Cassiopeia A

Cassiopeia A
A false color image composited of data from three sources. Red is infrared data from the Spitzer Space Telescope, orange is visible data from the Hubble Space Telescope, and blue and green are data from the Chandra X-ray Observatory. The cyan dot just off-center is the remnant of the star's core.
Other designations SN 1671, SN 1667, SN 1680, SNR G111.7-02.1, 1ES 2321+58.5, 3C 461, 3C 461.0, 4C 58.40, 8C 2321+585, 1RXS J232325.4+584838
Event type Supernova remnant, astronomical radio source edit this on wikidata
Spectral class IIb [1]
Date 1947
Constellation Cassiopeia Edit this on Wikidata
Right ascension 23h 23m 24s
Declination +58° 48.9′
Epoch J2000
Galactic coordinates 111.734745 -02.129570
Distance 11 kly (3.4 kpc)[2]
Remnant Shell
Host Milky Way
Progenitor Unknown
Progenitor type Unknown
Colour (B-V) Unknown
Notable features Strongest radio source beyond our solar system
Peak apparent magnitude 6?
Preceded by SN 1604
Followed by G1.9+0.3 (unobserved, c. 1868), SN 1885A (next observed)
Related media on Wikimedia Commons
Cassiopeia A observed by the Hubble Space Telescope

Cassiopeia A (Cas A) is a supernova remnant (SNR) in the constellation Cassiopeia and the brightest extrasolar radio source in the sky at frequencies above 1 GHz. The supernova occurred approximately 11,000 light-years (3.4 kpc) away within the Milky Way.[2][3] The expanding cloud of material left over from the supernova now appears approximately 10 light-years (3 pc) across from Earth's perspective. In wavelengths of visible light, it has been seen with amateur telescopes down to 234mm (9.25 in) with filters.[4]

It is estimated that light from the stellar explosion first reached Earth approximately 300 years ago, but there are no historical records of any sightings of the supernova that created the remnant. Since Cas A is circumpolar for mid-Northern latitudes, this is probably due to interstellar dust absorbing optical wavelength radiation before it reached Earth (although it is possible that it was recorded as a sixth magnitude star 3 Cassiopeiae by John Flamsteed on August 16, 1680[5]). Possible explanations lean toward the idea that the source star was unusually massive and had previously ejected much of its outer layers. These outer layers would have cloaked the star and re-absorbed much of the light released as the inner star collapsed.

Cas A was among the first discrete astronomical radio sources found. Its discovery was reported in 1948 by Martin Ryle and Francis Graham-Smith, astronomers at Cambridge, based on observations with the Long Michelson Interferometer.[6] The optical component was first identified in 1950.[7]

Cas A is 3C461 in the Third Cambridge Catalogue of Radio Sources and G111.7-2.1 in the Green Catalog of Supernova Remnants.

Earlier discovery

Calculations working back from the currently observed expansion point to an explosion that would have become visible on Earth around 1667. Astronomer William Ashworth and others have suggested that the Astronomer Royal John Flamsteed may have inadvertently observed the supernova on August 16, 1680, when he catalogued a star near its position. Another suggestion from recent cross-disciplinary research is that the supernova was the mythical "noon day star", observed in 1630, that heralded the birth of Charles II, the future monarch of Great Britain.[8] At any rate, no supernova occurring within the Milky Way has been visible to the naked eye from Earth since.

Expansion

The expansion shell has a temperature of around 50 million degrees Fahrenheit (30 megakelvins), and is expanding at 4000−6000 km/s.[2]

Observations of the exploded star through the Hubble telescope have shown that, despite the original belief that the remnants were expanding in a uniform manner, there are high velocity outlying eject knots moving with transverse velocities of 5,500−14,500 km/s with the highest speeds occurring in two nearly opposing jets.[2] When the view of the expanding star uses colors to differentiate materials of different chemical compositions, it shows that similar materials often remain gathered together in the remnants of the explosion.[3]

Radio source

Cas A had a flux density of 2720 ± 50 Jy at 1 GHz in 1980.[9] Because the supernova remnant is cooling, its flux density is decreasing. At 1 GHz, its flux density is decreasing at a rate of 0.97 ± 0.04 percent per year.[9] This decrease means that, at frequencies below 1 GHz, Cas A is now less intense than Cygnus A. Cas A is still the brightest extrasolar radio source in the sky at frequencies above 1 GHz.

X-ray source

In 1999, the Chandra X-Ray Observatory found a "hot point-like source" close to the center of the nebula that is the neutron star remnant left by the explosion.[10]

Although Cas X-1 (or Cas XR-1), the apparent first X-ray source in the constellation Cassiopeia was not detected during the June 16, 1964, Aerobee sounding rocket flight, it was considered as a possible source.[11] Cas A was scanned during another Aerobee rocket flight of October 1, 1964, but no significant X-ray flux above background was associated with the position.[12] Cas XR-1 was discovered by an Aerobee rocket flight on April 25, 1965,[13] at RA 23h 21m Dec +58° 30′.[14] Cas X-1 is Cas A, a Type II SNR at RA 23h 18m Dec +58° 30′.[15]

The designations Cassiopeia X-1, Cas XR-1, Cas X-1 are no longer used, but the X-ray source is Cas A (SNR G111.7-02.1) at 2U 2321+58.

