Surf Wiki
Save to docs
science/astronomy

From Surf Wiki (app.surf) — the open knowledge base

3C 58

Supernova remnant in the constellation of Cassiopeia

Supernova remnant in the constellation of Cassiopeia

Cassiopeia}} 3C 58 or 3C58 is a pulsar (designation PSR J0205+6449) and supernova remnant (pulsar wind nebula) within the Milky Way. The object is listed as No. 58 in the Third Cambridge Catalogue of Radio Sources.

It is located 2° northeast of ε Cassiopeiae and is estimated to be 10,000 light-years away. Its rotation period is 65.7 ms (so PSR J0205+6449 does not belong to the class of millisecond pulsars).

The pulsar is notable for its very high rate of cooling, which is unexplained by standard models 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 so that the star cools. 3C 58 has been proposed as a possible quark star (or strange star).

The age of the 3C 58 remnant has been measured by a number of independent methods. The proper motion of the expanding optical shell of 3C 58 has been measured three times, always with an indicated age of around 3500 years, with this being the direct and distance-independent measure.{{cite journal Estimates from the expansion measurements of the filamentary structure in the radio of the synchrotron nebula suggest the age to roughly 7000 years, independent of distance. Several methods for estimating the remnant's age have proven to have such a large uncertainty as to not be useful, with these methods including those involving the pulsar energetics, the swept-up mass, the pulsar offset from the center of 3C 58, and the changing of the nebular radio brightness.{{cite journal The spin-down age of the pulsar is 5380 years, while the cooling age of the neutron star is 5000 years. Taking all available evidence, 3C 58 has an age somewhere from 3500 to 5500 years.

From 1971 to 2021, 3C 58 has been speculatively connected to the Supernova of 1181 AD, as reported by Chinese and Japanese observers.{{cite journal So 3C 58 is not the remnant left behind by the 1181 supernova.

References

References

  1. {{cite constellation. 3C 58
  2. (1997). "The Westerbork Northern Sky Survey (WENSS), I. A 570 square degree Mini-Survey around the North Ecliptic Pole". Astronomy and Astrophysics Supplement Series.
  3. (2002). "The cooling neutron star in 3C 58". Astronomy & Astrophysics.
  4. (14 December 2004). "Chandra :: Photo Album :: 3C58". Chandra.harvard.edu.
  5. Cramer, John G.. (November 2002). "Quark Stars". Analog Science Fiction & Fact Magazine.
  6. "RX J1856.5-3754 (and the 3C58 Pulsar)".
  7. Bietenholz, M. F.. (October 2025). "Radio Images of 3C 58: Expansion and Motion of Its Wisp". The Astrophysical Journal.
  8. Schaefer, Bradley E.. (2023-08-01). "The path from the Chinese and Japanese observations of supernova 1181 AD, to a Type Iax supernova, to the merger of CO and ONe white dwarfs". Monthly Notices of the Royal Astronomical Society.
  9. (2023-01-11). "Discovery of an Exceptional Optical Nebulosity in the Suspected Galactic SN Iax Remnant Pa 30 Linked to the Historical Guest Star of 1181 CE". The Astrophysical Journal Letters.
Info: Wikipedia Source

This article was imported from Wikipedia and is available under the Creative Commons Attribution-ShareAlike 4.0 License. Content has been adapted to SurfDoc format. Original contributors can be found on the article history page.

quark-stars pulsars 3c-objects cassiopeia-(constellation)
Want to explore this topic further?

Ask Mako anything about 3C 58 — get instant answers, deeper analysis, and related topics.

Research with Mako

Free with your Surf account

Content sourced from Wikipedia, available under CC BY-SA 4.0.

This content may have been generated or modified by AI. CloudSurf Software LLC is not responsible for the accuracy, completeness, or reliability of AI-generated content. Always verify important information from primary sources.

Report