Chromospherically active stars. XVII. The double-lined binary 54 Camelopardalis (AE Lyncis)

被引:4
|
作者
Fekel, FC
Eitter, JJ
De Medeiros, JR
Kirkpatrick, JD
机构
[1] Tennessee State Univ, Ctr Automated Space Sci, Nashville, TN 37203 USA
[2] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37203 USA
[3] NASA, George C Marshall Space Flight Ctr, Space Sci Lab, Huntsville, AL 35812 USA
[4] Iowa State Univ, Erwin W Fick Observ, Ames, IA 50011 USA
[5] Univ Fed Rio Grande Norte, Dept Fis, BR-59072970 Natal, RN, Brazil
[6] CALTECH, Jet Prop Lab, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA
来源
ASTRONOMICAL JOURNAL | 1998年 / 115卷 / 03期
关键词
binaries; spectroscopic; stars; chromospheres;
D O I
10.1086/300260
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
New spectroscopic observations of the double-lined chromospherically active binary 54 Camelopardalis (=AE Lyncis) have been obtained, resulting in improved orbital elements and the determination of the fundamental properties of the system. 54 Cam has a period of 11.06794 days, an eccentricity of 0.125, and a mass ratio of 0.9945. The spectral types are F8 IV-V and G5 IV, positioning the components on opposite sides of the Hertzsprung gap. From a comparison with theoretical evolutionary tracks, the masses are estimated to be 1.60 and 1.59 M. for the G and F stars, respectively, while the radii are 3.7 and 3.2 R.. Only the G star is chromospherically active. 54 Cam is particularly interesting since the F star is the brighter star at blue and red wavelengths, but the G star is slightly more massive and evolved. Both stars appear to be pseudosynchronously rotating, and the orbital and rotational inclinations are aligned. The lithium abundances of the two components are significantly different but consistent with standard theory, supporting the conclusion that both stars are more massive than the lithium-dip stars.
引用
收藏
页码:1153 / 1159
页数:7
相关论文
共 27 条
  • [1] Chromospherically active stars. XXV. HD 144110=EV Draconis, a double-lined dwarf binary
    Fekel, FC
    Henry, GW
    Lewis, C
    ASTRONOMICAL JOURNAL, 2005, 130 (02): : 794 - 798
  • [2] Chromospherically active stars .16. The double-lined binary 42 Capricorni
    Fekel, FC
    ASTRONOMICAL JOURNAL, 1997, 114 (06): : 2747 - 2752
  • [3] CHROMOSPHERICALLY ACTIVE STARS .13. HD-30957 - A DOUBLE-LINED K DWARF BINARY
    FEKEL, FC
    DADONAS, V
    SPERAUSKAS, J
    VACCARO, TR
    PATTERSON, LR
    ASTRONOMICAL JOURNAL, 1994, 108 (05): : 1936 - 1939
  • [4] CHROMOSPHERICALLY ACTIVE STARS .5. HD 91816 = LR HYA - A DOUBLE-LINED BY DRACONIS TYPE BINARY
    FEKEL, FC
    GILLIES, K
    AFRICANO, J
    QUIGLEY, R
    ASTRONOMICAL JOURNAL, 1988, 96 (04): : 1426 - 1430
  • [5] Chromospherically active stars. XX. The giant single-lined binary HD 161570
    Fekel, FC
    Henry, GW
    Henry, SM
    ASTRONOMICAL JOURNAL, 2001, 122 (06): : 3447 - 3452
  • [6] CHROMOSPHERICALLY ACTIVE STARS .12. ADS 11060-C - A DOUBLE-LINED K-DWARF BINARY IN A QUINTUPLE SYSTEM
    FEKEL, FC
    HENRY, GW
    HAMPTON, ML
    FRIED, R
    MORTON, MD
    ASTRONOMICAL JOURNAL, 1994, 108 (02): : 694 - 700
  • [7] DOUBLE-LINED SPECTROSCOPIC BINARY STARS IN THE RAVE SURVEY
    Matijevic, G.
    Zwitter, T.
    Munari, U.
    Bienayme, O.
    Binney, J.
    Bland-Hawthorn, J.
    Boeche, C.
    Campbell, R.
    Freeman, K. C.
    Gibson, B.
    Gilmore, G.
    Grebel, E. K.
    Helmi, A.
    Navarro, J. F.
    Parker, Q. A.
    Seabroke, G. M.
    Siebert, A.
    Siviero, A.
    Steinmetz, M.
    Watson, F. G.
    Williams, M.
    Wyse, R. F. G.
    ASTRONOMICAL JOURNAL, 2010, 140 (01): : 184 - 195
  • [8] Spectroscopic Orbits of Subsystems in Multiple Stars. IV. Double-lined Pairs
    Tokovinin, Andrei
    ASTRONOMICAL JOURNAL, 2018, 156 (05):
  • [9] Chromospherically active stars. XXVI. the doubled-lined late-type binary HD 19485=WZ arietis
    Fekel, Francis C.
    Bolton, C. T.
    ASTRONOMICAL JOURNAL, 2007, 134 (05): : 2079 - 2085
  • [10] Chromospherically active stars. XXII. HD 18955, a massive K dwarf binary
    Fekel, FC
    Henry, GW
    Alston, FM
    ASTRONOMICAL JOURNAL, 2004, 127 (04): : 2303 - 2309