From AAS NOVA : “Reweighing A Heavy Neutron Star”



16 August 2021
Susanna Kohler

Artist’s impression of how the pulses emitted by the pulsar PSR J0740+6620 are affected by the gravity of its white-dwarf companion. Credit: B. Saxton/National Radio Astronomy Observatory (US)/Associated Universities Inc (US)

What does the inside of a neutron star — the incredibly dense remnant of an evolved star — look like? New observations of one of the most massive neutron stars provide some clues.

Mysterious Interior

With the mass of multiple Suns packed into the rough size of a city, neutron stars represent one of the most dense, exotic environments in the universe. We can’t create an equivalent environment on Earth, so we rely on theoretical models — constrained by observations — to understand how matter behaves under these extreme circumstances.

Different theoretical models predict different interior structures for neutron stars, each described by an equation of state. In turn, each equation of state predicts a different maximum mass that a neutron star can reach before the overwhelming crush of gravity causes it to collapse into a black hole.

The heaviest neutron stars we spot in the universe, then, can help us to set upper limits and rule out some equations of state, narrowing down which models of neutron star interiors are most likely.

The catch? Measuring the precise masses of objects located thousands of light-years away is difficult! Luckily, the universe occasionally offers up clever tricks for doing so.

A Delay from Gravity

Some highly magnetized neutron stars emit beams of light that regularly pulse across our line of sight as they rotate. If these incredibly precise cosmic clocks — pulsars — have a binary companion, and if we view that binary edge-on, then we have a unique opportunity for some mass measurements.

Dame Susan Jocelyn Bell Burnell, discovered pulsars with radio astronomy. Jocelyn Bell at the Mullard Radio Astronomy Observatory, University of Cambridge(UK), taken for the Daily Herald newspaper in 1968. Denied the Nobel.

In such a system, the distortion of spacetime caused by the gravity of the companion object can affect the signal of the pulsar, such that the pulses arrive at Earth at slightly offset times. This effect, known as the Shapiro time delay, allows us to precisely measure the companion’s mass — which can then be used with the binary orbit to establish the pulsar’s mass.

In a recent study, a team of scientists led by Emmanuel Fonseca (McGill University (CA); West Virginia University (US)) have now used this approach with new observations of the pulsar PSR J0740+6620 to place the tightest constraints on its mass yet — and it’s a doozy.

Tipping the Scales

Fonseca and collaborators use observations from the 100-m Green Bank Telescope and the Canadian Hydrogen Intensity Mapping Experiment (CHIME) telescope to carefully model the Shapiro delay and measure the properties of PSR J0740+6620 and its companion, significantly improving upon previous measurements.

Green Bank Radio Telescope, West Virginia, USA, now the center piece of the Green Bank Observatory(US), being cut loose by the National Science Foundation(US), supported by Breakthrough Listen Project, West Virginia University, and operated by the nonprofit Associated Universities, Inc..

The authors show that PSR J0740+6620 weighs in at 2.01–2.15 solar masses — confirming its status as the heaviest precisely measured neutron star currently known. They also confirm that the binary lies ~3,700 light-years away, and that the companion is an unusually cold white dwarf of just 0.25 solar mass.

Even more precise constraints — both on PSR J0740+6620 and other high-mass neutron stars — will be enabled by ongoing observations with currently technology, and by future studies using next-generation telescopes. Each improvement brings us a little closer to understanding the matter in these extreme objects.


“Refined Mass and Geometric Measurements of the High-mass PSR J0740+6620,” E. Fonseca et al 2021 ApJL 915 L12.

See the full article here .


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