PSR B0950+08
Radio pulsar in the constellation Leo
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PSR B0950+08 is a young pulsar that may have come from a supernova that occurred in the Constellation of Leo 1.8 million years ago. Off-pulse emissions from the young pulsar were detected by the Expanded Long Wavelength Array, suggesting the presence of a pulsar wind nebula around it.[3]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Leo |
| Right ascension | 09h 53m 09.310s |
| Declination | +07° 55′ 35.75″ |
| Characteristics | |
| Spectral type | Pulsar |
| Apparent magnitude (B) | 27.07(16)[1] |
| Astrometry | |
| Proper motion (μ) | RA: −2.09 mas/yr Dec.: 29.46 mas/yr |
| Parallax (π) | 3.82±0.07 mas |
| Distance | 850 ± 20 ly (262 ± 5 pc) |
| Details | |
| Rotation | 0.2530654277593 s |
| Age | 1.8 Myr |
| Other designations | |
| PSR J0953+0755, NVSS J095309+075536, PULS CP 0950, GAL 228.9+43.7, PSR B0950+08.[2] | |
| Database references | |
| SIMBAD | data |
PSR B0950+08 was fourth among the initial radio pulsars discovered in 1968.[1] It completes rotation every 0.253 seconds.
It was postulated in 2002 to be related to the Antlia Supernova Remnant,[4] but a 2021 study estimates the age of the remnant to be less than 100,000 years.[5]
