Why Pulsars Can't Spin Faster Than a Blender ✛

Original: "Sub-Millisecond Pulsars: Missing or Impossible?"
arXiv:2608.23704v1 · 2026-08-24 · CC BY 4.0 · 1 min
The fastest pulsar spins 716 times per second, but faster is impossible: there's not enough runway.

Imagine a spinning top that you spin up by pouring water on it. To make it spin very fast, you need a lot of water, but if you pour too hard, the water splashes and doesn't hit the top. The same goes for pulsars: they are superdense stars that spin up when matter falls onto them from a companion star. The fastest known pulsar spins 716 times per second — faster than a kitchen blender. But to spin even faster, it would need to accrete a mass equal to a quarter of the Sun. The companion star can't deliver that much matter slowly enough: it's either too light or lives too short.

Even if such an ultra-fast pulsar appeared, it would quickly slow down due to energy loss, like a top that's no longer being spun.

Scientists checked: maybe such pulsars exist but we don't see them? They added thousands of artificial ultra-fast pulsars to telescope data and saw whether the programs would detect them. It turned out that bright ones would definitely be spotted. So they really don't exist, or they disappear too quickly. It's like looking for a record-holder who ran the 100-meter dash in 8 seconds, but finding that such a feat would require a runway longer than the stadium allows.

The fastest known pulsar, PSR J1748-2446ad, spins 716 times per second — faster than a kitchen blender. If it were the size of Earth, a point on its equator would move at about 0.24 times the speed of light.

In Robert Forward's novel "Dragon's Egg," a neutron star spins so fast that creatures live on its surface perceiving time differently. A submillisecond pulsar would be an even more extreme object, but physics shows such stars cannot exist for long.

P_{eq} \simeq 1.40 \, \text{ms} \, B_8^{6/7} \left( \frac{\dot{M}}{0.1 \dot{M}_{\text{Edd}}} \right)^{-3/7} M_{1.4}^{-5/7} R_{13}^{18/7}
The period at which magnetic torque and accretion torque balance; depends on magnetic field, accretion rate, mass, and radius.
\Delta M_{\text{eq}} \simeq 0.22 \, M_\odot \, \frac{(M/M_\odot)^{1/3}}{P_{\text{ms}}^{4/3}}
The mass required to spin up a neutron star to period P_ms; for 1 ms, about 0.25 solar masses is needed.
P_H \simeq 0.0619 \, \text{ms} \, \left( \frac{M}{M_\odot} \right) \frac{1 + \sqrt{1 - a_*^2}}{a_*}
Characteristic timescale of spacetime rotation at the black hole horizon; for 10 solar masses and a*=1 gives 0.6 ms.
Scientists
Enrico FermiPaul DiracSubrahmanyan ChandrasekharMichael FaradayHendrik LorentzAlbert Einstein
Concepts
millisecond pulsar glitch neutron star spin neutron star mass limit pulsar phenomena spin rate x ray pulse ultrashort pulse stellar rotation black hole mass gap pulsation microarcsecond magnetar pulsations in grb kilometer per second microscopic black hole nanosecond oscillation period stellar planetary misalignment magnetar glitch pulsar