Astronomy:G12.82-0.02

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G12.82-0.02 also known as SNR G012.8-0.00, is a supernova remnant (SNR) and pulsar wind nebula (PWN) in the constellation of Sagittarius.[1][2] The supernova remnant is roughly 15,000 light years (or 4,500 parsecs) away, based on its likely association with the star-forming region designated W33.[2] The supernova remnant is located in the Galactic Plane, and a gas cloud was found near it with a molecular mass of 2.5×105 M☉.[3] The supernova remnant was discovered in 2005 as the host of the X-ray source and pulsar, HESS J1813-178.[4]

Supernova

G12.82-0.02 is the second youngest supernova remnant in the Milky Way only behind G1.9+0.3, which exploded in the late 19th century.[2] The supernova remnant is estimated to be extremely young because of its small size.[5] The supernova remnant has a diameter of 12.8 light years (or 4 parsecs) across, based on an angular diameter of 3 arcmin.[1] The supernova exploded between 1708 and 1720, preceded by Cassiopeia A, and was followed by G1.9+0.3.[2][6] The supernova was classified as a core collapse supernova (abbreviated as SNII).[6] The supernova could not have been observed from Earth due to it being obscured by dust.[6] The progenitor star was a 20 to 30 M☉ red supergiant, which is usual for this type of supernova.[5]

Central neutron star

The central neutron star of G12.82-0.02, referred to as PSR J1813-1749 is a millisecond pulsar.[5] PSR J1813-1749 has a rotational period of 44.7 milliseconds, and is extremely energetic.[7] The pulsar has one of the highest velocities of any neutron star in the Milky Way, with a velocity of 900 to 1,600 km/s.[7] It has a very strong magnetic field with a power of 2.7×1012 gauss.[5] The pulsar has a luminosity of 0.832 L☉ and an effective temperature of 3,481,000 kelvin, corresponding to a diameter of 3.49 kilometers.[8] The pulsar was originally formed in a nearby star cluster with a mass of 2,000 to 6,500 M☉.[5]

See also

  • G1.9+0.3, another recently formed supernova remnant.
  • Cassiopeia A, another core-collapse supernova in the Milky Way.

References

  1. ↑ 1.0 1.1 "G12.82-0.02". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=G12.82-0.02. 
  2. ↑ 2.0 2.1 2.2 2.3 Dean, A. J. (2008). "The properties of the putative pulsar associated with IGR J18135-1751/HESS J1813-178". Astronomy & Astrophysics 485 (1): 195. doi:10.1051/0004-6361:200809356. Bibcode: 2008A&A...485..195D. 
  3. ↑ Funk, S. (2007). "XMM-Newton observations of HESS J1813-178 reveal a composite Supernova remnant". Astronomy & Astrophysics 470 (1): 249. doi:10.1051/0004-6361:20066779. Bibcode: 2007A&A...470..249F. 
  4. ↑ Brogan, C. L. (2005). "Discovery of a Radio Supernova Remnant and Nonthermal X-Rays Coincident with the TeV Source HESS J1813-178". The Astrophysical Journal 629 (2): L105–L108. doi:10.1086/491471. Bibcode: 2005ApJ...629L.105B. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 Gotthelf, E. V. (2009). "Discovery of a Highly Energetic X-Ray Pulsar Powering HESS J1813-178 in the Young Supernova Remnant G12.82-0.02". The Astrophysical Journal 700 (2): L158–L161. doi:10.1088/0004-637X/700/2/L158. Bibcode: 2009ApJ...700L.158G. 
  6. ↑ 6.0 6.1 6.2 Chawner, H. (2020). "A complete catalogue of dusty supernova remnants in the Galactic plane". Monthly Notices of the Royal Astronomical Society 493 (2): 2706. doi:10.1093/mnras/staa221. Bibcode: 2020MNRAS.493.2706C. 
  7. ↑ 7.0 7.1 Ho, Wynn (2020). "Proper motion, spectra, and timing of PSR J1813-1749 using Chandra and NICER". Monthly Notices of the Royal Astronomical Society 498 (3): 4396–4403. doi:10.1093/mnras/staa2653. PMID 33204043. Bibcode: 2020MNRAS.498.4396H. 
  8. ↑ Hefland, D. J. (2007). "Discovery of the Putative Pulsar and Wind Nebula Associated with the TeV Gamma-Ray Source HESS J1813-178". The Astrophysical Journal 665 (2): 1297. doi:10.1086/519734. Bibcode: 2007ApJ...665.1297H. 



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