PSR B0950+08
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Template:Short description Template:Needs more references
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Leo |
| Right ascension | Template:RA |
| Declination | Template:DEC |
| Characteristics | |
| Apparent magnitude (B) | Template:Val[1] |
| Variable type | Pulsar |
| Astrometry | |
| Proper motion (μ) | RA: −2.09 mas/yr Dec.: 29.46 mas/yr |
| Parallax (π) | 3.82±0.07 mas |
| Distance | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Details | |
| Age | 1.8 million years |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| PSR J0953+0755, NVSS J095309+075536, PULS CP 0950, GAL 228.9+43.7, PSR B0950+08.[2] | |
| Database references | |
| SIMBAD | data |
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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. The large and old remnant of this supernova, located in the constellation of Antlia, may be the nearest besides the Local Bubble, and the supernova would have been as bright as the moon. 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]
PSR B0950+08 was fourth among the initial radio pulsars discovered in 1968.[1]
External links
- The Astrophysical Journal Letters, vol. 576, p. L41, August 2002
- New Scientist, August 24, 2002
- Image PSR B0950+08
- [1]