Understanding Meteor Scatter

Meteor scatter (or meteor burst) communication relies on the ionized trails left by meteors entering the Earth's atmosphere. When a meteor burns up, it leaves a trail of ionized gas that can often be seen as a bright streak across the sky. The ionized gas trail can reflect VHF and UHF radio signals, allowing for brief communication windows over distances (typically 600 to 2,000 km) that are usually beyond line-of-sight.

Amateur operators will often take advantage of meteor showers that provide more opportunities. Digital modes are usually used because of their superior efficiency and speed during the brief window of an ionization trail event.

Key Components for Success

• Antennas: High-gain directional antennas (like Yagis) are preferred to focus signal energy and maximize sensitivity.
• Transceivers: Modern VHF/UHF transceivers capable of stable frequency operation are essential.
• Software: The WSJT-X software suite, particularly the MSK144 mode, has revolutionized meteor scatter, making it possible to complete contacts in seconds during the brief windows when a trail is active.
• Time Synchronization: Precise timing via GPS or internet time sync is critical, as modes like MSK144 operate on strictly synchronized time sequences.

How Are Meteor Trails Spotted?

The operator monitors a distant CW radio beacon transmission. Because it is over the horizon, nothing can be heard. Often a brief chirp sound or "ping" will be heard as a meteor travels through the atmosphere and the beacon may be heard as it's reflected off the ionization tail.
Meanwhile a transceiver is continuously transmitting data packets to be reflected by the meteor's ionized trail to a distant station over the horizon. A listening station that receives and decodes the packet will immediately transmit a response which will (hopefully) be reflected back to the sending station.
This exchange takes place in the span of less than 30 seconds.