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3C58 or 3C 58 is a pulsar and supernova remnant within the Milky Way that is possibly associated with the supernova SN 1181. There are, however, signs that indicate that it could be several thousand years old, and thus not associated with that supernova.[2]

3C 58
X-Ray image of 3C58 by Chandra X-Ray Observatory.
The pullout box shows the inner toroidal-shaped nebula
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cassiopeia
Right ascension  02h 05m 38s
Declination +64° 49.7′
Apparent magnitude (V) 8.17
Spectral type III[1]
Distance10,000 ly
(3067.48 pc)
Absolute magnitude (MV)3.70
Mass1.36–1.52[1] M
Temperature150,000[1] K
Other designations
SNR G130.7+03.1, ASB 5, RX J0201.8+6435, PSR J0205+6449[1]
Database references

3C58 is notable for its very high rate of cooling which is unexplained by standard theories of neutron star formation. It is hypothesized that extreme conditions in the star's interior cause a high neutrino flux, which carries away the energy and the star cools.[3][1]

It is located in the direction of Cassiopeia and is estimated to be 10,000 light-years away. Its rotation period is about 11 seconds.

3C58 has been proposed as a possible quark star.[4][5]


  1. ^ a b c d e
  2. ^ Bietenholz, M. F. (1 July 2006). "Radio Images of 3C 58: Expansion and Motion of Its Wisp". The Astrophysical Journal. 645: 1180–1187. arXiv:astro-ph/0603197. Bibcode:2006ApJ...645.1180B. doi:10.1086/504584. ISSN 0004-637X.
  3. ^ "Chandra :: Photo Album :: 3C58". 14 December 2004. Retrieved 21 August 2012.
  4. ^ Cramer, John G. (November 2002). "Quark Stars". Analog Science Fiction & Fact Magazine. Retrieved 17 August 2015.
  5. ^ "RX J1856.5-3754 and 3C58 Pulsar". Retrieved 18 August 2015.

External linksEdit

  Media related to 3C 58 at Wikimedia Commons

Coordinates:   02h 05m 38.29s, +64° 49′ 44.4″