S Orionis

S Orionis
Data pengamatan
Epos J2000      Ekuinoks J2000
Rasi bintang Orion
Asensio rekta  05j 29m 00.8948d[1]
Deklinasi   -04° 41′ 32.748″[1]
Magnitudo tampak (V) 7.2 – 14.0[2]
Ciri-ciri
Tahap evolusi AGB[3]
Kelas spektrum M6.5e – M9.5e[2]
Indeks warna U−B +0.15[4]
Indeks warna B−V +1.73[4]
Jenis variabel Mira[2]
Astrometri
Gerak diri (μ) RA: 14.77[1] mdb/thn
Dek.: -10.87[1] mdb/thn
Paralaks (π)0,89±2,08[1] mdb
Jarak480 ± 120[3] pc
Detail
Radius411 – 498[3] R☉
Luminositas12,474[5] L☉
Suhu2,950[6] K
Penamaan lain
S Ori, BD−04°1146, HD 36090, SAO 132163, HIP 25673
Referensi basis data
SIMBADdata

S Orionis adalah bintang cabang raksasa asimtotik di rasi bintang Orion, berjarak sekitar 480 parsec (1.600 tahun cahaya). Bintang ini memiliki kecerahan yang bervariasi dan tingkat paling cerah berkekuatan 7,2 dan terjadi setiap 14 setiap 14 bulan.[7]

Referensi

  1. ^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  2. ^ a b c Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. ^ a b c Wittkowski, M.; Boboltz, D. A.; Ohnaka, K.; Driebe, T.; Scholz, M. (2007). "The Mira variable S Orionis: Relationships between the photosphere, molecular layer, dust shell, and SiO maser shell at 4 epochs". Astronomy and Astrophysics. 470 (1): 191–210. arXiv:0705.4614. Bibcode:2007A&A...470..191W. doi:10.1051/0004-6361:20077168. S2CID 14200520.
  4. ^ a b Celis s., L. (1982). "Red variable stars. I - UBVRI photometry and photometric properties". Astronomical Journal. 87: 1791. Bibcode:1982AJ.....87.1791C. doi:10.1086/113268.
  5. ^ Uttenthaler, S.; Stiphout, K. V.; Voet, K.; Winckel, H. V.; Eck, S. V.; Jorissen, A.; Kerschbaum, F.; Raskin, G.; Prins, S. (2011). "The evolutionary state of Miras with changing pulsation periods". doi:10.1051/0004-6361/201116463.
  6. ^ Hamsten, Bengt; Stangl, Gerhard; Uttenthaler, Josef (2002-09). "Development trends for buses by MAN and Neoplan". ATZ worldwide. 104 (9): 7–11. doi:10.1007/bf03225177. ISSN 2192-9076.
  7. ^ Templeton, M. R.; Mattei, J. A.; Willson, L. A. (2005-08). "Secular Evolution in Mira Variable Pulsations". The Astronomical Journal. 130 (2): 776–788. doi:10.1086/431740. ISSN 0004-6256.


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