65 Ursae Majoris is a sextuple star system. It contains six stars in a hierarchical orbit where each star orbits its inner stars. Such systems are uncommon, with only a few sextuple stars known.[5] Higher-multiplicity star systems are uncommon because they are less stable than their simpler counterparts, and often decay into smaller systems.
Multiplicity
Aa1
Period = 1.73d a = 0.2 mas
Aa2
Period = 641d a = 11 mas
Ab
Period = 118y a = 0.18″
B
3.4″ separation
C
63″ separation
D
Hierarchy of orbits in the 65 Ursae Majoris system
The central pair of stars, 65 Ursae Majoris Aa1 and Aa2, are both A-typemain-sequence stars. These are relatively bright, white-colored stars that typically have masses from 1.6 M☉ to 2.4 M☉.[12] They have relatively low masses for A-type main sequence stars and have spectral types of A7V.[5] Its orbital period is 1.73 days.[5]
The innermost binary pair 65 Ursae Majoris Aa is orbited by another star, designated 65 Ursae Majoris Ab. It is a spectroscopic binary: while the pair cannot be resolved, periodic Doppler shifts in their spectra indicate that there must be orbital motion. 65 Ursae Majoris Ab orbits the inner pair with a period of 641 days (1.76 years) and an eccentricity of 0.169.[5]
65 Ursae Majoris B orbits the three inner stars every 118 years. It is separated from the triple by 0.18″, and an astrometric orbit has been calculated. 65 Ursae Majoris C and D are common proper motion companions and are separated 4″ and 63″ respectively from the central system.[5] 65 Ursae Majoris D also appears to be a chemically peculiar star with higher amounts of chromium, strontium, and europium than normal.[13] Because of its unusual composition, determination of its stellar parameters is difficult; the effective temperature of this star may be 9,300 or 9,500 K, with the radius and the surface gravity determined for the star dependent on the effective temperature.[6]Speckle interferometry results have resolved 65 Ursae Majoris D into two components separated by 138 mas but this has not been confirmed by other observers. The two stars resolved differ in brightness by about two magnitudes.[14] An orbit for two stars has been estimated to have a period of about 79 years.[3]
65 Ursae Majoris A is a variable star with the variable star designationDN Ursae Majoris. The pair Aa1 and Aa2 form an eclipsing binary as they periodically pass in front of each other while orbiting. The primary and secondary eclipses are almost identical and the apparent magnitude of the system varies between 6.55 and 6.65 twice during each orbit of 1.73 days.[16] The brightness variation is very small because the non-eclipsing component Ab is the brightest of the three stars and contributes 80% of the visible light.[5]
Distance
Trigonometric parallax measurements made by the Hipparcosspacecraft put the 65 Ursae Majoris ABC system at a distance of about 690 light years (210 parsecs), and component D at about 1,000 light years (300 parsecs).[1] The dynamical parallax determined from the calculated orbits of the stars gives a distance of 763 ± 95 light-years (234 ± 29 pc).[5]Gaia has published measurements for the AB system and for component D, but they are both highly uncertain. Gaia Early Data Release 3 includes a somewhat more reliable measurement for the parallax of component C at 4.3897±0.0245 mas,[17] implying a distance of about 740 light years.[18]
See also
Castor, another multiple star system with six stars
Zeta Phoenicis, a multiple star system including an eclipsing binary
^Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
^Kharchenko, N. V.; et al. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889. arXiv:0705.0878. Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776. S2CID119323941.
^Gomez, A. E.; Luri, X.; Grenier, S.; Figueras, F.; North, P.; Royer, F.; Torra, J.; Mennessier, M. O. (1998). "The HR-diagram from HIPPARCOS data. Absolute magnitudes and kinematics of BP - AP stars". Astronomy and Astrophysics. 336: 953. Bibcode:1998A&A...336..953G.
^Balega, Yu. Yu; Dyachenko, V. V.; Maksimov, A. F.; Malogolovets, E. V.; Rastegaev, D. A.; Romanyuk, I. I. (2012). "Speckle interferometry of magnetic stars with the BTA. I. First results". Astrophysical Bulletin. 67 (1): 44. Bibcode:2012AstBu..67...44B. doi:10.1134/S199034131201004X. S2CID122554107.
^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.
