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]
 Radio image of G12.82-0.02 | |
| Event type | Supernova |
|---|---|
| SNII | |
| Date | c. 1708-1720 (discovered in 2005) |
| Constellation | Sagittarius |
| Right ascension | 18h 13m 36.0s |
| Declination | −17° 49′ 00″ |
| Epoch | J2000 |
| Distance | c. 14,700 ly (4,500 pc) |
| Host | Milky Way |
| Progenitor | Red supergiant |
| Other designations | G12.82-0.02, SNR G012.8-00.0, GAL 012.82-00.02 |
| Preceded by | Cassiopeia A |
| Followed by | G1.9+0.3 |
Supernova
editG12.82-0.02 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
editThe 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
edit- G1.9+0.3, another recently formed supernova remnant.
- Cassiopeia A, another core-collapse supernova in the Milky Way.
References
edit- 1 2 "G12.82-0.02". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2026-01-13.
- 1 2 3 4 Dean, A. J. (2008). "The properties of the putative pulsar associated with IGR J18135-1751/HESS J1813-178". Astronomy & Astrophysics. 485 (1): 195. arXiv:0804.3420. Bibcode:2008A&A...485..195D. doi:10.1051/0004-6361:200809356.
- ↑ Funk, S. (2007). "XMM-Newton observations of HESS J1813-178 reveal a composite Supernova remnant". Astronomy & Astrophysics. 470 (1): 249. arXiv:astro-ph/0611646. Bibcode:2007A&A...470..249F. doi:10.1051/0004-6361:20066779.
- ↑ 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. arXiv:astro-ph/0505145. Bibcode:2005ApJ...629L.105B. doi:10.1086/491471.
- 1 2 3 4 5 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. arXiv:0907.0137. Bibcode:2009ApJ...700L.158G. doi:10.1088/0004-637X/700/2/L158.
- 1 2 3 Chawner, H. (2020). "A complete catalogue of dusty supernova remnants in the Galactic plane". Monthly Notices of the Royal Astronomical Society. 493 (2): 2706. arXiv:2001.05504. Bibcode:2020MNRAS.493.2706C. doi:10.1093/mnras/staa221.
- 1 2 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. arXiv:2009.00031. Bibcode:2020MNRAS.498.4396H. doi:10.1093/mnras/staa2653. PMC 7668304. PMID 33204043.
- ↑ 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. arXiv:0705.0065. Bibcode:2007ApJ...665.1297H. doi:10.1086/519734.