Quecksilber-Mangan-Stern

Quecksilber-Mangan-Sterne oder auch HgMn-Sterne sind blauweiße Sterne mit Besonderheiten im Spektrum ihres ausgestrahlten Lichts. Sie sind nahe verwandt mit den Ap-Sternen; beide Sternenklassen gehören zu den Chemisch-Pekuliären Sternen, den CP-Sternen.

Die HgMn-Sterne zeigen starke Überhäufigkeiten von Hg, Mn (Namensgebung), P, Ga, Br, Sr, Y, Zr, Rh, Pd, Xe, Pr, Yb, W, Re, Os, Pt und Au sowie ausgeprägte Unterhäufigkeiten von He, Al, Zn, Ni und Co. Der Spektraltyp der HgMn-Sterne ist ein spätes B.[1] Einige Elemente zeigen stark abweichende Isotopenverhältnisse, die aber sehr individuell für jeden Stern sind.

Die Quecksilber-Mangan-Sterne rotieren für ihre frühe Spektralklasse sehr langsam, mit einer durchschnittlichen – für die projizierte Bahnneigung korrigierten – Geschwindigkeit v∙sin i von bis zu 30 Kilometern pro Sekunde. Dabei fällt die Häufigkeit der HgMn-Sterne mit ansteigender Rotationsgeschwindigkeit stark ab.

Mehr als zwei Drittel aller Quecksilber-Mangan-Sterne gehören zu den spektroskopischen Doppelsternen mit Bahnperioden zwischen drei und zwanzig Tagen.

Auch bei den Quecksilber-Mangan-Sternen sind die Elemente auf der Sternoberfläche nicht gleichmäßig verteilt. Das Quecksilber liegt wahrscheinlich am Äquator konzentriert vor. Andere Elemente wie das Ti, Cr, Fe, Mn, Sr, Y, und Pt dagegen liegen eher wie bei den Ap-Sternen als Flecken irgendwo auf den Hemisphären der Sterne vor. Dies wird meist mit einem Magnetfeld auf der Oberfläche der Sterne in Verbindung gebracht. Die Quecksilber-Mangan-Sterne haben ausgesprochen schwache Magnetfelder mit Flussdichten von höchstens einigen Millitesla, während die magnetische Flussdichte bei den Ap-Sternen einige hundert Millitesla erreicht.[2]

Vertreter

Folgende Tabelle zeigt eine Auswahl von Vertretern dieser Sternenklasse nach ihrer scheinbaren Helligkeit:[3]

Name[4] Bayer oder Flamsteed-Bezeichnung Spektraltyp[4] scheinbare Helligkeit[4]
Elnath β Tauri B7 IIIp 1,6 mag
Alpheratz α Andromedae B8 IV-V 2,0 mag
Gienah Corvi γ Corvi B8 III 2,6 mag
μ Leporis B9 IV 3,3 mag
Maia 20 Tauri B8 III 3,9 mag
χ Lupi B9 IV 4,0 mag
Muliphein γ Canis Majoris B8 II 4,1 mag
φ Herculis B9 V 4,2 mag
π1 Bootis B9 IIIp 4,5 mag
υ Herculis B9 III 4,7 mag
ET Ursae Majoris A A0 sp 4,9 mag
ι Coronae Borealis B9 IIIp 5,0 mag
κ Cancri B8 IIIp 5,2 mag
112 Herculis A B9 II-IIIp 5,4 mag
ν Cancri A0 III 5,5 mag
53 Tauri B9 V 5,5 mag
κ2 Volantis B9/A0 IV 5,6 mag
28 Herculis B9,5 III 5,6 mag
14 Sagittae B9 mnp 5,6 mag
21 Pegasi B9,5 V 5,8 mag
Dabih Minor β2 Capricorni B9/A0 III-IV 6,1 mag

Siehe auch

Einzelnachweise

  1. ↑ O. Kochukhov, V. Makaganiuk, N. Piskunov, S. V. Jeffers, C. M. Johns-Krull, C. U. Keller, M. Rodenhuis, F. Snik, H. C. Stempels, J. A. Valenti: Are there tangled magnetic fields on HgMn stars? In: Astronomy & Astrophysics. Vol. 554, A61, 2013, doi:10.1051/0004-6361/201321467, S. 1–12, bibcode:2013A&A...554A..61K.
  2. ↑ S. Hubrig, J. F. Gonzalez, I. Ilyin, H. Korhonen, M. Schoeller, I. Savanov, R. Arlt, F. Castelli, G. Lo Curto, M. Briquet, T. H. Dall: Magnetic fields of HgMn stars. In: Astronomy & Astrophysics. Vol. 547, A90, 2012, doi:10.1051/0004-6361/201219778, S. 1–24, bibcode:2012A&A...547A..90H.
  3. ↑ K. Yüce, S. J. Adelmann: Elemental Abundance Analyses with DAO Spectrograms. XXXIV. A Three-Dimensional Graphical Examination of the Elemental Abundances of the Mercury-Manganese and Metallic-Line Stars. In: Publications of the Astronomical Society of the Pacific. Vol. 126, 2014, doi:10.1086/676335, S. 345–358 bibcode:2014PASP..126..345Y.
  4. ↑ a b c Angaben zu Name, Spektraltyp und Helligkeit aus SIMBAD.

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