March 22, 2019

Saturday, March 23, 2019

Papers Submitted But Not Presented

2027 HamSCI Workshop

April 17-18, 2027 at The University of Scranton in Scranton, PA

April is Global Citizen Science Month and April 18 is World Amateur Radio Day!

HamSCI Science Telecons

There are currently three regularly scheduled telecons to support HamSCI work. All are open to the public, please see the calendar confirm teleconference times and view conference call connection information. Please visit the Get Involved page for the current telecon schedule.

Archival recordings of HamSCI and TangerineSDR telecons are available here.

Past Meetings

HamSCI Workshops

• HamSCI 2026 (Hybrid - ARRL/Central Connecticut State University, New Britain, CT)
• HamSCI 2025 (Hybrid - New Jersey Institute of Technology, K2MFF, Newark, NJ)
• HamSCI 2024 (Hybrid - Case Western Reserve University, W8EDU, Cleveland, OH)
• HamSCI 2023 (Hybrid - University of Scranton, W3USR, Scranton, PA)
• HamSCI 2022 (Hybrid - US Space and Rocket Center, Huntsville, AL)
• HamSCI 2021 (Virtual - The University of Scranton, W3USR, Scranton, PA)
• HamSCI 2020 (Virtual - The University of Scranton, W3USR, Scranton, PA)
• HamSCI 2019 (Case Western Reserve University, W8EDU, Clevland, OH)
• HamSCI 2018 (NJIT, K2MFF, Newark, NJ)
  • Logistics
  • Presentations
  • CQ Magazine Meeting Summary (Copyright CQ Communications, Inc., Posted by permission.)
• HamSCI-UK 2017 (Milton Keynes, UK)

Dayton Hamvention

• Hamvention 2019 (Xenia, OH)
• Hamvention 2018 (Xenia, OH)
• Hamvention 2017 (Dayton, OH)

ARRL-TAPR Digital Communicatons Conference

• DCC 2019 (Detroit, MI)
• DCC 2018 (Albuquerque, NM)
• DCC 2017 (St. Louis, MO)

American Geophysical Union Meeting

• Fall AGU 2019 (San Francisco, CA)
• Fall AGU 2018 (Washington, DC)
• Fall AGU 2016 (San Francisco, CA)