The archetype line-profile variable ɛ 45 Persei is a spectroscopic triple system.

Details The archetype line-profile variable ɛ 45 Persei is a spectroscopic triple system. The archetype line-profile variable ɛ 45 Persei is a spectroscopic triple system.

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26as..110...59t&link_type=abstract

Astronomy and Astrophysics Supplement, v.110, p.59

Astronomy and Astrophysics

Astrophysics

25

Binaries: Visual, Binaries: Spectroscopic, Stars: Fundamental Parameters, Open Clusters: {Alpha} Per

Scientific paper

An analysis of 66 old and 651 recent electronic and photographic spectrograms of the archetype line-profile variable ɛ Per led to the following conclusions: 1) ɛ Per is the primary component of a binary system. There are radial-velocity variations with a full amplitude of ~30km/s with a period 14.076d which can be traced back to old Allegheny observations from 1907-1912. The orbit is not circular but has a high eccentricity of 0.540+/-0.045. 2) The 14-d binary system probably moves in orbit with a distant, as yet unknown third star (which is not identical to the visual component ADS 2888B). A likely period is 4156d which then leads to an eccentric orbit with e=0.40+/-0.26 but several longer periods are also possible. The existence of the putative third component to ɛ Per could easily be checked by speckle-interferometric observations since its expected angular distance from the close pair in the sky does not decrease below =~0.04" even at periastron (for the shortest of the possible periods). 3) Some basic physical elements of the component stars and system dimensions were estimated as follows: primary: mass (13.5+/-2)Msun_ , radius (6.9+/-0.2)Rsun_, B0.5IV-III, T_eff_=(27600+/-1000)K, log g =3.85+/-0.15[CGS], He/H=0.23, logɛ(O)=8.89, logɛ(Si)=7.51; secondary: mass between 1 and 2Msun_; tertiary: mass between 2.3 and 5.3Msun_. The semimajor axis of the 14-d orbit is about 60Rsun_, that for the wide orbit 2800Rsun_ or more (depending on what is the correct value of the period). The data presented here make the membership of ɛ Per in the α Per cluster very improbable.

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