_cleaned_up.jpg) 2.4 Meter Kitt Peak image of the Pa 30 supernova remnant associated with the SN 1181 | |
| Observation data EpochJ2000.0 EquinoxJ2000.0 | |
|---|---|
| Constellation | Cassiopeia |
| Right ascension | 00h 53m 11.21s[1] |
| Declination | +67° 30′ 02.4″[1] |
| Apparent magnitude (V) | 15.4[2] |
| Astrometry | |
| Proper motion (μ) | RA: −2.258[1]mas/yr Dec.: −0.0988[1]mas/yr |
| Parallax (π) | 0.4065±0.0259 mas[1] |
| Distance | 8,000 ± 500 ly (2,500 ± 200 pc) |
| Details | |
| Mass | 1.20±0.17[3] M☉ |
| Radius | 0.155[3] R☉ |
| Luminosity | 36,000[3] L☉ |
| Temperature | 237,000[3] K |
| Database references | |
| SIMBAD | data |
IRAS 00500+6713 is the cataloguedinfrared source for an unusualnebula inCassiopeia, while the central star has a designation WD J005311, with the whole system designated asPa 30. The central star and its surrounding shell were created by thesupernova seen in the year 1181 (SN 1181) as reported by Chinese and Japanese observers.[4] Both the nebula and central star have unique and extreme properties, pointing to their creation by a raretype Iax supernova, where two ultra-densewhite dwarfs in-spiral to a collision and explosion.[3]
The Pa 30 system was discovered in 2013 by amateur astronomer Dana Patchick.[5] It was independently discovered by Dr. Vasili Gvaramadze and colleagues who first realized that the central star has extreme properties and proposed that it was created from a merger of twowhite dwarfs.[6] The star exhibits record-breakingwind speeds of 16,000 km/s and temperatures near 200,000 K. The central star, might be a rapidly-rotatingsuper-Chandrasekhar white dwarf with a mass ≳1.5 M☉.
The central star is surrounded by a nebula packed with hot gas and warm dust.[7] X-ray observations with theXMM-Newton telescope established that the star and its circumstellar nebula are strong X-ray sources. Analysis of X-ray spectra allowed for the first time to determine the chemical composition of the nebula. It was proposed that the nebula is a remnant of a rare type of supernova (SN Iax), and that the SN happened some 1000 years ago.[3]
It has been linked to the historic supernovaSN 1181.[4] The star is possibly highly unstable, too massive to remain as a white dwarf, and it is predicted to collapse into aneutron star within ten thousand years.[8]
Both the central star and the nebula contain large amounts ofneon,magnesium,silicon, andsulfur (but no hydrogen, helium, or nitrogen), with such requiring an origin in a recent supernova.[3] The surrounding shell has a unique structure with long radial filaments that have expansion velocities of around 1100 km/s.[9] Apparently, the filaments are the tattered remains of the original `slow' supernova ejecta, fragmented and streamed into long wakes by the on-going very fast stellar wind emanating from the central white dwarf.
![A comparison between an observed image (left panel; X-ray image (XMM) and IR contours (WISE)) and schematic picture of IRAS 00500+671[10]](/mt/?noimg=&dark=on&url=https%3a%2f%2fen.wikipedia.org%2fwiki%2fFile%3aIRAS_00500%252B6713.jpg)
