RR Ursae Minoris

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RR Ursae Minoris
File:RRUMiLightCurve.png
A light curve for RR Ursae Minoris, plotted from Hipparcos data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Ursa Minor
Right ascension 14h 57m 35.00959s[2]
Declination +65° 55′ 56.8146″[2]
Apparent magnitude (V) 4.44 - 4.85[3]
Characteristics
Spectral type M5 III[4]
B−V color index 1.590±0.017[5]
Variable type SRb[6]
Astrometry
Radial velocity (Rv)6.21±0.30[7] km/s
Proper motion (μ) RA: −78.23 mas/yr[8]
Dec.: +32.5 mas/yr[8]
Parallax (π)7.1±0.37 mas[8]
Distance460 ± 20 ly
(141 ± 7 pc)
Absolute magnitude (MV)−1.11[5]
Orbit[9]
Period (P)748.9 d
Eccentricity (e)0.13±0.05
Inclination (i)79.6±2.4[10]°
Longitude of the node (Ω)48.0±2.5[10]°
Periastron epoch (T)2,444,419±46 JD
Argument of periastron (ω)
(secondary)		212±22°
Semi-amplitude (K1)
(primary)		8.3±0.3 km/s
Details
Mass1.15±0.1[11] M☉
Radius113.93+5.4
−5.97[12] R☉
Luminosity1,583±172[12] L☉
Surface gravity (log g)0.00[13] cgs
Temperature3,410±37[12] K
Other designations
AAVSO 1456+66, Tau Ursae Minoris (τ UMi) [14], RR UMi, BD+66°878, FK5 554, HD 132813, HIP 73199, HR 5589, SAO 16558[2]
Database references
SIMBADdata

RR Ursae Minoris, abbreviated RR UMi, is a binary star[13] system in the northern circumpolar constellation of Ursa Minor. It can be viewed with the naked eye, typically having an apparent visual magnitude of around 4.710.[10] Based upon an annual parallax shift of 7.1 mas[8] as seen from Earth's orbit, it is located 460 light years away. The system is moving further from the Sun with a heliocentric radial velocity of +6 km/s.[7]

This star was found to have a variable radial velocity by J. H. Moore in 1910. It is a single-lined spectroscopic binary system with an orbital period of 2.05 years and an eccentricity (ovalness) of 0.13. The a sin i value is 84 Gm (0.56 AU),[9] where a is the semimajor axis and i is the orbital inclination to the line of sight from the Earth. This gives a lower bound on the physical size of the orbit. The system is a source for X-ray and far-UV emission, with the latter most likely coming from the companion.[13]

The visible component is an aging red giant star on the asymptotic giant branch[13] with a stellar classification of M4.5 III.[4] It was found to be a variable star by J. Ashbrook in 1946,[15] and is catalogued as a semiregular variable of subtype SRb[6] that ranges from magnitude 4.44 to 4.85 over a period of 43.3 days.[3] However, variations in the period have been observed on a time scale of 30–60 days.[16] The star has 1.15[11] times the mass of the Sun and has expanded to 110 times the Sun's radius. It is radiating 1,580 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,410 K.[12]

References

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  8. ^ a b c Lua error in Module:Citation/CS1/Configuration at line 2172: attempt to index field '?' (a nil value). RR UMi's database entry at VizieR.
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