Astronomy:B324
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Triangulum |
| Right ascension | 01h 33m 55.93272s |
| Declination | 30° 45′ 30.4452″ |
| Apparent magnitude (V) | 14.683 |
| Characteristics | |
| Evolutionary stage | Yellow hypergiant |
| Spectral type | A8–F0Ia |
| B−V color index | 0.428 |
| Astrometry | |
| Proper motion (μ) | RA: 0.066±0.029 mas/yr Dec.: 0.007±0.020 mas/yr |
| Parallax (π) | -0.1049 ± 0.0259 mas |
| Distance | 2,700,000 ly |
| Absolute magnitude (MV) | –10.2 |
| Absolute bolometric magnitude (Mbol) | –10.1 |
| Details | |
| Radius | 484 - 642 R☉ |
| Luminosity | 863,000 - 875,000 L☉ |
| Temperature | 6,970 - 8,000 K |
| Other designations | |
LGGS J013355.96+304530.6 | |
| Database references | |
| SIMBAD | data |
B324 is a yellow hypergiant in the Triangulum Galaxy, located near the giant H II region IC 142 around 2.7 million light years away. It is the brightest star in the Triangulum Galaxy in terms of apparent magnitude.
Discovery
The star has been first catalogued in 1980 by Humphreys and Sandage. The star was found to be the brightest star in the galaxy. It was given the spectral type A5eIa and it was considered a blue supergiant with emission lines.[1]
Physical properties
In 1980 the star was already known as a very luminous star. The absolute visual magnitude was estimated to be -9.4, making it brighter than any other blue supergiant.[1] Later in 1990 and 1996 two papers obtained an even higher absolute magnitude of -10 and a luminosity of 787,000 L☉.[2][3]
The star has a P Cygni profile. This is commonly thought to be a characteristic of luminous blue variables. However, it is present in some other stars with high mass-loss rates, such as IRC +10420. Notably it's luminosity is similar to that of LBVs like S Doradus during an outburst. It also shares some characteristics with the A-type hypergiant HD 33579.[4]
The star was first suggested to be a star similar to S Doradus in 1995 based on the spectral similarities to Var B. Independently a year later a different study came to the same conclusion based on the spectral variation and the profile. It was given the spectral type F0-F5Ia+.[5]
A 2004 study has rejected this classification based on the lack of variability in this star.[6]
In 2012 a study found that the star is more similar to cool LBVs than to yellow hypergiants based on spectral variation, recent circumstellar ejecta and the very high luminosity (which the paper estimated to be 2 million L☉, significantly above the Humphreys-Davidson limit for stars with temperatures comparable to those of the star. While this would imply that the star has stayed in an outburst state for around 20 years, some stars have stayed in this state for even longer.[7]
However, a 2013 paper casts doubt on this classification. The Ca II and [Ca II] emission is strong and the star shows little variability, making it similar to the post-RSG IRC +10420. B324 also has small near-infrared excess. The high derived luminosity was based on a large distance to M33 and the luminosity was revised to 863,000 L☉. Other similarities to the yellow hypergiant mentioned above include the similar absorption line spectra. The star's temperature was estimaged to be 8,000 K and the spectral type A8-F0Ia was assigned to this star.[8]
A 2016 paper got a similar luminosity for the star (873,000 L☉) and a slighty lower temperature of 6,970 K.[9]
In 2017 it has been suggested that the star might be evolving to cooler temperatures instead, suggesting that the star has never been a red supergiant yet.[10]
The same year a paper supporting the post-RSG classification has been published, such as the small 12C/13C ratio and the Na I emission, present in Rho Cassiopeiae, HR 8752 and other yellow hypergiants.[11]
References
- ↑ 1.0 1.1 Humphreys, R. M.; Sandage, A. (1980-11-01). "On the stellar content and structure of the spiral galaxy M33.". The Astrophysical Journal Supplement Series 44: 319–381. doi:10.1086/190696. ISSN 0067-0049. Bibcode: 1980ApJS...44..319H. https://ui.adsabs.harvard.edu/abs/1980ApJS...44..319H.
- ↑ Humphreys, Roberta M.; Massey, Philip; Freedman, Wendy L. (1990-01-01). "Spectroscopy of Luminous Blue Stars in M31 and M33". The Astronomical Journal 99: 84. doi:10.1086/115315. ISSN 0004-6256. Bibcode: 1990AJ.....99...84H. https://ui.adsabs.harvard.edu/abs/1990AJ.....99...84H.
