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A pulsar can capture gas lost by a companion star or draw material from it in a close binary. The gas falls toward the neutron star, heats up and can shine in X-rays; the star’s magnetic field may funnel it onto hot regions near its poles. As those regions rotate into and out of view, telescopes detect pulses. The process is called accretion, and it does not mean the pulsar swallows its companion whole.
What “feeding” means in a pulsar binary
A pulsar is a rapidly rotating, strongly magnetized neutron star. Its beams of radiation sweep through space, and observers see pulses when a beam points toward Earth. The star is not switching on and off: rotation changes what reaches the observer. NASA’s HEASARC introduction to pulsars explains this lighthouse-like effect.
In a binary, a companion can supply gas that the neutron star captures or that flows toward it. Material captured and falling toward a compact object is undergoing accretion. The gas may orbit the neutron star, form a disk, heat up and emit X-rays. Some of it can reach the neutron star’s surface; some may not. The companion is not necessarily consumed, and a pulsar need not be accreting at all times.
How gas gets from the companion to the neutron star
Wind capture
Some massive stars lose gas in a stellar wind. A neutron star in orbit can capture part of that flowing material. The captured gas carries motion and may form a turbulent disk, but disk formation and behavior depend on the conditions in that particular system.
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BP Crucis is a wind-fed example. In NASA’s report published September 18, 2026, Japan-led XRISM observations of GX 301-2 and its companion, the blue hypergiant Wray 977, showed X-ray flares as the pulsar passed through a denser stream of gas. NASA gives the system’s orbital period as 41.5 days and its distance as about 13,000 light-years. The report describes a disk that formed, broke up when the flow lacked enough angular momentum to sustain it, and later rebuilt with the opposite rotation direction. That sequence describes this system and observation, not a universal pattern for pulsars. NASA researcher Roi Rahin said, “We’ve never before seen clear indications of wind plasma falling onto a compact object.” NASA’s XRISM report on BP Crucis
Transfer in a close binary
In a close binary, gas from the companion can flow toward the neutron star and collect in an accretion disk. NASA’s NICER account of IGR J17062–6143 describes an accreting millisecond X-ray pulsar with a white-dwarf companion. Material forms a disk before reaching the star, where hot spots appear. NASA reported that the binary takes 38 minutes to orbit; it described that as a record-fast orbit for a binary containing an accreting millisecond X-ray pulsar at the time of its 2018 report, not as a current record. NASA’s NICER report on IGR J17062–6143
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What happens as the gas falls inward
- Gravity pulls captured material inward. Depending on the flow, it may travel through a disk or approach the neutron star through another stream of gas.
- The infalling gas heats up. Falling through the neutron star’s intense gravitational field releases energy, which can produce X-rays.
- The magnetic field guides some material. Near the neutron star, its magnetic field can direct gas toward hot regions above the magnetic poles. NASA’s NuSTAR pulsar animation illustrates disk accretion, magnetic funneling and X-ray emission from the hot regions.
- Rotation makes the X-ray signal pulse. The hot regions rotate with the neutron star. Their emission grows brighter to an observer as they turn into view and dims as they turn away. The pulses reflect the changing view, not a change in whether the neutron star exists or rotates.
How accretion can change a pulsar over time
Gas falling onto a neutron star can transfer angular momentum as well as energy. Over time, that transfer can spin the star faster. Accretion is one proposed route to the rapid rotation of millisecond pulsars, but it is a long-term evolutionary process—not a guarantee that every binary pulsar will become one. The European Space Agency’s account of IGR J00291+5934 describes a companion-fed pulsar and the evolutionary link between slower-spinning binary pulsars and faster isolated radio pulsars. ESA: “Star eats companion”
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.Why some pulsars stop accreting—or change state
Feeding can vary or stop when the flow of material changes. In the transitional system PSR J1023+0038, NASA’s Fermi account describes an earlier low-mass X-ray binary phase with X-ray pulses from hot gas, followed by a millisecond radio-pulsar state after mass transfer stopped. This illustrates that accretion-powered X-ray behavior and radio-pulsar behavior can be different states of one system, rather than a single uninterrupted feeding process. NASA Fermi: “NASA’s Fermi Finds a ‘Transformer’ Pulsar
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