Supernova reflected echo

Recently, an infrared echo of the Cassiopeia A explosion was observed on nearby gas clouds using Spitzer Space Telescope.[1] The recorded spectrum proved the supernova was of Type IIb, meaning it resulted from the internal collapse and violent explosion of a massive star, most probably a red supergiant with a helium core which had lost almost all of its hydrogen envelope. This was the first observation of the infrared echo of a supernova whose explosion had not been directly observed which opens up the possibility of studying and reconstructing past astronomical events.[16]

Phosphorus detection

In 2013, astronomers detected phosphorus in Cassiopeia A, which confirmed that this element is produced in supernovae through supernova nucleosynthesis. The phosphorus-to-iron ratio in material from the supernova remnant could be up to 100 times higher than in the Milky Way in general.[17]

See also

References

  1. 1 2 Krause, Oliver; et al. (2008). "The Cassiopeia A Supernova was of Type IIb". Science. 320 (5880): 1195–1197. arXiv:0805.4557. Bibcode:2008Sci...320.1195K. doi:10.1126/science.1155788. PMID 18511684.
  2. 1 2 3 4 Fesen, Robert A.; Hammell, Molly C.; Morse, Jon; Chevalier, Roger A.; Borkowski, Kazimierz J.; Dopita, Michael A.; Gerardy, Christopher L.; Lawrence, Stephen S.; Raymond, John C.; van den Bergh, Sidney (July 2006). "The Expansion Asymmetry and Age of the Cassiopeia A Supernova Remnant". The Astrophysical Journal. 645 (1): 283–292. arXiv:astro-ph/0603371. Bibcode:2006ApJ...645..283F. doi:10.1086/504254.
  3. 1 2 Stover, Dawn (2006). "Life In A Bubble". Popular Science. 269 (6): 16.
  4. ↑ Howard Banich. A Visual Guide to the Cassiopeia A Supernova Remnant. Sky & Telescope, December 2014.
  5. ↑ Hughes DW (1980). "Did Flamsteed see the Cassiopeia A supernova?". Nature. 285 (5761): 132–133. Bibcode:1980Natur.285..132H. doi:10.1038/285132a0.
  6. ↑ Ryle, M.; Smith, F. G. (September 18, 1948). "A New Intense Source of Radio-Frequency Radiation in the Constellation of Cassiopeia". Nature. 162 (4116): 462–463. Bibcode:1948Natur.162..462R. doi:10.1038/162462a0.
  7. ↑ Fabian, A. C. (2008). "Astronomy. A blast from the past". Science. 320 (5880): 1167–1168. doi:10.1126/science.1158538. PMID 18511676.
  8. ↑ Oullette, Jennifer. "Did Supernova Herald the Birth of a King?". Discovery.com. Retrieved 18 April 2011.
  9. 1 2 Baars, J. W. M.; Genzel, R.; Pauliny-Toth, I. I. K.; Witzel, A. (1977). "The Absolute Spectrum of Cas A; An Accurate Flux Density Scale and a Set of Secondary Calibrators". Astronomy and Astrophysics. 61: 99. Bibcode:1977A&A....61...99B.
  10. ↑ Elshamouty, K. G.; Heinke, C. O.; Sivakoff, G. R.; Ho, W. C. G.; Shternin, P. S.; Yakovlev, D. G.; Patnaude, D. J.; David, L. (2013). "Measuring the cooling of the neutron star in Cassiopeia A with all Chandra X-Ray Observatory detectors". Astrophysical Journal. 777 (1): 22. arXiv:1306.3387. Bibcode:2013ApJ...777...22E. doi:10.1088/0004-637X/777/1/22.
  11. ↑ Bowyer S, Byram ET, Chubb TA, Friedman H (1965). Steinberg JL, ed. "Observational results of X-ray astronomy". Astronomical Observations from Space Vehicles, Proceedings from Symposium no. 23 held in Liege, Belgium, 17 to 20 August 1964. Symposium. International Astronomical Union. no. 23: 227–39. Bibcode:1965IAUS...23..227B.
  12. ↑ Fisher PC, Johnson HM, Jordan WC, Meyerott AJ, Acton LW (1966). "Observations of Cosmic X-rays". Astrophysical Journal. 143: 203–17. Bibcode:1966ApJ...143..203F. doi:10.1086/148491.
  13. ↑ Byram ET, Chubb TA, Friedman H (Apr 1966). "Cosmic X-ray Sources, Galactic and Extragalactic". Science. 152 (3718): 66–71. Bibcode:1966Sci...152...66B. doi:10.1126/science.152.3718.66. PMID 17830233.
  14. ↑ Friedman H, Byram ET, Chubb TA (April 1967). "Distribution and Variability of Cosmic X-Ray Sources". Science. 156 (3773): 374–8. Bibcode:1967Sci...156..374F. doi:10.1126/science.156.3773.374. PMID 17812381.
  15. ↑ Webber WR (December 1968). "X-ray astronomy-1968 vintage". Proc Astron Soc Australia. 1: 160–4. Bibcode:1968PASAu...1..160W.
  16. ↑ Fabian, Andrew C. (2008). "A Blast from the Past". Science. 320 (5880): 1167–1168. doi:10.1126/science.1158538. PMID 18511676.
  17. ↑ Koo, B. -C.; Lee, Y. -H.; Moon, D. -S.; Yoon, S. -C.; Raymond, J. C. (2013). "Phosphorus in the Young Supernova Remnant Cassiopeia A". Science. 342 (6164): 1346. arXiv:1312.3807. Bibcode:2013Sci...342.1346K. doi:10.1126/science.1243823. PMID 24337291.
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