Alpha Chamaeleontis
(Aangestuur vanaf Gliese 305)
Alpha Chamaeleontis (afgekort as α Cha) is die helderste ster in die suidelike sirkumpolêre sterrebeeld Kameleon (Chamaeleon). Dit het ’n skynbare magnitude van 4,06[3] en kan dus met die blote oog gesien word. Dit is 63,8 ligjare van die Son af.
Alpha Chamaeleontis
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| Alpha Chamaeleontis se posisie (in die rooi sirkel). | ||||
| Sterrebeeld | Kameleon | |||
| Spektraaltipe | F5 V Fe-0.8[1] | |||
| Soort | Hoofreeksster | |||
| Waarnemingsdata (Epog J2000) | ||||
| Regte klimming | 08h 18m 31.55319s[2] | |||
| Deklinasie | -76° 55′ 10.9964″[2] | |||
| Skynmagnitude (m) | 4,06[3] | |||
| Absolute magnitude (M) | +2,59[4] | |||
| B-V-kleurindeks | +0,40[3] | |||
| U-B-kleurindeks | -0,04[3] | |||
| Besonderhede | ||||
| Massa (M☉) | 1,42[5] | |||
| Ligsterkte (L☉) | 7,64[6] | |||
| Ouderdom (jaar) | 1,8 miljard[5] | |||
| Temperatuur (K) | 6 776[5] | |||
| Rotasiespoed (km/s) | 0[7] | |||
| Metaalinhoud [Fe/H] | -0,26[1] | |||
| Ander name | ||||
| α Cha, CPD−76° 507, Gliese 305, HD 71243, HIP 40702, HR 3318, SAO 256496 | ||||
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α Cha is ’n F-tipe hoofreeksster met ’n klassifikasie van F5 V Fe-0,8,[1] waar "Fe-0,8" ’n onreëlmatige lae voorkoms van yster aandui. Sy massa is 1,4 keer dié van die Son[5] en sy ligsterkte 7,64 keer[6] die Son s’n. Sy effektiewe temperatuur is 6 776 K.[5] Die ster is sowat 1,8 miljard jaar oud[5] en het ’n rotasiespoed wat te laag is om te meet.[7]
Verwysings
wysig- ↑ 1,0 1,1 1,2 Gray, R. O. et al. (2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal 132 (1): 161–70, doi:10.1086/504637, Bibcode: 2006AJ....132..161G.
- ↑ 2,0 2,1 van Leeuwen, F. (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- ↑ 3,0 3,1 3,2 3,3 Mermilliod, J.-C. (1986), Compilation of Eggen's UBV data, transformed to UBV (unpublished), SIMBAD, Bibcode: 1986EgUBV........0M.
- ↑ 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 5,3 5,4 5,5 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ 6,0 6,1 McDonald, I. et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society 427 (1): 343–57, doi:10.1111/j.1365-2966.2012.21873.x, Bibcode: 2012MNRAS.427..343M.
- ↑ 7,0 7,1 Uesugi, Akira; Fukuda, Ichiro (1970), "Catalogue of rotational velocities of the stars", Contributions from the Institute of Astrophysics and Kwasan Observatory (University of Kyoto), Bibcode: 1970crvs.book.....U.
Eksterne skakels
wysig
Hierdie artikel is vertaal uit die Engelse Wikipedia
