R Lyrae

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R Lyrae
File:Lyra constellation map.svg
R Lyrae (labelled as 13)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Lyra
Right ascension Template:RA[1]
Declination Template:DEC[1]
Apparent magnitude (V) 3.9 - 5.0[2]
Characteristics
Spectral type M5 III[3]
Apparent magnitude (J) −0.90[4]
U−B Template:Engvar +1.41[4]
B−V Template:Engvar +1.59[4]
Variable type SRb[2]
Astrometry
Radial velocity (Rv)−27.15[5] km/s
Proper motion (μ) RA: 21.05[1] mas/yr
Dec.: 82.06[1] mas/yr
Parallax (π)10.94±0.12 mas[1]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)−1.1[3]
Details
MassScript error: No such module "val".[6] Template:Solar mass
RadiusTemplate:Solar radius calculator[6]Template:Efn Template:Solar radius
Luminosity4,130[6]Template:Efn Template:Solar luminosity
Surface gravity (log g)0.47[7] cgs
Temperature3,313[6] K
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
R Lyrae, 13 Lyrae, HR 7157, BD+43°3117, HD 175865, SAO 47919, HIP 92862, GC 25996, GSC 03131-02155
Database references
SIMBADdata

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R Lyrae, also known as its Flamsteed designation 13 Lyrae, is a 4th magnitude semiregular variable star in the constellation Lyra, approximately 350 light years away from Earth. It is visible to the naked eye. It is a red giant star of the spectral type M5III, currently at the last stages of evolution. It is much larger and brighter, yet cooler, than the Sun. In the near-infrared J band, it is brighter than the nearby Vega.

R Lyrae is unusual in that it is a red star with a high proper motion, greater than 50 milliarcseconds a year.[8] It is one of the brightest stars at the K band, having an apparent magnitude of −2.08, only 14 stars are brighter.[9]

File:RLyrLightCurve.png
Visual band light curves for R Lyrae, adapted from Percy et al. (2001)[10]

In 1856, Joseph Baxendell announced that the star, then called 13 Lyrae, is a variable star.[11] In 1907 it appeared with its variable star designation, R Lyrae, in Annie Jump Cannon's Second Catalog of Variable Stars.[12] The variability is not consistent and regular, but periods of 46, 64, 378, and 1,000 days have been reported, with the 46-day period being the strongest.[3][13]

It is calculated that R Lyrae was a Template:Solar mass star on the main sequence, similar to Sirius A today. It is now an oxygen-rich asymptotic giant branch star, with both hydrogen and helium shells fusing. Due to stellar mass loss, R Lyrae now has a mass of Template:Solar mass.[6]

Notes

Template:Notelist

References

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  1. ↑ a b c d e Template:R:Van Leeuwen 2007 Validation of the new Hipparcos reduction
  2. ↑ a b Script error: No such module "citation/CS1".
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  6. ↑ a b c d e Script error: No such module "Citation/CS1".
  7. ↑ Script error: No such module "Citation/CS1".
  8. ↑ Script error: No such module "Citation/CS1".
  9. ↑ Kmag < -2.08. SIMBAD.
  10. ↑ 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".

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Template:Stars of Lyra

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