Hostname: page-component-745bb68f8f-l4dxg Total loading time: 0 Render date: 2025-01-13T19:54:41.411Z Has data issue: false hasContentIssue false
  • English
  • Français

High Resolution X-ray Observations of 3C 58

Published online by Cambridge University Press:  19 July 2016

Patrick Slane
Patrick Slane*
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

As the presumed remnant of SN 1181, 3C 58 houses one of the youngest known neutron stars in the Galaxy. The properties of this young pulsar and its associated pulsar wind nebula (PWN) differ considerably from those of the Crab Nebula, and may well offer a more typical example of the endpoint of massive star collapse. High resolution X-ray studies reveal structures in the inner nebula that may be associated with the pulsar wind termination shock, a jet that may be aligned with the rotation axis, and other regions of enhanced emission. Spectral variations in the PWN are consistent with the expected evolution of the postshock flow, and complex loops of emission are seen in the nebula interior. Limits on the neutron star surface temperature fall below standard cooling models, indicating that some more rapid neutrino cooling process is required. The outer regions of 3C 58 show thermal emission with enhanced levels of neon, indicative of shocked ejecta bounding the PWN.

Type
Part 4: Pulsar Wind Nebulae and Their Environments
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 185 - 188
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Begelman, M. C., & Li, Z.-Y. 1992, ApJ, 397, 187.Google Scholar
Bocchino, F. et al. 2001, A&A, 369, 1078.Google Scholar
Chevalier, R. A. 2004, Adv. Sp. Res., 33, 456.CrossRefGoogle Scholar
Frail, D. A., & Moffett, D. A. 1993, ApJ, 408, 637.Google Scholar
Murray, S. S. et al. 2002, 568, 226.Google Scholar
Slane, P., Helfand, D. J., & Murray, S. S. 2002, ApJ, 571, L45.Google Scholar
Torii, K. et al. 2000, PASJ, 52, 875.Google Scholar
Tsuruta, S. et al. 2002, ApJ, 571, L143.Google Scholar
van der Swaluw, E. 2003, A&A, 404, 939.Google Scholar
Yakovlev, D. G. et al. 2002, A&A, 389, L24.Google Scholar