- ↑ Massey, Philip; Bianchi, Luciana; Hutchings, John B.; Stecher, Theodore P. (1996-10-01). "The UV-brightest Stars of M33 and Its Nucleus: Discovery, Photometry, and Optical Spectroscopy". The Astrophysical Journal 469: 629. doi:10.1086/177811. ISSN 0004-637X. Bibcode: 1996ApJ...469..629M. https://ui.adsabs.harvard.edu/abs/1996ApJ...469..629M.
- ↑ Herrero, A.; Lennon, D. J.; Vilchez, J. M.; Kudritzki, R. P.; Humphreys, R. H. (1994-07-01). "Spectroscopic observations of AB-supergiants in M 31 and M 33". Astronomy and Astrophysics 287: 885–892. ISSN 0004-6361. Bibcode: 1994A&A...287..885H. https://ui.adsabs.harvard.edu/abs/1994A&A...287..885H.
- ↑ Monteverde, M. I.; Herrero, A.; Lennon, D. J.; Kudritzki, R. P. (1996-08-01). "Spectroscopic observations of AB supergiants in M 33.". Astronomy and Astrophysics 312: 24–32. ISSN 0004-6361. Bibcode: 1996A&A...312...24M. https://ui.adsabs.harvard.edu/abs/1996A&A...312...24M.
- ↑ Chu, You-Hua; Gruendl, Robert A.; Stockdale, Christopher J.; Rupen, Michael P.; Cowan, John J.; Teare, Scott W. (2004-05-01). "The Nature of SN 1961V" (in en). The Astronomical Journal 127 (5): 2850. doi:10.1086/383556. ISSN 1538-3881. Bibcode: 2004AJ....127.2850C. https://iopscience.iop.org/article/10.1086/383556/meta.
- ↑ Clark, J. S.; Castro, N.; Garcia, M.; Herrero, A.; Najarro, F.; Negueruela, I.; Ritchie, B. W.; Smith, K. T. (2012-05-01). "On the nature of candidate luminous blue variables in M 33" (in en). Astronomy & Astrophysics 541: A146. doi:10.1051/0004-6361/201118440. ISSN 0004-6361. Bibcode: 2012A&A...541A.146C. https://www.aanda.org/articles/aa/abs/2012/05/aa18440-11/aa18440-11.html.
- ↑ Humphreys, Roberta M.; Davidson, Kris; Grammer, Skyler; Kneeland, Nathan; Martin, John C.; Weis, Kerstin; Burggraf, Birgitta (2013-07-24). "Luminous and Variable Stars in M31 and M33. I. The Warm Hypergiants and Post-Red Supergiant Evolution". The Astrophysical Journal 773 (1): 46. doi:10.1088/0004-637x/773/1/46. ISSN 0004-637X. Bibcode: 2013ApJ...773...46H. https://iopscience.iop.org/article/10.1088/0004-637X/773/1/46.
- ↑ Gordon, Michael S.; Humphreys, Roberta M.; Jones, Terry J. (2016-06-28). "Luminous and Variable Stars in M31 and M33. III. The Yellow and Red Supergiants and Post-Red Supergiant Evolution". The Astrophysical Journal 825 (1): 50. doi:10.3847/0004-637x/825/1/50. ISSN 1538-4357. Bibcode: 2016ApJ...825...50G.
- ↑ Humphreys, Roberta M.; Davidson, Kris; Hahn, David; Martin, John C.; Weis, Kerstin (2017-07-20). "Luminous and Variable Stars in M31 and M33. V. The Upper HR Diagram". The Astrophysical Journal 844 (1): 40. doi:10.3847/1538-4357/aa7cef. ISSN 1538-4357. Bibcode: 2017ApJ...844...40H.
- ↑ Kourniotis, M.; Bonanos, A. Z.; Yuan, W.; Macri, L. M.; Garcia-Alvarez, D.; Lee, C.-H. (2017-05-01). "Monitoring luminous yellow massive stars in M 33: new yellow hypergiant candidates" (in en). Astronomy & Astrophysics 601: A76. doi:10.1051/0004-6361/201629146. ISSN 0004-6361. Bibcode: 2017A&A...601A..76K. https://www.aanda.org/articles/aa/abs/2017/05/aa29146-16/aa29146-16.html.
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