WR 7

Today, WR 7 is a topic that has captured the attention of people of all ages and interests. Whether it is a cultural phenomenon, a prominent figure, or a historical event, WR 7 has managed to make a significant impact on society. In this article, we will explore everything related to WR 7 in detail, from its origin to its implications today. Over the next few pages, we will dive into a comprehensive analysis that will allow us to better understand the importance of WR 7 in today's world. Get ready to discover surprising and fascinating things about WR 7.

HD 56925

WR7 at the centre of NGC 2359
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Canis Major
Right ascension 07h 18m 29.1311s[1]
Declination −13° 13′ 01.514″[1]
Apparent magnitude (V) 11.56[2]
Characteristics
Spectral type WN4-s[3]
U−B color index −0.47[4]
B−V color index +0.28[4]
Astrometry
Proper motion (μ) RA: −3.601[1] mas/yr
Dec.: −2.998[1] mas/yr
Parallax (π)0.2096±0.0268 mas[1]
Distanceapprox. 16,000 ly
(approx. 4,800 pc)
Absolute magnitude (MV)−3.8[5]
Details
Mass13[3] M☉
Radius1.26[3] R☉
Luminosity229,000[3] L☉
Temperature112,200[3] K
Other designations
WR 7, HIP 35378, HD 56925, 2MASS J07182912-1313015.
Database references
SIMBADdata

WR 7 (HD 56925) is a Wolf–Rayet star in the constellation of Canis Major. It lies at the centre of a complex bubble of gas which is shocked and partially ionised by the star's radiation and winds.

The distance is uncertain, with estimates between 3.5 kiloparsecs (11,410 light-years) and 6.9 kiloparsecs (22,500 light-years). Assuming a distance of 4.8 kiloparsecs (15,600 light-years), this star is calculated to be 229,000 times brighter than the Sun, 13 times more massive, and 1.26 times larger with a surface temperature of 112,200 K. This makes it currently the second smallest known WN star in the galaxy, after WR 2.

Stars of its kind are characterised by a rapid loss of stellar mass, driven by chemically enriched high-speed stellar winds. It is estimated that it loses mass at the rate of 7x10−5 solar masses each year through winds of 1,545 km/s.[6]

The ring nebula NGC 2359 is excited by the ionising radiation of WR7. It is also known as Thor's Helmet or the Duck Nebula. The ring is approximately 4pc across and prominent at wavelengths from radio to X-ray.[6][7]

References

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (2012). "VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012)". VizieR On-line Data Catalog: I/322A. Originally Published in: 2012yCat.1322....0Z; 2013AJ....145...44Z. 1322. Bibcode:2012yCat.1322....0Z.
  3. ^ a b c d e Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J.; Oskinova, L. M. (2019). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy & Astrophysics. A57: 625. arXiv:1904.04687. Bibcode:2019A&A...625A..57H. doi:10.1051/0004-6361/201834850. S2CID 104292503.
  4. ^ a b Reed, B. Cameron (1998). "UBVβ Database for Case-Hamburg Northern and Southern Luminous Stars". The Astrophysical Journal Supplement Series. 115 (2): 271–275. Bibcode:1998ApJS..115..271R. doi:10.1086/313088. S2CID 120773004.
  5. ^ Crowther, Paul A.; Rate, Gemma (2020). "Unlocking Galactic Wolf–Rayet stars with Gaia DR2 – I. Distances and absolute magnitudes". Monthly Notices of the Royal Astronomical Society. 493 (1): 1512–1529. arXiv:1912.10125. Bibcode:2020MNRAS.493.1512R. doi:10.1093/mnras/stz3614. S2CID 209444955.
  6. ^ a b Cappa, C. E.; Goss, W. M.; Niemela, V. S.; Ostrov, P. G. (1999). "A Study of Neutral and Ionized Gas of the Wolf-Rayet Ring Nebula NGC 2359". The Astronomical Journal. 118 (2): 948. Bibcode:1999AJ....118..948C. doi:10.1086/300995. S2CID 123709946.
  7. ^ Zhekov, S. A. (2014). "X-rays from wind-blown bubbles: An XMM-Newton detection of NGC 2359". Monthly Notices of the Royal Astronomical Society. 443 (1): 12–18. arXiv:1406.2463. Bibcode:2014MNRAS.443...12Z. doi:10.1093/mnras/stu1138. S2CID 118510853.