IRC +10216
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Leo (constellation) |
| Right ascension | 09h 47m 57.406s[1] |
| Declination | +13° 16′ 43.56″[1] |
| Characteristics | |
| Spectral type | C |
| Apparent magnitude (R) | 10.96[1] |
| Apparent magnitude (J) | 7.34[1] |
| Apparent magnitude (H) | 4.04[1] |
| Apparent magnitude (K) | 1.19[1] |
| Astrometry | |
| Distance | 390–490[2] ly (120–150 pc) |
| Details | |
| Mass | 0.8[3] M☉ |
| Radius | 700[3] R☉ |
| Luminosity | 11,300[4] L☉ |
| Temperature | 2,200[3] K |
| Other designations | |
IRC +10216 or CW Leonis is a well-studied carbon star that is embedded in a thick dust envelope. It was first discovered in 1969 by a group of astronomers led by Eric Becklin, based upon infrared observations made with the 62 inches (1.6 m) Caltech Infrared Telescope at Mount Wilson Observatory. Its energy is emitted mostly at infrared wavelengths. At a wavelength of 5 μm, it was found to have the highest flux of any object outside the Solar System.[6]
CW Leonis is believed to be in a late stage of its life, blowing off its own sooty atmosphere to form a white dwarf in a distant future. Based upon isotope ratios of magnesium, the initial mass of this star has been constrained to lie between 3–5 solar masses. The mass of the star's core, and the final mass of the star once it becomes a white dwarf, is about 0.7–0.9 solar masses.[7] It has a nominal luminosity of 11,300 times the Sun. This varies over the course of a 649 day pulsation cycle, ranging from a minimum of about 6,250 times the Sun's luminosity up to a peak of around 15,800 times.[4]
The carbon-rich gaseous envelope surrounding this star is at least 69,000 years old and the star is losing about (1–4) × 10−5 solar masses per year.[4] The extended envelope contains at least 1.4 solar masses of material.[2] Speckle observations from 1999 show a complex structure to this dust envelope, including partial arcs and unfinished shells. This clumpiness may be caused by a magnetic cycle in the star that is comparable to the solar cycle in the Sun and results in periodic increases in mass loss.[8] Various chemical elements and about 50 molecules have been detected in the outflows from CW Leonis, among others nitrogen, oxygen and water, silicon and iron.
If the distance to this star is assumed to be at the lower end of the estimate range, 120 pc, then the astrosphere surrounding the star spans a radius of about 84,000 AU. The star and its surrounding envelope are advancing at a velocity of more than 91 km/s through the surrounding interstellar medium.[2] It is moving with a space velocity of [U, V, W] = [21.6 ± 3.9, 12.6 ± 3.5, 1.8 ± 3.3] km s−1.[7]
[edit] References
- ^ a b c d e f Cutri, R. M.; et al. "2MASS All-Sky Catalog of Point Sources". VizieR On-line Data Catalog: II/246. Bibcode 2003yCat.2246....0C. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246.
- ^ a b c Sahai, Raghvendra; Chronopoulos, Christopher K. (March 2010). "The Astrosphere of the Asymptotic Giant Branch Star IRC+10216". The Astrophysical Journal Letters 711 (2): L53–L56. Bibcode 2010ApJ...711L..53S. DOI:10.1088/2041-8205/711/2/L53.
- ^ a b c Weigelt, G. et al. (may 1998), "76mas speckle-masking interferometry of IRC+10216 with the SAO 6m telescope: Evidence for a clumpy shell structure", Astronomy and Astrophysics 333: L51–L54, arXiv:astro-ph/9805022, Bibcode 1998A&A...333L..51W
- ^ a b c De Beck, E. et al. (January 10, 2012), "On the physical structure of IRC+10216", Astronomy & Astrophysics, arXiv:1201.1850, DOI:10.1051/00046361/201117635
- ^ "V* CW Leo -- Variable Star of Mira Cet type". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=V*+CW+Leo. Retrieved 2011-05-09.
- ^ Becklin, E. E.; et al (December 1969). "The Unusual Infrared Object IRC+10216". Astrophysical Journal 158: L133. Bibcode 1969ApJ...158L.133B. DOI:10.1086/180450.
- ^ a b Astronomy and Astrophysics; et al (July 2010). Herschel PACS and SPIRE imaging of CW Leonis. 518. Bibcode 2010A&A...518L.141L. DOI:10.1051/0004-6361/201014658.
- ^ Dinh-V-Trung, Jeremy; Lim (May 2008), "Molecular Shells in IRC+10216: Evidence for Nonisotropic and Episodic Mass-Loss Enhancement", The Astrophysical Journal 678 (1): 303–308, Bibcode 2008ApJ...678..303D, DOI:10.1086/527669
[edit] External links
- Water Found Around Nearby Star CW Leonis NASA article.
- Variations in the dust envelope around IRC +10216 revealed by aperture masking interferometry
- Simbad info for IRC +10216 including over 1200 articles discussing this object.
- http://jumk.de/astronomie/special-stars/cw-leonis.shtml
- IRC +10216 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
