SN 393 is the modern designation for a probable supernova that was reported by the Chinese in the year 393 CE. An extracted record of this astronomical event was translated into English as follows:
 The Wěi asterism appears in the lower half of the Scorpius constellation | |
| Event type | Supernova  |
|---|---|
| Type II/Ib[1] | |
| Date | 27 February− 28 March 393 22 October− 19 November 393 CE[2] |
| Constellation | Scorpius |
| Right ascension | 17h 14m [3] |
| Declination | −39.8°[3] |
| Epoch | J2000 |
| Galactic coordinates | G347.4−00.6°[3] |
| Distance | 1 kpc (3×103 ly)[4] |
| Remnant | Shell |
| Host | Milky Way |
| Peak apparent magnitude | −1[5] |
| Other designations | SN 393 |
| Preceded by | SN 386 |
| Followed by | SN 1006 |
A guest star appeared within the asterism Wěi during the second lunar month of the 18th year of the Tai-Yuan reign period, and disappeared during the ninth lunar month.
The second lunar month mentioned in the record corresponds to the period 27 February to 28 March 393 CE, while the ninth lunar month ran from 22 October to 19 November 393 CE. The bowl-shaped asterism named Wěi is formed by the tail of the modern constellation Scorpius. This asterism consists of the stars in Scorpius designated ε, μ, ζ, η, θ, ι, κ, λ and ν. The guest star reached an estimated apparent magnitude of −1 and was visible for about eight months before fading from sight,[5] whose lengthy duration suggests the source was a supernova.[6] However, a classical nova is not excluded as possibility.[7][6]
Suggested as supernova
editBefore 1975, the observation made by the Chinese between February and March 393 CE was considered to be likely a bright nova with a secondary maximum.[6] At the time, there were only seven possible candidate supernova remnants near where SN 393 was observed. Assuming maximum –1 magnitude occurred close to 10,000 pc (33,000 ly) away, this immediately ruled out four possible candidates. Another discounted remnant was G350.0-1.8, as the expectant expansion rate indicated the supernova occurred around 8,000 years ago. Of the two remaining sources, G348.5+0.1 and G348.7+0.3, were both at the required 10,000 pc. distance and also each had estimated ages of 1,500 years.[5] If true, it seems unlikely such supernovae would be visible to the naked eye over eight months, especially because they occurred close to a particularly dusty part of the galactic plane.[2]
Stephenson[8] and his colleagues preferred the supernova suggestion. In their most recent book and subsequent articles, Stephenson and Green[9] refer to the suggestion by Wang et al. (1997)[10] who suggested G347.3–00.5.
Suggested as classical nova
editThe decline time of classical novae is measured typically as the duration of decline by 3 mag from peak. This so-called t3 time ranges from typical 25–30 days (a month or two) for fast novae up to ten months for the slowest known classical novae (and even longer for diffusion induced novae).[11][12] Thus, this historical transient could easily have been caused by a (slow) classical nova: postulating a peak brightness of (at least) 2 mag for the historical sighting and vanishing to invisibility (>5 mag) within 8 months, it could be a slow nova. The brighter the peak, the faster the nova: if the peak was −1 mag (like Sirius) or −4 (like Venus) and declined to >5 mag within eight months (6 mag or more in eight months) it could also refer to a moderately fast nova. Possible (and certainly not the only) candidates in the Chinese constellation of Wei are according to:[7]
| V643 Sco | a Z Cam-type dwarf nova |
| IGR J17195–4100 | intermediate polar |
Possible confirmation of SN 393
editDuring 1996, the ROSAT All Sky Survey discovered another nearby supernova remnant, RX J1713.7-3946, which two years later, was suggested as a better match for SN 393.[13] Observations in 1999 suggested that this remnant was associated with a H II region, G347.611 +0.204, whose distance was about 6,000 pc (20,000 ly), but in 2003, examining interactions between a nearby molecular cloud and the expanding remnant found the closer distance of around 1,000 pc (3,000 ly). In 2004, measures of the degree of X-ray and neutral hydrogen absorption by intervening matter between the remnant and Earth, confirmed this closer distance, making the true physical remnant diameter as 20 pc (65 ly), assuming the apparent angular diameter of about 1.2° or 70 arcminutes.[4]
Supernova remnant RX J1713.7-3946 is consistent with type II or type Ib supernovae. SN 393's progenitor had a mass of at least 15 solar masses, whose destruction generated energies of about 1.3 × 1051 erg, with three solar masses of material ejected into the surrounding interstellar medium.[1]
See also
editReferences
edit- ^ a b Berezhko, E. G.; Völk, H. J. (February 2010). "Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946". Astronomy and Astrophysics. 511: A34. arXiv:0910.2094. Bibcode:2010A&A...511A..34B. doi:10.1051/0004-6361/200913312. S2CID 56214010.
