The two stellar components of this system have a
projected separation of about 152
AU, and an estimated orbital
semimajor axis of 190 AU.[17] The primary has about 48% of the
Sun's mass, while the secondary is only 10%.[10] The primary has a projected
rotation velocity at the
equator of less than 3 km/s; the secondary has a rotation velocity of 7.7±1.7 km/s.[14]
The primary star was monitored for
radial velocity (RV) variations caused by a
Jupiter-mass companion in a short-period orbit. It displayed no significant excess of RV variation that could be attributed to a planet.[18] A search of the system using near-infrared speckle interferometry also failed to detect a companion orbiting at distances of 1–10 AU.[19] Nor has a
brown dwarf been detected orbiting within this system.[20]
The
space velocity components of this system are U = 141, V = –7 and W = 7. They are members of the halo population of the
Milky Way galaxy.[14]
X-ray source
The secondary is a
flare star that is referred to as WX Ursae Majoris. It is characterized as a
UV Ceti-type variable star that displays infrequent increases in luminosity. This star was observed to flare as early as 1939 by the Dutch astronomer
Adriaan van Maanen.[21]
Component B (WX Ursae Majoris) has been identified as an
X-ray source, while no significant X-ray emission was detected from component A.[22] This system had not been studied in X-rays prior to
ROSAT.[22] The Gaia DR2 release gives a parallax of 204.059 ±0.169
mas for B, indicating a distance of around 16 light-years.[3]
^
abNicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Observatory.
Bibcode:
1978ppch.book.....N.
^Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto:
International Astronomical Union.
Bibcode:
1967IAUS...30...57E.
^
abcdDelfosse, Xavier; Forveille, Thierry; Perrier, Christian; Mayor, Michel (March 1998). "Rotation and chromospheric activity in field M dwarfs". Astronomy and Astrophysics. 331: 581–595.
Bibcode:
1998A&A...331..581D.
^Reid, I. Neill; Gizis, John E. (June 1997). "Low-Mass Binaries and the Stellar Luminosity Function". Astronomical Journal. 113: 2246–2269.
Bibcode:
1997AJ....113.2246R.
doi:
10.1086/118436.
^Leinert, C.; et al. (September 1997). "A search for companions to nearby southern M dwarfs with near-infrared speckle interferometry". Astronomy and Astrophysics. 325: 159–166.
Bibcode:
1997A&A...325..159L.