A pulsar-helium star compact binary system formed by common envelope evolution

A stellar common envelope occurs in a binary system when the atmosphere of an evolving star expands to encompass an orbiting companion object. Such systems are predicted to evolve rapidly, ejecting the stellar envelope and leaving the companion in a tighter orbit around a stripped star. We use radio timing to identify a pulsar, PSR J1928+1815, with a spin period of 10.55 ms in a compact binary system with an orbital period of 3.60 hours. The companion star has 1.0 to 1.6 solar masses and eclipses the pulsar for about 17% of the orbit, so is most likely a stripped helium star but is undetected at other wavelengths. We interpret this system as having recently undergone a common envelope phase, producing a compact binary., , # Data from: A pulsar-helium star compact binary system formed by common envelope evolution

Dataset DOI: [10.5061/dryad.f1vhhmh6z](10.5061/dryad.f1vhhmh6z)

## Description of the data and file structure

Processed FAST data of PSR J1928+1815, a binary pulsar discovered in FAST GPPS survey.

### Files and variables

#### File: yhz25dat.tar.gz

**Description:** Processed FAST data of PSR J1928+1815, a binary pulsar discovered in FAST GPPS survey.

1\) Folded pulsar profiles of PSR J1928+1815. These profiles have a bin number of 128 a sub-bint integration time is 300 s and 4 frequency channels. The radio frequency range is 1.0 to 1.5 GHz.

2\) We link three observations during which the pulsar was eclipsed to the 'nodect' folder .

3\) The sum polarization profile is in 'sum_profile' folder.

4\) The ephemeris and TOAs of PSR J1928+1815 is in 'timing' folder.

## Code/software

The code used for view the data is PSRCHIVE package ([https://psrchive.sourceforge.net/](https://psrchive.source...,