G11.2-0.3 the Remnant of SN 386 AD: Is it too good to be true?

Details G11.2-0.3 the Remnant of SN 386 AD: Is it too good to be true? G11.2-0.3 the Remnant of SN 386 AD: Is it too good to be true?

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprk11005r&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

1616 years ago, a guest star was observed by the Chinese in the southern sky. The composite SNR G11.2-0.3, consisting of a spherical shell, central 65ms X-ray pulsar and pulsar wind nebula (PWN), is the likely result. Expansion measurements of the radio shell put strong age constraints on the remnant consistent with a birthdate of 386AD. The inferred initial spin period of the pulsar (P0 62ms) suggests a simple approximation of constant energy input into the PWN is, for once, reasonable. We combine data from the VLA and Chandra to infer a variety of properties of the system. The geometrical simplicty of G11.2-0.3 and the measurable properties of the system components make it an ideal test-bed of models of the early evolution of composite SNRs.

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