AFGL 2298
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aquila |
| Right ascension | 19h 00m 10.89s[1] |
| Declination | +03° 45′ 47.1″[1] |
| Characteristics | |
| Spectral type | B:I:[e][2] B0-0.5I[3] |
| Apparent magnitude (J) | 12.164[1] |
| Apparent magnitude (H) | 8.918[1] |
| Apparent magnitude (K) | 6.91[4] |
| Variable type | LBV[2] |
| Astrometry | |
| Distance | 30,000±10,000 ly (10,000±3,000[2] pc) |
| Absolute bolometric magnitude (Mbol) | -11.25[5] |
| Details | |
| Radius | 158 - 385[5] R☉ |
| Luminosity | 1,300,000 - 2,000,000[5] L☉ |
| Temperature | 11,000 - 15,500[5] or 26,000[3] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
AFGL 2298, also known as IRAS 18576+0341, is a luminous blue variable star (LBV) located in the constellation Aquila, very close to the galactic plane. Its distance is not well known; it may be anywhere between 23,000 and 42,000 light years (7,000 to 13,000 parsecs) away from the Earth.[2] Despite being extremely luminous, it is extremely reddened by interstellar extinction, so its apparent magnitude is brighter for longer-wavelength passbands; in fact, in visual wavelengths it is completely undetectable.[6]
AFGL 2298 has an absolute bolometric magnitude of −11.25,[5] making it one of the most luminous stars known. Indeed, many of the hottest and most luminous stars known are luminous blue variables and other early-type stars. However, like all LBVs, AFGL 2298 is highly variable and the bolometric magnitude refers to its peak luminosity.[5] Its status as an LBV was confirmed in 2003.[2]
Like most extremely massive stars, AFGL 2298 is undergoing mass loss.[3] For example, in 2005 it was estimated to be losing 3.7×10−5 solar masses each year,[3] although the rate of mass loss itself varies frequently and dramatically.[5] The stellar mass is currently being ejected as a nebula around the star (similar to AG Carinae), which was imaged by the Very Large Telescope in 2010.[7] The nebula was found to be fairly circular, and the properties of the dust appeared to be constant throughout the entire nebula.[7]
| Effective temperature (K) | Mass loss rate (M☉/yr) | Bolometric luminosity (L☉) | |
|---|---|---|---|
| June 2001 | 11,700 | 4.5×10−5 | 1.5×106 |
| August 2002 | 10,900 | 1.2×10−4 | 1.3×106 |
| June 2006 | 10,300 | 5.2×10−5 | 2.0×106 |
| May 2007 | 10,900 | 4×10−5 | 1.5×106 |
See also
References
- 1 2 3 4 Cutri, R. M. (2003). "2MASS All-Sky Catalog of Point Sources". VizieR On-line Data Catalog. Bibcode:2003yCat.2246....0C.
- 1 2 3 4 5 Clark, J. S.; et al. (2003). "Confirmation of the Luminous Blue Variable nature of AFGL 2298". Astronomy and Astrophysics. 403: 653–658. Bibcode:2003A&A...403..653C. doi:10.1051/0004-6361:20030389.
- 1 2 3 4 Umana, G.; Buemi, C. S.; Trigilio, C.; Leto, P. (2005). "Current day mass loss rate for Luminous Blue Variable IRAS 18576+0341". Astronomy and Astrophysics. 437 (1): L1–L5. Bibcode:2005A&A...437L...1U. doi:10.1051/0004-6361:200500126.
- ↑ Kazarovets, E. V. (2006). "The 78th Name-List of Variable Stars". Information Bulletin on Variable Stars. Bibcode:2006IBVS.5721....1K.
- 1 2 3 4 5 6 7 8 Clark, J. S.; et al. "Bolometric luminosity variations in the luminous blue variable AFGL2298". Astronomy and Astrophysics. 507 (3): 1555–1565. arXiv:0909.4160. Bibcode:2009A&A...507.1555C. doi:10.1051/0004-6361/200912358.
- 1 2 "AFGL 2298". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 January 2017.
- 1 2 Buemi, C. S.; et al. (2010). "VISIR/VLT and VLA Joint Imaging Analysis of the Circumstellar Nebula Around IRAS 18576+0341". The Astrophysical Journal. 721 (2): 1404–1411. arXiv:1008.0997. Bibcode:2010ApJ...721.1404B. doi:10.1088/0004-637X/721/2/1404.