PSR B0950+08 is a young pulsar that may have come from a supernova that occurred in 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
Observation data
Epoch J2000      Equinox J2000
Constellation Leo
Right ascension 09h 53m 09.310s
Declination +07° 55' 35.75"'
Characteristics
Apparent magnitude (B) 27.07(16)[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
Distance850 ± 20 ly
(262 ± 5 pc)
Details
Age1.8 million years
Other designations
PSR J0953+0755, NVSS J095309+075536, PULS CP 0950, GAL 228.9+43.7, PSR B0950+08.[2]
Database references
SIMBADdata

PSR B0950+08 was fourth among the initial radio pulsars discovered in 1968.[1]

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References

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  1. ^ a b Zharikov, S. V.; et al. (2002). "Subaru optical observations of the old pulsar PSR B0950+08". Astronomy & Astrophysics. 394 (2): 633–639. arXiv:astro-ph/0206229. Bibcode:2002A&A...394..633Z. doi:10.1051/0004-6361:20021155.
  2. ^ "PSR B0950+08". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2024-04-19.
  3. ^ Ruan, D. (8 May 2020). "Discovery of a Pulsar Wind Nebula around B0950+08 with the ELWA". Monthly Notices of the Royal Astronomical Society. 495 (2): 2125–2134. arXiv:2005.03303. doi:10.1093/mnras/staa1305. S2CID 218537942.