Magnetars, as pictured above in the artist's conception by Robert Mallozzi (UAH/MSFC), are thought to be extremely energetic isolated pulsars with ultra-high magnetic field strengthes (B~10^14 G), and are powered by the decay of their strong magnetic fields. The magnetar model had significant consequences for two classes of neutron star that were previously thought to be unrelated: anomalous X-ray pulsars (AXPs) and soft gamma repeaters (SGRs) are now both considered observable examples of magnetars. The model was introduced by Robert Duncan and Christopher Thompson. Magnetars are the focus of research by McGill Pulsar Group members Fotis Gavriil, Victoria Kaspi, and Cindy Tam, and former member Maxim Lyutikov.

What differentiates magnetars from ordinary radio pulsars? This question is currently under consideration by Marjorie Gonzalez and Victoria Kaspi, who study high magnetic field radio pulsars observed at X-ray wavelengthes. These extreme pulsars are not magnetars: they are powered by rotational spin-down, as oppposed to magnetic field decay. However, a growing class of rotation-powered pulsars exhibit magnetar-like properties, such as high B-fields and slow rotation periods. What, then, is the nature of the relationship between these high-B pulsars and magnetars?