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3C 392

Supernova remnant 3C 392
Event typeSupernova remnant
Type II (?)
ConstellationAquila
Right ascension18h 56m 11s
EpochJ2000
Galactic coordinatesG034.6-00.5
Distance~3,000 parsecs
RemnantPSR B1853+01
Notable featuresInteraction with a molecular cloud
[edit on Wikidata]

3C 392 (also known as SNR G034.6-00.5, W44 and CTB 60)[1] is a supernova remnant located in the constellation Aquila. It was discovered by Gart Westerhout in 1958 as part of a study of continuous radiation in the Milky Way at a frequency of 1390 MHz.[2]

Morphology

3C 392 is a supernova remnant of mixed morphology characterized by a bright radio-band shell and concentrated thermal X-ray emission from its center. In the radio band, 3C 392 has the appearance of a quasi-elliptic asymmetric bright shell, its emission being most intense along the eastern boundary; in the western region a bright arc can be seen.[3] In the X-ray spectrum it presents continuums of radiant recombination of highly ionized atoms, a common characteristic of other remnants with mixed morphology. The emission is predominantly thermal, which is based on the presence of magnesium, silicon and sulfur emission lines.[4] Likewise, the emission in hard X-rays has an arc-shaped structure that is correlated in space with the filament seen in the radio band.[5] 3C 392 has also been detected in gamma rays, probably originating from the decay of neutral pions.[6]

3C 392 is one of the few demonstrated cases of interaction between a supernova remnant and a molecular cloud, as corroborated by observations of OH masers at 1720 MHz.[4] Two stellar objects have been discovered at the interface between 3C 392 and an H II region massive youth.[5]

Remnant

3C 392 is associated with the pulsar PSR B1853+01, located to the south of the rest of the supernova, indicating that 3C 392 comes from a core collapse (CC) supernova. The wind from the pulsar has created a small synchrotron nebula (PWN) observed in both radio frequencies and X-rays.[7]

Age and distance

The age of 3C 392, evaluated by the characteristic age of the associated pulsar, is approximately 20,000 years.[8] Another different estimate, calculated by the age of the thermal plasma, 16,700 ± 2,500 years, is comparable to the previous value; however, its dynamic age—based on the speed and size of the shock wave—is considerably higher, although it is subject to a wide margin of error (55,000 ± 20,000 years).[9]

3C 392 is located at a distance between 2200[10] and 3000[11] parsecs, and is located in a complex region of the inner galactic plane. It is immersed in the W48 molecular cloud complex, a rich region of star formation.

See also

References

  1. ^ "W44". simbad.u-strasbg.fr. Retrieved 2024-07-18.
  2. ^ Westerhout, Gart (December 31, 1958). "A Survey Of the Continuous Radiation From The Galactic System At Frequency of 1390 Mc/S". ADSABS at HARVARD. Retrieved July 17, 2024.
  3. ^ Loru, S.; Pellizzoni, A.; Egron, E.; Righini, S.; Iacolina, M. N.; Mulas, S.; Cardillo, M.; Marongiu, M.; Ricci, R.; Bachetti, M.; Pilia, M.; Trois, A.; Ingallinera, A.; Petruk, O.; Murtas, G. (2019-01-01). "Investigating the high-frequency spectral features of SNRs Tycho, W44, and IC443 with the Sardinia Radio Telescope". Monthly Notices of the Royal Astronomical Society. 482 (3): 3857–3867. arXiv:1805.04376. Bibcode:2019MNRAS.482.3857L. doi:10.1093/mnras/sty1194. ISSN 0035-8711.
  4. ^ a b Okon, Hiromichi; Tanaka, Takaaki; Uchida, Hiroyuki; Yamaguchi, Hiroya; Tsuru, Takeshi Go; Seta, Masumichi; Smith, Randall K.; Yoshiike, Satoshi; Orlando, Salvatore; Bocchino, Fabrizio; Miceli, Marco (2020-02-01). "Deep XMM-Newton Observations Reveal the Origin of Recombining Plasma in the Supernova Remnant W44". The Astrophysical Journal. 890 (1): 62. arXiv:1912.08129. Bibcode:2020ApJ...890...62O. doi:10.3847/1538-4357/ab6987. ISSN 0004-637X.
  5. ^ a b Onić, D. (2015-12-01). "On the Integrated Continuum Radio Spectrum of Supernova Remnant W44 (G34.7-0.4): New Insights From Planck". Serbian Astronomical Journal. 191 (191): 29–37. arXiv:1505.03179. Bibcode:2015SerAJ.191...29O. doi:10.2298/SAJ150715004O.
  6. ^ Cardillo, M.; Tavani, M.; Giuliani, A.; Yoshiike, S.; Sano, H.; Fukuda, T.; Fukui, Y.; Castelletti, G.; Dubner, G. (2014-05-01). "The supernova remnant W44: Confirmations and challenges for cosmic-ray acceleration". Astronomy and Astrophysics. 565: A74. arXiv:1403.1250. Bibcode:2014A&A...565A..74C. doi:10.1051/0004-6361/201322685. ISSN 0004-6361.
  7. ^ Onić, D. (2015-12-01). "On the Integrated Continuum Radio Spectrum of Supernova Remnant W44 (G34.7-0.4): New Insights From Planck". Serbian Astronomical Journal. 191 (191): 29–37. arXiv:1505.03179. Bibcode:2015SerAJ.191...29O. doi:10.2298/SAJ150715004O.
  8. ^ Harrus, Ilana M.; Hughes, John P.; Singh, K. P.; Koyama, K.; Asaoka, I. (1997-10-01). "Interpretation of the Center-filled Emission from the Supernova Remnant W44". The Astrophysical Journal. 488 (2): 781–791. arXiv:astro-ph/9705239. Bibcode:1997ApJ...488..781H. doi:10.1086/304717. ISSN 0004-637X.
  9. ^ Suzuki, Hiromasa; Bamba, Aya; Shibata, Shinpei (2021-06-01). "Quantitative Age Estimation of Supernova Remnants and Associated Pulsars". The Astrophysical Journal. 914 (2): 103. arXiv:2104.10052. Bibcode:2021ApJ...914..103S. doi:10.3847/1538-4357/abfb02. ISSN 0004-637X.
  10. ^ Peron, Giada; Aharonian, Felix; Casanova, Sabrina; Zanin, Roberta; Romoli, Carlo (2020-06-01). "On the Gamma-Ray Emission of W44 and Its Surroundings". The Astrophysical Journal. 896 (2): L23. arXiv:2007.04821. Bibcode:2020ApJ...896L..23P. doi:10.3847/2041-8213/ab93d1. ISSN 0004-637X.
  11. ^ Ranasinghe, S.; Leahy, D. A. (2018-05-01). "Revised Distances to 21 Supernova Remnants". The Astronomical Journal. 155 (5): 204. arXiv:1808.09082. Bibcode:2018AJ....155..204R. doi:10.3847/1538-3881/aab9be. ISSN 0004-6256.
Quelle: https://en.wikipedia.org/wiki/3C_392