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36 Ursae Majoris: Wikis


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36 Ursae Majoris
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ursa Major
Right ascension 10h 30m 37.5798s
Declination +55° 58' 49.931"
Apparent magnitude (V) 3.41
Spectral type F8V
Distance 41.89 ly
(12.85 pc)
Absolute magnitude (MV) 2.63
Mass ≈1 M
Radius 1.12 R
Luminosity 1.6 L
Temperature 6126 [1] K
Age ≈2.7x109 [1] years
Other designations
36 Ursae Majoris, HD 90839, HR 4112, SAO 27670, FK5 394, BD +56 1459, HIP 51459

36 Ursae Majoris is a yellowish main sequence star of spectral type F8V. The star is 1.2 times more massive than Sun and has a 1.2 times larger radius. Its age is around 2 billion years.

The star is thought to have a stellar companion B of spectral type K7V at wide separation (1500 AUs). An optical companion C (spectral type K2V) is located at 49,000 Astronomical Units, but it's likely not bound to the system.

Hunt for substellar objects

According to Nelson & Angel (1998)[2], 36 Ursae Majoris could host one or two (or at least three) jovian planets (or even brown dwarfs) at wide separations from the host star, with orbital periods of 10-15, 25 and 50 years respectively. The authors have set upper limits of 1.1-2, 5.3 and 24 Jupiter masses for the putative planetary objects. Also Lippincott (1983)[3] had previously noticed the possible presence of a massive unseen companion (with nearly 70 times the mass of Jupiter, just below the stellar regime, thus a brown dwarf). Putative parameters for the substellar object show an orbital period of 18 years and quite a high eccentricity (e=0.8). Even Campbell et al. 1988[4] inferred the existence of planetary objects or even brown dwarfs less massive than 14 Jupiter masses around 36 Ursae Majoris. Nevertheless no certain planetary companion has still been detected or confirmed. McDonald Observatory team has set limits to the presence of one or more planets [5] with masses between 0.13 and 2.5 Jupiter masses and average separations spanning between 0.05 and 5.2 Astronomical Units.


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