IRC-10414
| Observation data Epoch 2000 Equinox 2000 | |
|---|---|
| Constellation | Scutum |
| Right ascension | 18h 23m 17.85s |
| Declination | −13° 42′ 47.0″ |
| Apparent magnitude (V) | 12 |
| Characteristics | |
| Evolutionary stage | Red supergiant |
| Spectral type | M7I |
| Astrometry | |
| Proper motion (μ) | RA: 5.4 mas/yr Dec.: 1.6 mas/yr |
| Distance | 2,000 pc |
| Details | |
| Mass | 20-25 M☉ |
| Radius | 1,200 R☉ |
| Luminosity | 160,000 L☉ |
| Temperature | 3,300 K |
| Database references | |
| SIMBAD | data |
IRC-10414 is a red supergiant and runaway star in the constellation Scutum that forms a double star with the Wolf-Rayet star WR 114.
Features
This star, of spectral type M7, is highly notable for being one of the very few bow shock-producing red supergiant stars, the two others being Betelgeuse and Mu Cephei, and unlike the two others the bow shock is visible in visible light. Its stellar wind seems to be ionized too by the stars of the cluster NGC 6611 and/or the nearby (in the sky) Wolf-Rayet star WR 114.[1]
Its distance is not very well known, but it is estimated to be of the order of 2 kiloparsecs on the basis its parallax and closeness of this star to the open clusters and star formation regions NGC 6604, Eagle Nebula, and the Omega Nebula (the three sharing a similar distance to the Sun, of around 2 kiloparsecs too);[1] the studies of the water masers that surround her suggest a higher distance, up to around 3 kiloparsecs.[2] However, the birthplace of this star is not clear and its kinematics and age show its unlikely it had formed in any of the previous three star-forming regions mentioned.[1]
Assuming the distance given above and a surface temperature of 3,300K, IRC-10414 is 160,000 times brighter than the Sun and its diameter in the order of 1,200 times the solar one, which places this star among the largest known. Stellar evolution models suggest in that case an initial mass between 20 and 25 solar masses and an age between 6 and 10 million years.[1]
WR 114
WR 114 (HD 169010) is a Wolf-Rayet star of spectral class WC5 located close in the sky (45 arc-seconds away) to IRC-10414. Its distance (2 kiloparsecs -6.500 light years-) is similar to its apparent companion-, being around 220,000 times brighter than the Sun, and despite being just 2.5 times larger than our star is brighter than IRC-10414 because of its high surface temperature of 79,000K[3] versus the 3,300K estimated for its apparent companion.
The actual distance to its red supergiant neighbor is unclear, however, since was its projected separation in the sky the actual separation between the Wolf-Rayet and the red supergiant star, the strong stellar wind of the former would impede the formation of the bow shock of the latter. On the other hand, it has been suggested both stars formed part of a dissolved triple star system moving more or less together; however as the kinematicals of WR 114 are very poorly known is difficult to resolve this enigma.[1]
References
- 1 2 3 4 5 Gvaramadze, V. V.; Menten, K. M.; Kniazev, A. Y.; Langer, N.; MacKey, J.; Kraus, A.; Meyer, D. M.-A.; Kamiński, T. (2014). "IRC -10414: A bow-shock-producing red supergiant star". Monthly Notices of the Royal Astronomical Society 437: 843. Bibcode:2014MNRAS.437..843G. doi:10.1093/mnras/stt1943.
- ↑ Maeda, Toshihisa; Imai, Hiroshi; Omodaka, Toshihiro; Kobayashi, Hideyuki; Shibata, Katsunori M.; Bushimata, Takeshi; Choi, Yoon Kyung; Hirota, Tomoya; Honma, Mareki; Horiai, Koji; Inomata, Noritomo; Iwadate, Kenzaburo; Jike, Takaaki; Kameno, Seiji; Kameya, Osamu; Kamohara, Ryuichi; Kan-Ya, Yukitoshi; Kawaguchi, Noriyuki; Kuji, Seisuke; Kurayama, Tomoharu; Manabe, Seiji; Miyaji, Takeshi; Nagayama, Takumi; Nakagawa, Akiharu; Nakashima, Kouichiro; Oh, Chung Sik; Oyama, Tomoaki; Sakai, Satoshi; Sakakibara, Seiichiro; et al. (2008). "A Bipolar Outflow of the M-Type Giant IRC -10414 Traced by H2O Maser Emission". Publications of the Astronomical Society of Japan 60 (5): 1057. Bibcode:2008PASJ...60.1057M. doi:10.1093/pasj/60.5.1057.
- ↑ Sander, A.; Hamann, W. -R.; Todt, H. (2012). "The Galactic WC stars". Astronomy & Astrophysics 540: A144. arXiv:1201.6354. Bibcode:2012A&A...540A.144S. doi:10.1051/0004-6361/201117830.
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