Omega Cassiopeiae

ω Cassiopeiae
Données d'observation
(époque J2000.0)
Ascension droite 01h 56m 00,02830s[1]
Déclinaison +68° 41′ 06,8639″[1]
Constellation Cassiopée
Magnitude apparente +4,99[2]

Localisation dans la constellation : Cassiopée

(Voir situation dans la constellation : Cassiopée)
Caractéristiques
Type spectral B5III[3]
Indice U-B −0,41[4]
Indice B-V −0,09[4]
Variabilité suspectée[5]
Astrométrie
Vitesse radiale −24,8 ± 4,2 km/s[6]
Mouvement propre μα = +15,067 mas/a[1]
μδ = −10,313 mas/a[1]
Parallaxe 4,480 2 ± 0,091 2 mas[1]
Distance 223,204 ± 4,544 pc (∼728 al)[1]
Magnitude absolue +0,09[7]
Caractéristiques physiques
Masse 3,5 M[8]
Rayon 2,7 R[8]
Gravité de surface (log g) 4,1[8]
Luminosité 178 L[8]
Température 12 737 ± 100 K[9]
Rotation 45,7 km/s[10]
Âge 232 × 106 a[7]
Orbite
Compagnon ω Cas[11]
Excentricité (e) 0,30
Période (P) 69,92 j
Argument du périastre (ω) 50°
Époque du périastre (τ) 2 420 426,02 JJ

Désignations

NSV 659, ω Cas, 46 Cas, HR 548, HD 11529, HIP 9009, BD+67°169, FK5 2129, SAO 12038[12]

Omega Cassiopeiae (ω Cassiopeiae / ω Cas) est une étoile binaire de la constellation boréale de Cassiopée. Elle est visible à l'œil nu avec une magnitude apparente combinée de 4,99[2]. Le système présente une parallaxe annuelle de 4,48 mas telle que mesurée par le satellite Gaia, ce qui permet d'en déduire qu'il est distant d'environ 223 pc (∼727 al) de la Terre[1]. À cette distance, sa magnitude visuelle est diminuée de 0,16 en raison du facteur d'extinction créé par la poussière interstellaire présente sur le trajet de sa lumière[7].

Omega Cassiopeiae est une binaire spectroscopique à raies simples qui complète une orbite avec une période de 69,92 jours et selon une excentricité de 0,30[11]. Sa composante visible est classée comme une géante bleue de type spectral B5III[3]. C'est une étoile pauvre en hélium, un type d'étoile chimiquement particulière qui montre des raies d'absorption anormalement faibles de l'hélium pour une étoile de cette température[13]. Elle est estimée être 3,5 fois plus massive que le Soleil et son rayon est 2,7 fois plus grand que le rayon solaire[8]. Elle est 178 fois plus lumineuse que le Soleil[8] et sa température de surface est de 12 737 K[9].

Notes et références

  1. a b c d e f et g (en) A. G. A. Brown et al. (Gaia collaboration), « Gaia Early Data Release 3 : Summary of the contents and survey properties », Astronomy & Astrophysics, vol. 649,‎ , article no A1 (DOI 10.1051/0004-6361/202039657, Bibcode 2021A&A...649A...1G, arXiv 2012.01533). Notice Gaia EDR3 pour cette source sur VizieR.
  2. a et b (en) P. P. Eggleton et A. A. Tokovinin, « A catalogue of multiplicity among bright stellar systems », Monthly Notices of the Royal Astronomical Society, vol. 389, no 2,‎ , p. 869–879 (DOI 10.1111/j.1365-2966.2008.13596.x, Bibcode 2008MNRAS.389..869E, arXiv 0806.2878)
  3. a et b (en) Gerard T. van Belle et Kaspar von Braun, « Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars », The Astrophysical Journal, vol. 694, no 2,‎ , p. 1085–1098 (DOI 10.1088/0004-637X/694/2/1085, Bibcode 2009ApJ...694.1085V, arXiv 0901.1206, S2CID 18370219)
  4. a et b (en) D. L. Crawford, « U, b, v, and Hβ Photometry for the Bright B8- and B9-TYPE Stars », The Astrophysical Journal, vol. 137,‎ , p. 530 (DOI 10.1086/147526, Bibcode 1963ApJ...137..530C)
  5. (en) N. N Samus', E. V. Kazarovets et al., « General Catalogue of Variable Stars: NSV and supplement », Astronomy Reports, vol. 61, no 1,‎ , p. 80 (DOI 10.1134/S1063772917010085, Bibcode 2017ARep...61...80S)
  6. (en) J. H. J. de Bruijne et A.-C. Eilers, « Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project », Astronomy & Astrophysics, vol. 546,‎ , p. 14, article no A61 (DOI 10.1051/0004-6361/201219219, Bibcode 2012A&A...546A..61D, arXiv 1208.3048)
  7. a b et c (en) G. A. Gontcharov, « Spatial distribution and kinematics of OB stars », Astronomy Letters, vol. 38, no 11,‎ , p. 694–706 (DOI 10.1134/S1063773712110035, Bibcode 2012AstL...38..694G, arXiv 1606.09028, S2CID 119108982)
  8. a b c d e et f (en) Keivan G. Stassun et al., « The TESS Input Catalog and Candidate Target List », The Astronomical Journal, vol. 156,‎ , p. 102 (ISSN 0004-6256, DOI 10.3847/1538-3881/aad050, Bibcode 2018AJ....156..102S)
  9. a et b (en) Wenjin Huang, D. R. Gies et M. V. McSwain, « A Stellar Rotation Census of B Stars: From ZAMS to TAMS », The Astrophysical Journal, vol. 722, no 1,‎ , p. 605–619 (DOI 10.1088/0004-637X/722/1/605, Bibcode 2010ApJ...722..605H, arXiv 1008.1761, S2CID 118532653)
  10. (en) A. V. Moiseeva et al., « Fundamental Parameters of CP Stars Observed at the 6-m Telescope. I. Observations in 2009–2011 », Astrophysical Bulletin, vol. 74, no 1,‎ , p. 62–65 (DOI 10.1134/S1990341319010061, Bibcode 2019AstBu..74...62M, S2CID 149673065)
  11. a et b (en) D. Pourbaix et al., « SB9: The ninth catalogue of spectroscopic binary orbits », Astronomy & Astrophysics, vol. 424,‎ , p. 727-732 (DOI 10.1051/0004-6361:20041213, Bibcode 2004A&A...424..727P, arXiv astro-ph/0406573)
  12. (en) * ome Cas -- Spectroscopic Binary sur la base de données Simbad du Centre de données astronomiques de Strasbourg.
  13. (en) P. Renson et J. Manfroid, « Catalogue of Ap, HgMn and Am stars », Astronomy & Astrophysics, vol. 498, no 3,‎ , p. 961–966 (DOI 10.1051/0004-6361/200810788, Bibcode 2009A&A...498..961R, lire en ligne)

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