Nu Cephei

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Template:Short description

ν Cephei
Template:Location mark
Location of ν Cephei (circled in red)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cepheus
Right ascension Template:RA[1]
Declination Template:DEC[1]
Apparent magnitude (V) 4.289[2] (4.25 - 4.35[3])
Characteristics
Evolutionary stage Blue supergiant[4]
Spectral type A2Iab[2]
Apparent magnitude (U) 4.94[5]
Apparent magnitude (B) 4.81[5]
Apparent magnitude (J) 3.14[5]
Apparent magnitude (K) 2.85[5]
U−B Template:Engvar +0.119[2]
B−V Template:Engvar +0.518[2]
Variable type Alpha Cygni[3]
Astrometry
Radial velocity (Rv)−25.90[6] km/s
Proper motion (μ) RA: −3.74 ± 0.13[1] mas/yr
Dec.: −2.10 ± 0.12[1] mas/yr
Parallax (π)0.48±0.14 mas[1]
Distance1,450[7] pc
Absolute magnitude (MV)−6.82[8]
Details
Mass15.4[7] Template:Solar mass
Radius137[7] Template:Solar radius
Luminosity102,000[7] Template:Solar luminosity
Surface gravity (log g)1.35[2] cgs
Temperature8,800[2] K
Rotational velocity (v sin i)15[2] km/s
Age8[4] Myr
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
10 Cephei, HD 207260, HR 8334, SAO 19624, FK5 1572, BD+60°2288, HIP 107418
Database references
SIMBADdata

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File:NuCepLightCurve.png
A light curve for Nu Cephei, plotted from TESS data,[9]

Nu Cephei (ν Cephei) is a class A2, fourth-magnitude blue supergiant star in the constellation Cepheus, visible to the naked eye. It is a white pulsating α Cygni variable star located about 4,700 light-years from Earth.

ν Cephei is a member of the Cepheus OB2 stellar association,[4] which includes stars such as μ Cephei and VV Cephei.[10] It began life as an approximately Template:Solar mass[7][4] star around eight million years ago. It has now exhausted its core hydrogen and expanded and cooled into a supergiant. Elemental abundance analyses indicate that it has not yet spent time as a red supergiant, which would have brought about convection of fusion products to the surface in a Dredge-up.[4]

ν Cephei is currently about 15 times as massive as the sun, 137 times as large, and 100,000 times as luminous.[7] Its large size and luminosity cause it to be somewhat unstable and produce irregular pulsations. This is a common feature of class A and B supergiants, which are grouped as α Cygni variable stars. Variability was first reported by Helmut Abt in 1957.[11] The brightness changes by at most a tenth of a magnitude.[3] A variety of values for the variability period have been published, including 5 to 10 days,[12] 7.6 days[13][11] and 90 days.[14]

References

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  4. ↑ a b c d e Script error: No such module "Citation/CS1".
  5. ↑ a b c d Script error: No such module "Citation/CS1".
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  7. ↑ a b c d e f Template:Cite thesis
  8. ↑ Script error: No such module "Citation/CS1".
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  10. ↑ Script error: No such module "Citation/CS1".
  11. ↑ a b 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".

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External links

Template:Stars of Cepheus

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