Iota Aquarii
Iota Aquarii
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| Ligging van ι Aquarii (in die rooi sirkel). | ||||
| Sterrebeeld | Waterdraer | |||
| Spektraaltipe | B8V[1] | |||
| Waarnemingsdata (Epog J2000) | ||||
| Regte klimming | 22h 06m 26.22742s[2] | |||
| Deklinasie | –13° 52′ 10.8615″[2] | |||
| Skynmagnitude (m) | 4,279[3] | |||
| Absolute magnitude (M) | +0,64[4] | |||
| B-V-kleurindeks | -0,062[3] | |||
| U-B-kleurindeks | -0,288[3] | |||
| Besonderhede | ||||
| Radius (R☉) | 2,7[5] | |||
| Ligsterkte (L☉) | 74[4] | |||
| Ouderdom (jaar) | 30-60 miljoen[6] | |||
| Temperatuur (K) | 11 284 ± 284[5] | |||
| Rotasiespoed (km/s) | 135[7] | |||
| Metaalinhoud [Fe/H] | -0,08 ± 0,12[8] | |||
| Ander name | ||||
| ι Aqr, 33 Aquarii, BD-14 6209, FK5 828, HD 209819, HIP 109139, HR 8418, SAO 164861[9] | ||||
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Iota Aquarii of ι Aquarii is die Bayer-naam van ’n ster in die sterrebeeld Waterdraer. Met ’n skynbare magnitude van 4,279 is dit met die blote oog sigbaar.[3] Volgens parallaksmetings deur die Hipparcos-sending is dit sowat 175 ligjare van die Son af.[3]
Die ster se spektrum stem ooreen met ’n sterreklassifikasie van B8V,[1] wat beteken dit moet ’n B-tipe hoofreeksster wees. Sy radius is 2,7 keer dié van die Son[5] en dit roteer vinnig, met ’n spoed van sowat 135 km/s.[7] ’n Infrarooisoektog in 2010 na metgeselle om die ster was onsuksesvol.[6]
Verwysings
[wysig | wysig bron]- ↑ 1,0 1,1 Houk, Nancy (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode: 1988mcts.book.....H.
- ↑ 2,0 2,1 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 3,0 3,1 3,2 3,3 3,4 Kozok, J. R. (September 1985), "Photometric observations of emission B-stars in the southern Milky Way", Astronomy and Astrophysics Supplement Series 61: 387–405, Bibcode: 1985A&AS...61..387K.
- ↑ 4,0 4,1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 5,0 5,1 5,2 Underhill, A. B. et al. (November 1979), "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars", Monthly Notices of the Royal Astronomical Society 189: 601–605, doi:10.1093/mnras/189.3.601, Bibcode: 1979MNRAS.189..601U.
- ↑ 6,0 6,1 Ehrenreich, D. et al. (November 2010), "Deep infrared imaging of close companions to austral A- and F-type stars", Astronomy and Astrophysics 523: A73, doi:10.1051/0004-6361/201014763, Bibcode: 2010A&A...523A..73E.
- ↑ 7,0 7,1 Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal 573 (1): 359–365, doi:10.1086/340590, Bibcode: 2002ApJ...573..359A.
- ↑ Wu, Yue et al. (Januarie 2011), "Coudé-feed stellar spectral library - atmospheric parameters", Astronomy and Astrophysics 525: A71, doi:10.1051/0004-6361/201015014, Bibcode: 2011A&A...525A..71W.
- ↑ Iota Aquarii by Simbad, besoek op 6 September 2020
Skakels
[wysig | wysig bron]
Hierdie artikel is in sy geheel of gedeeltelik uit die Engelse Wikipedia vertaal.
