Edge Rewrite
location Source code View original
// request.cf · coarse context

A page that knows where it met you.

Only coarse request metadata is shown. This demo does not display or persist visitor IP addresses.

Country
US
Cloudflare location
CMH
Connection
HTTP/2
Language
Not provided

Ray ID: a41e7fc68f49ddf0

Jump to content

RCW 114

From Wikipedia, the free encyclopedia

RCW 114
Supernova remnant
Observation data: J2000.0 epoch
Right ascension17h 25m 0.00s[1]
Declination−46° 30′ 0.0″[1]
Distance~600 to ~4,900[2] ly
ConstellationAra
Physical characteristics
Radius163[2] ly
DesignationsG 343.0-06.0, GRS G343.00-06.00, SNR G343.0-06.0[1]
See also: Lists of nebulae

RCW 114 aslo known as the Dragon's Heart is a massive faint supernova remnant (SNR) located 200 or 1,500 pc away in the constellation Ara. The remnant was discovered in 1960 by Alexander Rodgers, Colin Campbell, and John Whiteoak in their catalogue of Hα emission nebulae.[3]

Structure

[edit]

RCW 114 was originally thought to be a Wolf–Rayet nebula but was later proven to be an old supernova remnant (SNR). RCW 114 is ancient and a faint SNR with an angular size of approximately 250 arcminutes. It has a diameter of about 326 ly and a radius of 163 ly.[2] The shell interactions and shock-wave dynamics with the ambient interstellar medium (ISM) result in a radial expansion speed between 25 and 35 km/s.[4]

The star that most likely produced RCW 114 is pulsar B1727-47, the distance of the pulsar is ~0.6 kpc, which is consistent with a distance of ~600 ly.[5] Another study found that the pulsar formed near the center of RCW 114.[6]

History

[edit]

A 2003 study originally suggested that RCW 114 was a Wolf–Rayet nebula that was produced by the star HD 156385. HD 156385 is a B-type WR progenitor star at a distance of ~1,500 pc, which produced a small wind-blown bubble with a mass of 6,200 M☉ and a kinetic energy of ~10⁵⁰ ergs.[2] These values match with the kinetic energy of RCW 114, which is ≥10⁵¹ ergs. HD 156385 was also thought to be responsible for the observed Si II and Na I absorption lines, these lines were linked to a pre-existing SNR where RCW 114 expanded.[7] Estimates put the age of RCW 114 at 5 x 1,000,000 or 1.1 x 1,000,000 years, which aligned with the age of HD 156385.[8] This estimated the distance of RCW 114 at ~4,900 ly or ~1,500 pc with a radius of ~50 pc for RCW 114.[2]

A 2010 study detected a C IV emission-line in RCW 114 and gave a distance of ~200 pc (~600 ly) based on luminosity estimations.[4] This placed the distance of RCW 114 much closer than HD 156385, meaning that HD 156385 is not associated with RCW 114 aswell as the wind-blown bubble around the star. The C IV emission-line also proved that the pre-existing SNR is actually a part of RCW 114, confirming that RCW 114 is an old SNR.[9] The global morphologies of the C IV, Hα, H I emissions show that RCW 114 formed in a non-uniform interstellar medium (ISM).[10] The low density southeast region that overlaps the line of sight of HD 156385 explains why it was associated with RCW 114.[4]

References

[edit]
  1. 1 2 3 "SNR G343.0-06.0". simbad.cds.unistra.fr.
  2. 1 2 3 4 5 Welsh, B. Y.; Sallmen, S.; Jelinsky, S.; Lallement, P. (May 2003). "The RCW 114 nebula: An old supernova remnant or a WR wind-blown bubble?". Astronomy and Astrophysics. 403 (2): 605–611. Bibcode:2003A&A...403..605W. doi:10.1051/0004-6361:20030168.
  3. ↑ Rodgers, A. W.; Campbell, C. T.; Whiteoak, J. B. (1960). "A catalogue of Hα-emission regions in the southern Milky Way". Monthly Notices of the Royal Astronomical Society. 121: 103. Bibcode:1960MNRAS.121..103R. doi:10.1093/mnras/121.1.103.
  4. 1 2 3 Kim, I.-J.; Min, K.-W.; Seon, K.-I.; Han, W.; Edelstein, J. (February 2010). "Civ EMISSION-LINE DETECTION OF THE SUPERNOVA REMNANT RCW 114". The Astrophysical Journal. 709 (2): 823–831. arXiv:0912.2156. Bibcode:2010ApJ...709..823K. doi:10.1088/0004-637X/709/2/823.
  5. ↑ Shternin, P. S.; Yu, M.; Kirichenko, A. Yu.; Shibanov, Yu. A.; Danilenko, A. A.; Voronkov, M. A.; Zyuzin, D. A. (December 2017). "Proper motion of the radio pulsar B1727-47 and its association with the supernova remnant RCW 114". Journal of Physics: Conference Series. 932 (1) 012004. arXiv:1711.02517. Bibcode:2017JPhCS.932a2004S. doi:10.1088/1742-6596/932/1/012004. 012004.
  6. ↑ Shternin, P.; Kirichenko, A.; Zyuzin, D.; Yu, M.; Danilenko, A.; Voronkov, M.; Shibanov, Yu. (June 2019). "Tracking the Footprints of the Radio Pulsar B1727–47: Proper Motion, Host Supernova Remnant, and the Glitches". The Astrophysical Journal. 877 (2): 78. arXiv:1904.06368. Bibcode:2019ApJ...877...78S. doi:10.3847/1538-4357/ab1905. 78.
  7. ↑ Bedford, D. K.; Elliott, K. H.; Ramsey, B.; Meaburn, J. (October 1984). "Some properties of the filamentary nebula at 1723-46". Monthly Notices of the Royal Astronomical Society. 210 (3): 693–699. Bibcode:1984MNRAS.210..693B. doi:10.1093/mnras/210.3.693.
  8. ↑ Marston, A. P. (1997). "A Survey of Nebulae around Galactic Wolf-Rayet Stars in the Southern Sky. III. Survey Completion and Conclusions". The Astrophysical Journal. 475 (1): 188. Bibcode:1997ApJ...475..188M. doi:10.1086/303534.
  9. ↑ Shelton, R. L. (1999). "Simulations of Supernova Remnants in Diffuse Media. II. Three Remnants and Their X-Ray Emission"". The Astrophysical Journal. 521 (1): 217. arXiv:astro-ph/9904392. Bibcode:1999ApJ...521..217S. doi:10.1086/307553.
  10. ↑ Walker, A. J.; Zealey, W. J. (July 2001). "Multifibre spectroscopy of the supernova remnant candidate RCW 114". Monthly Notices of the Royal Astronomical Society. 325 (1): 287–292. Bibcode:2001MNRAS.325..287W. doi:10.1046/j.1365-8711.2001.04423.x.
Retrieved from "https://en.wikipedia.org/w/index.php?title=RCW_114&oldid=1377090700"