Chi Cassiopeiae

χ Cassiopeiae
Description de l'image Chi Cassiopeiae.jpg.
Données d'observation
(époque J2000.0)
Ascension droite 01h 25m 56,022s[1]
Déclinaison +68° 07′ 48,05″[1]
Constellation Cassiopée
Magnitude apparente +4,696[2]

Localisation dans la constellation : Cassiopée

(Voir situation dans la constellation : Cassiopée)
Caractéristiques
Type spectral G9 IIIb[3]
Indice U-B +0,762[2]
Indice B-V +0,997[2]
Astrométrie
Vitesse radiale +6,66 ± 0,14 km/s[4]
Mouvement propre μα = −43,03 mas/a[1]
μδ = −22,31 mas/a[1]
Parallaxe 15,67 ± 0,39 mas[1]
Distance 208 ± 5 al
(64 ± 2 pc)
Magnitude absolue +0,52[5]
Caractéristiques physiques
Masse 2,04 M[5]
Rayon 11,0 ± 0,8 R[3]
Gravité de surface (log g) 2,21[5]
Luminosité 67,6 L[5]
Température 4 746 K[5]
Métallicité [Fe/H] = −0,34[5]
Rotation 0,44 ± 0,45 km/s[6]
Âge 1,0 × 109 a[5]

Désignations

χ Cas, 39 Cas, HR 442, HD 9408, HIP 7294, BD+58°260, SAO 22397[7]

Chi Cassiopeiae (χ Cassiopeiae / χ Cas) est une étoile géante de la constellation boréale de Cassiopée. Elle est visible à l'œil nu avec une magnitude apparente de 4,70[2]. L'étoile présente une parallaxe annuelle de 15,67 mas telle que mesurée par le satellite Hipparcos[1], ce qui permet d'en déduire qu'elle est distante d'environ ∼ 208 a.l. (∼ 63,8 pc) de la Terre. À cette distance, sa magnitude visuelle est diminuée de 0,18 en raison du facteur d'extinction créé par la poussière interstellaire présente sur le trajet de sa lumière[4]. L'étoile s'éloigne du Système solaire à une vitesse radiale héliocentrique de +6,7 km/s[4].

Chi Cassiopeiae est une géante jaune de type spectral G9 IIIb[3] dont l'âge est estimé à un milliard d'années[5]. Il s'agit d'une étoile du red clump, qui génère son énergie par la fusion de l'hélium dans son noyau[8]. L'étoile est environ deux fois plus massive que le Soleil[5] et son rayon s'est étendu jusqu'à ce qu'il devienne onze fois plus grand que le rayon solaire[3]. Elle est près de 68 fois plus lumineuse que le Soleil et sa température de surface est de 4 746 K[5].

Notes et références

  1. a b c d e et f (en) F. van Leeuwen, « Validation of the new Hipparcos reduction », Astronomy & Astrophysics, vol. 474, no 2,‎ , p. 653–664 (DOI 10.1051/0004-6361:20078357, Bibcode 2007A&A...474..653V, arXiv 0708.1752)
  2. a b c et d (en) P. A. Jennens et H. L. Helfer, « A new photometric metal abundance and luminosity calibration for field G and K giants », Monthly Notices of the Royal Astronomical Society, vol. 172, no 3,‎ , p. 667–679 (DOI 10.1093/mnras/172.3.667, Bibcode 1975MNRAS.172..667J)
  3. a b c et d (en) Tyler E. Nordgren et al., « Stellar Angular Diameters of Late-Type Giants and Supergiants Measured with the Navy Prototype Optical Interferometer », The Astronomical Journal, vol. 118, no 6,‎ , p. 3032–3038 (DOI 10.1086/301114, Bibcode 1999AJ....118.3032N, lire en ligne)
  4. a b et c (en) B. Famaey et al., « Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters », Astronomy & Astrophysics, vol. 430, no 1,‎ , p. 165–186 (DOI 10.1051/0004-6361:20041272, Bibcode 2005A&A...430..165F, arXiv astro-ph/0409579)
  5. a b c d e f g h i et j (en) Yoichi Takeda, Bun'ei Sato et Daisuke Murata, « Stellar Parameters and Elemental Abundances of Late-G Giants », Publications of the Astronomical Society of Japan, vol. 60, no 4,‎ , p. 781–802 (DOI 10.1093/pasj/60.4.781, Bibcode 2008PASJ...60..781T, arXiv 0805.2434)
  6. (en) E. Jofré et al., « Stellar parameters and chemical abundances of 223 evolved stars with and without planets », Astronomy & Astrophysics, vol. 574,‎ , p. 46, article no A50 (DOI 10.1051/0004-6361/201424474, Bibcode 2015A&A...574A..50J, arXiv 1410.6422)
  7. (en) * chi Cas -- Star sur la base de données Simbad du Centre de données astronomiques de Strasbourg.
  8. (en) M. Valentini et U. Munari, « A spectroscopic survey of faint, high-Galactic-latitude red clump stars. I. The high resolution sample », Astronomy & Astrophysics, vol. 522,‎ , A79 (DOI 10.1051/0004-6361/201014870, Bibcode 2010A&A...522A..79V, arXiv 1007.0207)

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