PSR B0950+08

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]

PSR B0950+08

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]

External links

• New Scientist, August 24, 2002
• Image PSR B0950+08