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SN 1181

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Supernova SN 1181
Pa 30 is the presumed remnant.
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Datebetween August 4 and August 6, 1181
ConstellationCassiopeia
Right ascension00h 53m 11.2s
Declination+67° 30′ 02.4″
EpochJ2000
RemnantPa 30
HostMilky Way
Notable featuresVisible at night for 185 days
Peak apparent magnitude0?
Preceded bySN 1054
Followed bySN 1572
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First observed between August 4 and August 6, 1181, Chinese and Japanese astronomers recorded the supernova now known as SN 1181 in eight separate texts. One of only five supernovae in the Milky Way confidently identified in pre-telescopic records,[1] it appeared in the constellation Cassiopeia and was visible and motionless against the fixed stars for 185 days. F. R. Stephenson first recognized that the 1181 AD "guest star" must be a supernova, because such a bright transient that lasts for 185 days and does not move in the sky can only be a galactic supernova.[2]

3C 58

Main article: 3C 58

The only plausible conventional supernova remnant in the historical area is the radio and X-ray pulsar J0205+6449 (also known as 3C 58), which rotates about 15 times per second. If the supernova and pulsar are associated, the star is still rotating about as quickly as it did when it first formed.[3] This is in contrast to the Crab pulsar, known to be the remnant of the SN 1054 supernova in the year 1054, which has lost two-thirds of its rotational energy in essentially the same span of time.[4]

In 2008, a review of the physical properties of 3C 58 suggested that the age of 3C 58 is too large to be associated with SN 1181. The proper motion of the expanding shell of 3C 58 had been measured three times, resulting in an estimated age of around 3500 years. A collection of age measurements from eight methods also returned ages from 2400 to 7000 years, none of which were as young as SN 1181.[5] However, in 2013 it was shown that many of the age results assumed an erroneous estimation of the distance to 3C 58 (~10 kpc), and that a more realistic distance estimate (2.0±0.3 kpc) brought the age of 3C 58 back into agreement with the age of SN 1181. As a result, 3C 58 still remained a plausible candidate for the remnant of SN 1181, as of 2013.[6]

A study from January 2023 showed that the ancient observations from 1181 AD are limited to a fairly small region. This region contains Pa 30, but does not contain 3C 58. This and other observations make it unlikely that 3C 58 is the remnant of SN 1181.[7]

Pa 30

Pa 30 was discovered in 2013 by American amateur astronomer Dana Patchick while searching for planetary nebula in WISE infrared data. [8] It was the 30th successful entry discovered by his searches, and as a result it is designated Pa 30. Pa 30 appeared as a nearly-round nebula roughly 171x156 arc-seconds in size, with an extremely blue central star. The shell is bright in the infrared, but very faint in the optical, at first visible only by light in the [O III] band.

The central star of Pa 30 is called IRAS 00500+6713 (WD J005311). The central star is an oxygen-rich Wolf-Rayet star.[9]

In 2019, optical spectroscopy of the central star revealed a very hot star with an intense stellar wind expanding at a very high rate of 16,000 km/s and a composition mainly of carbon, oxygen, and neon (with no hydrogen or helium).[10] Such a speed could only arise from a supernova or an event of similar magnitude, more specifically from a merger of two white dwarfs. X-ray spectroscopy studies of the shell also revealed a very hot nebula composed mainly of carbon, oxygen, and neon, and suggested that the age of the remnant was on the order of 800 years, similar to the known age of SN 1181.[11] However, the remnant star of Pa 30 is a white dwarf, not one of the conventional supernova remnants (neutron stars or black holes). It has been suggested that Pa 30 is the remnant of a rare class of supernovae known as "sub-luminous Type Iax Supernova" and that a merger of a CO white dwarf and an ONe white dwarf produced the remnant shell along with its supermassive white dwarf remnant. More recent observations in the [SII] band also revealed fine filamentary structures within the shell that had not previously been seen.[12][13]

A 2021 study reviewed the evidence favoring either 3C 58 or Pa 30 being SN 1181, and concluded that Pa 30 was more likely to be the remnant. The ages of the two remnants are both consistent with the age of SN 1181, but the brightness of a possible supernova from 3C 58 would be far too bright compared to the observed brightness of SN 1181 as recorded by Chinese and Japanese astronomers.[14]

