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Clear out junk files and repair common Windows errorsFree Scan →Scan for outdated or missing drivers - takes under a minuteDriver Scan →Repair Windows errors before they cause bigger problemsFix Now →A pulsar can capture gas lost by a companion star or receive gas transferred through a close binary system. The captured material falls toward the neutron star, heats up and can emit X-rays; its magnetic field may channel some of it onto hot regions near the magnetic poles. The pulsar’s rotation makes those regions appear to pulse as they sweep into view. This process, called accretion, can also gradually spin the neutron star faster—but it does not mean the companion is swallowed whole.
What “feeding” means in a pulsar binary
A pulsar is a rapidly rotating, strongly magnetized neutron star. Its radiation beams sweep through space as it turns, so an observer sees pulses when a beam crosses the line of sight; the star is not switching on and off. NASA’s HEASARC introduction to pulsars explains this lighthouse-like effect.
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In a binary, the companion can supply gas that the neutron star captures or that flows toward it. Gas captured and falling toward a compact object is undergoing accretion. It may orbit the neutron star, heat up, form or disrupt a disk, and some of it may never reach the surface. “Feeding” is shorthand for this transfer of material, not the consumption of an entire star.
How gas reaches the neutron star
Wind capture
Some massive stars shed gas in a stellar wind. A neutron star orbiting one can capture part of that outflow. The amount and timing depend on the wind and the binary’s geometry; a wind-fed system does not necessarily have a steady, orderly disk.
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Transfer through a close binary
In a close system, gas from a companion can flow toward the neutron star and collect into an accretion disk. The disk’s formation and behavior depend on the incoming flow and its angular momentum. This channel differs from capturing gas streaming out in a stellar wind.
What happens to the captured gas
- Gravity pulls it inward. The gas moves through the neutron star’s intense gravitational field, releasing energy and heating up.
- The hot material radiates. Accreting gas can produce X-rays, which space telescopes can detect. NASA’s NuSTAR animation illustrates how an accretion disk and magnetic field can shape this emission.
- Magnetic fields guide some of the flow. Close to the neutron star, its magnetic field can funnel infalling gas toward hot regions near the magnetic poles.
- Rotation makes the X-ray signal pulse. As the star turns, the hot regions move across the observer’s view. A telescope detects changing X-ray brightness, even though the neutron star keeps rotating continuously.
The neutron star’s rotation, its orbit around the companion, and the motion of gas in a disk are different motions. The pulses arise from the rotating star and the changing view of its emitting regions—not simply from the companion’s orbit or a disk revolving around the neutron star.
Two systems show different feeding routes
| System | Gas supply | What observers see |
|---|---|---|
| BP Crucis (GX 301-2 and Wray 977) | GX 301-2 captures gas from the wind of Wray 977, a blue hypergiant; NASA’s 2026 account also describes a denser stream. | NASA reported X-ray flares as the pulsar passes through dense parts of the stream. Its orbit is 41.5 days, and the system is about 13,000 light-years away, according to NASA’s September 18, 2026 report. |
| IGR J17062–6143 | Material from its white-dwarf companion collects into a disk around an accreting millisecond X-ray pulsar. | NASA’s 2018 report gives the binary orbit as 38 minutes and describes hot spots where material reaches the neutron star. NASA called this a record-fast orbit for a binary containing an accreting millisecond X-ray pulsar at the time; that report does not establish it as today’s record. |
NASA reported on September 18, 2026, that Japan-led XRISM observed BP Crucis with its Resolve spectrometer. The observations were taken February 1, 2025. NASA’s account describes a turbulent disk forming, breaking up when the flow lacks enough angular momentum to sustain it, and later rebuilding with the opposite rotation direction. That sequence describes this system and observation, not a universal stage in pulsar accretion. Roi Rahin, a researcher at the University of Maryland, Baltimore County and NASA’s Goddard Space Flight Center, said: “We’ve never before seen clear indications of wind plasma falling onto a compact object.”
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Gas flowing toward a neutron star can transfer angular momentum as well as energy. Over a long period, accretion can spin a neutron star up, helping explain how some systems produce millisecond pulsars. The European Space Agency’s account of IGR J00291+5934 describes companion gas fueling a fast pulsar’s acceleration and presents such binaries as part of an evolutionary path toward faster-spinning pulsars. This is a possible route, not a guaranteed outcome for every binary.
Independent reader supportYour contribution helps us test, update, and keep practical guides available for everyone.Why a pulsar may stop feeding
Some systems change between accretion-related X-ray behavior and radio-pulsar behavior. NASA’s Fermi account of PSR J1023+0038 describes an earlier low-mass X-ray binary phase, when gas transfer produced X-ray pulses from hot gas, followed by a millisecond radio-pulsar state after mass transfer stopped. A pulsar therefore need not be accreting continuously; its observed state can change as the flow from its companion changes.
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