AE Andromedae (AE And) is a luminous blue variable (LBV), a type of variable star. The star is one of the most luminous variables in M31, the Andromeda Galaxy.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 00h 43m 02.52s[2] |
| Declination | +41° 49′ 12.2″[2] |
| Apparent magnitude (V) | 17.0-17.9[3] |
| Characteristics | |
| Spectral type | LBV |
| U−B color index | ~ −0.9[3] |
| B−V color index | ~ +0.1[3] |
| Variable type | LBV |
| Astrometry | |
| Radial velocity (Rv) | -193[4] km/s |
| Distance | ~2.5 million ly (~780 thousand pc) |
| Absolute magnitude (MV) | −7.0 to −10.2[3] |
| Details | |
| Mass | 50-120[5] M☉ |
| Radius | 55[6] R☉ |
| Luminosity | 450,000-700,000[6] L☉ |
| Temperature | 20,000[7] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
Discovery
editThe star was discovered to be variable in 1928, with a photographic magnitude range of 14.7-15.6, at the Harvard College Observatory and designated HV 4476.[8] A year later it was given the variable star designation AE Andromedae.[9] At that time it was the brightest stellar object in M31 and maintained a similar brightness for about 20 years.[7]
Early in the investigations leading to the definition of LBVs, AE And was identified as similar to the five Hubble–Sandage variables: Var A, Var B, Var C, and Var 2 in M33, and Var 19 in M31 (=AF Andromedae).[10][11][12] On the basis of color–color comparisons, it was assigned as spectral type B and described as related to the P Cygni variables. Observations from 1960 to 1970 showed irregular variations in the B (blue) magnitude between 16.2 and 17.6, with very similar V magnitudes, and U magnitudes around 0.4 brighter.[10] The first detailed spectrum was published in 1975.[4]
Spectrum
editAE And is seen to have a peculiar emission line spectrum described as very much like Eta Carinae, likely due to a dense stellar wind.[4] The spectrum in 2010 showed weaker emission lines and some weak and variable absorption lines.[7]
AE And has prominent allowed and forbidden FeII and hydrogen lines in its emission spectrum, as well as weaker HeI and NII lines. Some features suggest a B2-B3 spectral type but the emission and variability defy a normal classification.[4]
The 250.7 nm FeII line is unusually strong in emission. The same feature in Eta Carinae's spectrum has been attributed to a UV laser.[7]
Properties
editAE And was the brightest star in M31 when it was first noticed during an outburst, at an apparent magnitude around 15, equivalent to an absolute magnitude of −10.2, or around a million times brighter than the Sun. This implies that the outburst may have increased the luminosity of the star, which would be unusual for an LBV. The temperature at that time is not known because of a lack of spectra or multiband photometry, but a typical LBV is around 8,000K during an outburst.
Since the discovery outburst, AE And has mostly been in the quiescent, or hot, LBV phase, with small irregular brightness fluctuations. The spectrum has varied considerably even during that time, attributed to variations in the wind strength. The temperature is generally considered to be around 20,000K, consistent with a position on the S Doradus instability strip.[7]
The star's stellar winds are strong, at 3×10−5 M☉/yr, but slow, and have been measured on the order of 100 km/s which contributes to their optical density.[13] There is a shell of 6×10−3 M☉ thought to have been ejected during the early 20th century outburst at a rate of at least 3×10−4 M☉/yr.[6]
The effective radius when quiescent has been modelled at 55 R☉, based on an effective temperature of 21,000K. During an outburst, the temperature would drop and the radius increase dramatically as a pseudo-photosphere is formed due to increased mass loss.[7]
The star's mass has not been calculated explicitly, but this type of star is massive, typically 50–120 M☉.[5]
See also
edit
References
edit- ^ Soraisam, Monika D.; Bildsten, Lars; Drout, Maria R.; Prince, Thomas A.; Kupfer, Thomas; Masci, Frank; Laher, Russ R.; Kulkarni, Shrinivas R. (April 2020). "Variability of Massive Stars in M31 from the Palomar Transient Factory". The Astrophysical Journal. 893 (1): 11. arXiv:1908.02439. Bibcode:2020ApJ...893...11S. doi:10.3847/1538-4357/ab7b7b. S2CID 199472825.
- ^ a b Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
- ^ a b c d Humphreys, R. M.; Blaha, C.; d'Odorico, S.; Gull, T. R.; Benvenuti, P. (1984). "IUE and ground-based observations of the Hubble-Sandage variables in M31 and M33". The Astrophysical Journal. 278: 124. Bibcode:1984ApJ...278..124H. doi:10.1086/161774.
- ^ a b c d Humphreys, R. M. (1975). "The spectra of AE Andromedae and the Hubble-Sandage variables in M31 and M33". Astrophysical Journal. 200: 426. Bibcode:1975ApJ...200..426H. doi:10.1086/153806.
- ^ a b Burggraf, B.; Weis, K.; Bomans, D. J. (2006). "LBVs in M33: Their Environments and Ages". Stellar Evolution at Low Metallicity: Mass Loss. 353: 245. Bibcode:2006ASPC..353..245B.
- ^ a b c Szeifert, T.; Humphreys, R. M.; Davidson, K.; Jones, T. J.; Stahl, O.; Wolf, B.; Zickgraf, F.-J. (1996). "HST and groundbased observations of the 'Hubble-Sandage' variables in M 31 and M 33". Astronomy and Astrophysics. 314: 131. Bibcode:1996A&A...314..131S.
- ^ a b c d e f Humphreys, Roberta M.; Weis, Kerstin; Davidson, Kris; Bomans, D. J.; Burggraf, Birgitta (2014). "Luminous and Variable Stars in M31 and M33. II. Luminous Blue Variables, Candidate LBVs, Fe II Emission Line Stars, and Other Supergiants". The Astrophysical Journal. 790 (1): 48. arXiv:1407.2259. Bibcode:2014ApJ...790...48H. doi:10.1088/0004-637X/790/1/48. S2CID 119177378.
- ^ Luyten, W. J. (1928). "A New Variable in the Andromeda Nebula, H.V. 4476". Harvard College Observatory Bulletin. 859 (859): 1. Bibcode:1928BHarO.859....1L.
- ^ Guthnick, P.; Prager, R. (1929). "Benennung von veränderlichen Sternen". Astronomische Nachrichten. 234 (20): 377. Bibcode:1929AN....234..377G. doi:10.1002/asna.19282342002.
- ^ a b Sharov, A. S. (1973). "Bright variable stars in the Andromeda M31 and Triangulum M33 nebulae". Perem. Zvezdy. 19: 3. Bibcode:1973PZ.....19....3S.
- ^ Humphreys, R. M. (1978). "Luminous variable stars in M31 and M33". The Astrophysical Journal. 219: 445. Bibcode:1978ApJ...219..445H. doi:10.1086/155797.
- ^ Hubble, Edwin; Sandage, Allan (1953). "The Brightest Variable Stars in Extragalactic Nebulae. I. M31 and M33". Astrophysical Journal. 118: 353. Bibcode:1953ApJ...118..353H. doi:10.1086/145764.
- ^ King, N. L.; Walterbos, R. A. M.; Braun, R. (1998). "Discovery of Candidate Luminous Blue Variables in M31". The Astrophysical Journal. 507 (1): 210–220. Bibcode:1998ApJ...507..210K. doi:10.1086/306296.