  • Constrains from ancient Chinese and Japanese observations of SN 1181 (cyan area) and the position of 3C 58 and Pa 30 according to Schaefer 2023[7]
    Constrains from ancient Chinese and Japanese observations of SN 1181 (cyan area) and the position of 3C 58 and Pa 30 according to Schaefer 2023[7]
  • Pa 30 as shown with WISE
    Pa 30 as shown with WISE

See also

References

  1. ^ Stephenson, F. Richard; Green, David (2002). Historical Supernovae and their Remnants. Clarendon Press. ISBN 0-19-850766-6.
  2. ^ Stephenson, F. Richard (1971). "A Suspected Supernova in A. D. 1181". Quarterly Journal of the Royal Astronomical Society. 12: 10–38. Bibcode:1971QJRAS..12...10S.
  3. ^ Panagia, N.; Weiler, K. W. (1980). "The absolute magnitude and the type classification of SN 1181 equals 3 C 58". Astronomy and Astrophysics. 82 (3): 389–391. Bibcode:1980A&A....82..389P.
  4. ^ Galas, C. M. F.; Tuohy, I. R.; Garmire, G. P. (1980). "Soft X-ray observations of the supernova remnants HB 3 and 3C 58". The Astrophysical Journal Letters. 236: L13–L16. Bibcode:1980ApJ...236L..13G. doi:10.1086/183188.
  5. ^ Fesen, Robert; Rudie, Gwen; Hurford, Alan; Soto, Aljeandro (2008). "Optical Imaging and Spectroscopy of the Galactic Supernova Remnant 3C 58 (G130.7+3.1)". The Astrophysical Journal Supplement Series. 174 (2): 379–395. Bibcode:2008ApJS..174..379F. doi:10.1086/522781. S2CID 120672848.
  6. ^ Kothes, A. (2013). "Distance and age of the pulsar wind nebula 3C 58". Astronomy and Astrophysics. 560: A18. arXiv:1307.8384. Bibcode:2013A&A...560A..18K. doi:10.1051/0004-6361/201219839. S2CID 118595074.
  7. ^ a b Schaefer, Bradley E. (August 1, 2023). "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. 523: 3885–3904. arXiv:2301.04807. doi:10.1093/mnras/stad717. ISSN 0035-8711.{{cite journal}}: CS1 maint: unflagged free DOI (link)
  8. ^ Kronberger, M.; et al. (2014). New Planetary Nebulae and Candidates from Multicolour Multiwavelength Surveys (PDF). Asymmetrical Planetary Nebulae VI conference.
  9. ^ Ritter, Andreas; Parker, Quentin A.; Lykou, Foteini; Zijlstra, Albert A.; Guerrero, Martin A.; Le Du, Pascal (November 7, 2023). "From an amateur PN candidate to the Rosetta Stone of SN Iax research". IAU 384 conference proceedings: 6. arXiv:2311.03700. Bibcode:2023arXiv231103700R.
  10. ^ Gvaramadze, Vasilii V.; et al. (2019). "A massive white-dwarf merger product before final collapse". Nature. 569 (7758): 684–687. arXiv:1904.00012. Bibcode:2019Natur.569..684G. doi:10.1038/s41586-019-1216-1. PMID 31110332. S2CID 90260784.
  11. ^ Oskinova, Lidia M.; et al. (2020). "X-rays observations of a super-Chandrasekhar object reveal an ONe and a CO white dwarf merger product embedded in a putative SN Iax remnant". Astronomy & Astrophysics. 644: L8. arXiv:2008.10612. Bibcode:2020A&A...644L...8O. doi:10.1051/0004-6361/202039232. S2CID 221293111.
  12. ^ Hall, Shannon (January 26, 2023). "Weird supernova remnant blows scientists' minds". Nature. 614 (7947): 206. Bibcode:2023Natur.614..206H. doi:10.1038/d41586-023-00202-1. PMID 36702966.
  13. ^ Fesen, Robert A.; Schaefer, Bradley E.; Patchick, Dana (January 11, 2023). "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. 945 (1): L4. arXiv:2301.04809. Bibcode:2023ApJ...945L...4F. doi:10.3847/2041-8213/acbb67.
  14. ^ Ritter, Andreas; et al. (2021). "The Remnant and Origin of the Historical Supernova 1181 AD". The Astrophysical Journal Letters. 918 (2): L33. arXiv:2105.12384. Bibcode:2021ApJ...918L..33R. doi:10.3847/2041-8213/ac2253.
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