PSR J1946+2052

[3]: 5784  The general theory of relativity predicts their orbits are gradually decaying due to emitting gravitational waves, which will eventually lead to a neutron star merger and a kilonova in 46 million years.

[2]: 4–5  It is unlikely in the near future that PSR J1946+2052's distance could be determined more precisely with direct methods such as very-long-baseline interferometry or hydrogen line absorption, as it is too faint and distant.

On the other hand, the first-born pulsar is expected to continue pulsating for billions of years thanks to the high angular momentum it had acquired from accretion.

This is potentially the lowest mass measured for a double neutron star system as of 2022[update], though it could be tied with PSR J1411+2551 (2.538±0.022 M☉) within uncertainty bounds.

This is a relatively low spin-down rate for a neutron star, which suggests the pulsar must have a weakened surface magnetic field strength of 4×109 gauss (4.0×105 T).

The pulsar is estimated to have a characteristic age of 290 million years, assuming it only experienced constant spin-down to its present rotation period.

[2]: 4–5  The orbital decay rate will progressively increase in magnitude as the components spiral closer to each other, and will lead to a neutron star merger in 46 million years.

[7]: 19, 23  Up to 0.1 M☉ of these heavy elements are predicted to be ejected outward at about 0.1 times the speed of light, due to the extreme angular momentum and heating involved in the merger.

[7]: 13  Over time, these ejected heavy elements undergo radioactive decay and produce electromagnetic radiation from infrared to ultraviolet wavelengths, generating a kilonova.

[7]: 23  The low total mass of the PSR J1946+2052 merger will likely form a strongly magnetized supramassive neutron star remnant that slightly exceeds the 2.1–2.4 M☉ Tolman–Oppenheimer–Volkoff limit.