A Catalogue of “Guest Stars” Recorded in East Asian History from Earliest Times to a.d. 1600

Stephenson F. R. Green D. A. , Historical supernovae and their remnants (Oxford, 2002); Stephenson F. R. Yau K. K. C. , “Four Korean ‘guest stars’ observed in AD 1592”, Quarterly journal of the Royal Astronomical Society, xxviii (1987), 1987–44.

Yoke Ho Peng Yeong Chiu Ling , Ming shilu zhong zhi tianwen luli (Astronomical records in the veritable history Ming shilu) (Hong Kong, 1986).

Observatory Beijing , Zhongguo gudai tianxiang jilu zongji (A union table of ancient Chinese records of celestial phenomena) (Kiangxu, 1988).

Shigeru Kanda , Nihon temmon shiryo (Japanese historical astronomical data) (Tokyo, 1934).

Yoke Ho Peng , “Ancient and medieval observations of comets and novae in Chinese sources”, Vistas in astronomy, v (1962), 127–225; Zhentao Xu Pankenier D. W. , and Yaotiao Jiang , East Asian archaeoastronomy: Historical records from astronomical observations of China, Japan and Korea (Amsterdam, 2000).

See Stephenson Green , op. cit. (ref. 1).

For a discussion of the angular equivalents of chi and cun, see Stephenson Green , ibid. and Stephenson F. R. , “East-Asian records of the A.D. 1054 supernova”, Astronomical instruments and archives from the Asia-Pacific region, ed. by Orchiston W. (Seoul, 2004), 95–102.

Stephenson Yau , op. cit. (ref. 1); see also Hoffleit D. , “History of the discovery of Mira stars”, The journal of the American Association of Variable Star Observers, xxv (1997), 115–36.

Green D. A. , A catalogue of galactic supernova remnants (2006 April version) (2006; available at http://www.mrao.cam.ac.uk/surveys/snrs/); see also Green D. A. , “Galactic supernova remnants: An updated catalogue and some statistics”, Bulletin of the Astronomical Society of India, xxxii (2004), 2004–70.

Shitong Yi , Qantian xingtu: 2000.0 (All sky star atlas for epoch 2000) (Beijing, 1984); Nai Pan , Zhongguo hengxing guance shi (History of Chinese star observations) (Shanghai, 1989).

Stephenson F. R. , “A suspected supernova in AD 1181”, Quarterly journal of the Royal Astronomical Society, xii (1971), 10–38; Stephenson Green , op. cit. (ref. 1).

See Stephenson Green , op. cit. (ref. 1).

Wang Z.-R. , “Some possible identification between Chinese guest stars and supernova remnants”, Highlights of astronomy, vii (1986), 583–4; Wang Z.-R. , “Ancient guest stars as harbingers of neutron star formation”, The origin and evolution of neutron stars, ed. by Helfand D. J. Huang J.-H. (IAU Symposium 125; Dordrecht, 1987), 305–17.

See Shitong Yi , op. cit. (ref. 10), and Nai Pan , op. cit. (ref. 10).

Wang , opera cit. (ref. 13); Wang Z.-R. Li M. , and Zhao Y. , “Historical evidence for the birth of the newly discovered pulsar PSR J1833–1034”, Chinese journal of astronomy and astrophysics, vi (2006), 625–8.

E.g. Gupta Y. Mitra D. Green D. A. , and Acharyya A. , “The discovery of PSR J1833–1034: The pulsar associated with the supernova remnant G21.5–0.9”, Current science, lxxxix (2005), 853–56.

Yoke Ho Peng , op. cit. (ref. 5).

Ibid.

Ibid.

Stephenson F. R. Green D. A. , “A reappraisal of some proposed historical supernovae”, Journal for the history of astronomy, xxxvi (2005), 217–29.

Shklovsky I. S. , “Identification of the extended source of radio emission close to η Gemini with the nebula remnant of the outburst of nova AD 837”, Doklady Akademii Nauk SSSR, xcvii (1954), 53–55; see also Shajn E. A. Gaze V. F. , “The nebula IC 443 and the new source of radio emission in Gemini”, Doklady Akademii Nauk SSSR, xcvi (1954), 1954–15, and Gaze V. F. Shajn E. A. , “The nebula IC 443 and the source of radio emission in Gemini”, Astronomicheskii Zhurnal, xxxi (1954), 1954–12.

Wang Z. R. , “Hard X-rays from the supernova remnant IC 443”, Publications of the Astronomical Society of Japan, xliv (1992), 303–8.

Keohane J. W. , “A possible site of cosmic ray acceleration in the supernova remnant IC 443”, The astrophysical journal, cccclxxxiv (1997), 350–0, revealed the harder X-ray emission from IC 443 was from the same location as a region of flat spectrum radio emission previously seen ( Green D. A. , “Observations of IC 443 at 151 and 1419 MHz”, Monthly notices of the Royal Astronomical Society, ccxxi (1986), 1986–82) and therefore likely to be due to a pulsar powered nebula within IC 443, and not from unusually fast shocks. This was subsequently confirmed by later observations (e.g. Olbert C. M. , “A bow shock nebula around a compact X-ray source in the supernova remnant IC 443”, The astrophysical journal, dliv (2001), L205–8; Bocchino F. Bykov A. M. , “The plerion nebula in IC 443: The XMM-Newton view”, Astronomy and astrophysics, ccclxxvi (2001), 2001–53), and consequently the age of only about a thousand years for IC 433 deduced by Wang is no longer appropriate. Instead, Olbert estimate an age of about 3 × 10⁴ years for IC 443.

Stephenson F. R. , “Some accurate positions of early Korean ‘guest stars’”, Astrophysical letters, ix (1971), 81–84.

Stephenson , op. cit. (ref. 24).

Ibid.

Shitong Yi , op. cit. (ref. 10).

Nai Pan , op. cit. (ref. 10).

Stephenson Green , op. cit. (ref. 1).

Stephenson Green , op. cit. (ref. 20).