- ^ a b c Wang, Zhen-Ru (2005-04-01). "The impact of historical Chinese astronomical records". Astrophysics and Space Science. 305 (3): 207–210. Bibcode:2006Ap&SS.305..207W. doi:10.1007/s10509-006-9187-8. ISBN 9789211009590. S2CID 120568398.
- ^ a b c "SN 393 -- SuperNova". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2011-07-16.
- ^ a b Acero, F.; et al. (October 2009). "A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946". Astronomy and Astrophysics. 505 (1): 157–167. arXiv:0906.1073. Bibcode:2009A&A...505..157A. doi:10.1051/0004-6361/200811556. S2CID 53982263.
- ^ a b c Clark, D. H.; Stephenson, F. R. (October 1975). "The remnants of the supernovae of AD 185 and AD 393". The Observatory. 95: 190–195. Bibcode:1975Obs....95..190C.
- ^ a b c Clark, D. H.; Stephenson, F. R.; Stephenson, F. R. (September 1976). "Which historical new stars were supernovae". Quarterly Journal of the Royal Astronomical Society. 17: 290–302. Bibcode:1976QJRAS..17..290C.
- ^ a b Hoffmann, Susanne M.; Vogt, Nikolaus (2020-07-01). "A search for the modern counterparts of the Far Eastern guest stars 369 CE, 386 CE and 393 CE". Monthly Notices of the Royal Astronomical Society. 497 (2): 1419–1433. arXiv:2007.01013. Bibcode:2020MNRAS.497.1419H. doi:10.1093/mnras/staa1970.
- ^ Clark, D. H.; Stephenson, F. R. (1976-09-01). "Which historical new stars were supernovae". Quarterly Journal of the Royal Astronomical Society. 17: 290–302. Bibcode:1976QJRAS..17..290C. ISSN 0035-8738.
- ^ Stephenson, F. R.; Green, D. A. (2005-12-01). "Historical Supernovae". 1604-2004: Supernovae as Cosmological Lighthouses. 342: 63–70. Bibcode:2005ASPC..342...63S.
- ^ Wang, Z. R.; Qu, Q.-Y.; Chen, Y. (1997-02-01). "Is RX J1713.7-3946 the remnant of the AD393 guest star?". Astronomy and Astrophysics. 318: L59–L61. Bibcode:1997A&A...318L..59W. ISSN 0004-6361.
- ^ Strope, Richard J.; Schaefer, Bradley E.; Henden, Arne A. (2010-07-01). "Catalog of 93 Nova Light Curves: Classification and Properties". The Astronomical Journal. 140 (1): 34–62. arXiv:1004.3698. Bibcode:2010AJ....140...34S. doi:10.1088/0004-6256/140/1/34.
- ^ Hoffmann, Susanne M.; Vogt, Nikolaus (2020-07-01). "Counterparts of Far Eastern Guest Stars: Novae, supernovae, or something else?". Monthly Notices of the Royal Astronomical Society. 496 (4): 4488–4506. arXiv:2006.00977. Bibcode:2020MNRAS.496.4488H. doi:10.1093/mnras/staa1685.
- ^ Wang, Z.-R.; Qu, Q. Y.; Chen, Y. (1998). "The AD 393 Guest Star; the SNR RX 51713.7-3946". In Katsuji Koyama; Shunji Kitamoto; Masayuki Itoh (eds.). The Hot Universe. Proceedings of IAU Symposium #188. Dordrecht: Kluwer Academic. p. 262. Bibcode:1998IAUS..188..262W.