36 Ursae Majoris

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Template:Short description

36 Ursae Majoris
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ursa Major
A
Right ascension Template:RA[1]
Declination Template:DEC[1]
Apparent magnitude (V) 4.82[2]
B
Right ascension Template:RA[3]
Declination Template:DEC[3]
Apparent magnitude (V) 8.86[4]
Characteristics
A
Evolutionary stage main sequence
Spectral type F8 V[5]
U−B Template:Engvar −0.01[2]
B−V Template:Engvar +0.52[2]
B
Evolutionary stage main sequence
Spectral type K7Ve[6]
B−V Template:Engvar +1.34[7]
Astrometry
A
Radial velocity (Rv)+8.57[1] km/s
Proper motion (μ) RA: −177.045[1] mas/yr
Dec.: −32.634[1] mas/yr
Parallax (π)77.2485±0.0805 mas[1]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)4.29[8]
B
Radial velocity (Rv)+8.67[3] km/s
Proper motion (μ) RA: −182.443[3] mas/yr
Dec.: −32.034[1] mas/yr
Parallax (π)77.4072±0.0182 mas[3]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)8.2[7]
Details
A
Mass1.10[1] Template:Solar mass
Radius1.17[1] Template:Solar radius
Luminosity1.69[1] Template:Solar luminosity
Surface gravity (log g)4.4.23[1] cgs
Temperature6,066[1] K
Metallicity [Fe/H]−0.09[9] dex
Rotational velocity (v sin i)1.50[9] km/s
Age4.0[1] Gyr
B
Mass0.626[4] Template:Solar mass
Radius0.648[4] Template:Solar radius
Luminosity0.10[10] Template:Solar luminosity
Surface gravity (log g)4.61[4] cgs
Temperature4,132[10] K
Metallicity [Fe/H]−0.08[10] dex
Rotational velocity (v sin i)9[11] km/s
Age5[12] Gyr
Other designations
Template:Odlist[5]
A: Template:Odlist[5]
B: Template:Odlist
Database references
SIMBADA
B

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36 Ursae Majoris is a double star[5] in the northern constellation of Ursa Major. With an apparent visual magnitude of 4.8, it can be seen with the naked eye in suitable dark skies. Based upon parallax measurements, this binary lies at a distance of Script error: No such module "convert". from Earth.

The brighter star of the two is a solar analog—meaning it has physical properties that make it similar to the Sun. It has 10% more mass and a radius 17% larger than the Sun, with an estimated age of four billion years. The spectrum of this star matches a stellar classification of F8 V, which indicates this is a main sequence star that is generating energy at its core through the nuclear fusion of hydrogen. The energy is being radiated into space from its outer envelope at an effective temperature of Script error: No such module "val".. This gives the star the characteristic yellow-white hue of an F-type star.[13]

The fainter of the two stars has an apparent magnitude 8.86 and shares a common proper motion witIts spectral type of K7Ve indicates it is a red dwarf. Its has a mass 60% of the Sun's, a temperature of Script error: No such module "val". and a bolometric luminosity only 10% of the Sun's.

36 Ursae Majoris has a second companion with a magnitude of 11.44 located at an angular separation of 240.6″ along a position angle of 292°, as of 2004.[14] It does not share the proper motion of the other two stars and is a more massive and luminous star but much further away.[15]

Hunt for substellar objects

Script error: No such module "anchor". According to Nelson & Angel (1998),[16] 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)[17] 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[18] 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 yet been detected or confirmed. The McDonald Observatory team has set limits to the presence of one or more planets[19] with masses between 0.13 and 2.5 Jupiter masses and average separations spanning between 0.05 and 5.2 AU.

An infrared excess has been detected around this star, most likely indicating the presence of a circumstellar disk at a radius of 38.6 AU. The temperature of this dust is Script error: No such module "val"..[20]

References

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  1. ↑ a b c d e f g h i j k l m Template:Cite Gaia DR3
  2. ↑ a b c Script error: No such module "citation/CS1".
  3. ↑ a b c d e Template:Cite Gaia DR3
  4. ↑ a b c d Script error: No such module "citation/CS1".
  5. ↑ a b c d Script error: No such module "citation/CS1".
  6. ↑ Script error: No such module "citation/CS1".
  7. ↑ a b Script error: No such module "citation/CS1".
  8. ↑ Script error: No such module "citation/CS1".
  9. ↑ a b Script error: No such module "citation/CS1".
  10. ↑ a b c Script error: No such module "citation/CS1".
  11. ↑ Script error: No such module "citation/CS1".
  12. ↑ Script error: No such module "citation/CS1".
  13. ↑ Script error: No such module "citation/CS1".
  14. ↑ Script error: No such module "citation/CS1".
  15. ↑ Template:Cite Gaia DR3
  16. ↑ Script error: No such module "citation/CS1".
  17. ↑ Script error: No such module "citation/CS1".
  18. ↑ Script error: No such module "citation/CS1".
  19. ↑ Script error: No such module "citation/CS1".
  20. ↑ Script error: No such module "Citation/CS1".

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External links

Template:Stars of Ursa Major

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