Mu Cephei

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μ Cephei
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cepheus
Right ascension Template:RA[1]
Declination Template:DEC[1]
Apparent magnitude (V) 3.43–5.1[2]
Characteristics
Evolutionary stage Red supergiant[3] or red hypergiant[4]
Spectral type M2-Ia[3] (M2e Ia[5] or M2 Ia+[4])
U−B color index +2.42[6]
B−V color index +2.35[6]
Variable type SRc[2]
Astrometry
Radial velocity (Rv)+20.63[7] km/s
Proper motion (μ) RA: 3.439 mas/yr[1]
Dec.: −4.108 mas/yr[1]
Parallax (π)0.55±0.20 mas[8]
Distance2,090 – 3,060 ly
(641+148
−144[9]–940+140
−40[10] pc)
Absolute magnitude (MV)–7.63[11]
Details
Mass25[12] M☉
Radius972±228[9] or 1,259[13] – 1,420[11] R☉
Luminosity269,000+111,000
−40,000[10] (135,000[9] – 340,000[11]) L☉
Surface gravity (log g)–0.36[13][12] cgs
Temperature3,750[13] K
Age10.0±0.1[14] Myr
Other designations
Template:Odlist[15]
Database references
SIMBADdata

Mu Cephei is a red supergiant or hypergiant star in the northern constellation Cepheus. It is officially named the Garnet Star;[16] Mu Cephei is its Bayer designation, which is Latinized from μ Cephei and abbreviated Mu Cep or μ Cep. This star appears garnet red and is located at the edge of the IC 1396 nebula. It is a 4th magnitude star easily visible to the naked eye under good observing conditions. Since 1943, the spectrum of this star has served as a spectral standard by which other stars are classified.

Mu Cephei is more than 100,000 times brighter than the Sun, with an absolute visual magnitude of −7.6. It is one of the largest known stars and also one of the most luminous and massive of its kind, with a radius around or over 1,000 times that of the Sun (R☉), and were it placed in the Sun's position, it would engulf the orbits of Mars and Jupiter.

History

File:Granatstern.webm
Zooming to the μ Cep (Garnet star) in the constellation Cepheus.

The deep red color of Mu Cephei was noted by William Herschel, who described it as "a very fine deep garnet colour, such as the periodical star ο Ceti".[17] It is thus commonly known as Herschel's "Garnet Star".[18] Mu Cephei was called Garnet sidus by Giuseppe Piazzi in his catalogue.[19][20] An alternative name, Erakis, used in Antonín Bečvář's star catalogue, is probably due to confusion with Mu Draconis, which was previously called Script error: No such module "lang". Script error: No such module "IPA". in Arabic.[21] The IAU Working Group on Star Names approved the name Garnet Star for Mu Cephei on 19 September 2024 and it is now so entered in the IAU Catalog of Star Names.[16]

In 1848, English astronomer John Russell Hind discovered that Mu Cephei was variable. This variability was quickly confirmed by German astronomer Friedrich Wilhelm Argelander. Almost continual records of the star's variability have been maintained since 1881.[22]

The angular diameter of μ Cephei has been measured interferometrically. One of the most recent measurements gives a diameter of 18.672±0.435 mas at 800 μm, modelled as a limb-darkened disk 20.584±0.480 mas across.[23] However, this later turned out to be the surrounding molecular layer and not the actual star, as the star has an angular diameter of 14.11±0.6 mas.[24] μ Cephei was used as one of the original "dagger stars", those with well-defined spectra that could be used for the classification of other stars, for MK spectral classifications. In 1943 it was the standard star for M2  Ia, updated in 1980 to be the standard star for the new type M2- Ia.[3][25]

Distance

File:MuCephei.jpg
Mu Cephei (circled) as can be seen in binoculars. The bright star on the right is Alderamin (Alpha Cephei).
File:IC 1396 rev 20140921 s (18237481073).jpg
IC 1396 with μ Cephei towards the top (north)

The distance to Mu Cephei is not very well known. The Hipparcos satellite was used to measure a parallax of 0.55±0.20 mas, which corresponds to an estimated distance of 1,800 parsecs. However, this value is close to the margin of error. A determination of the distance based upon a size comparison with Betelgeuse gives an estimate of 390±140 parsecs.[26]

Calculation of the distance from the measured angular diameter, surface brightness, and calculated luminosity leads to 641 pc.[9] Averaging the distances of nearby luminous stars with similar reddening and reliable Gaia Data Release 2 parallaxes gives a distance of 940 pc.[10]

Surroundings

Mu Cephei is surrounded by a shell extending out to a distance at least equal to 0.33 times the star's radius with a temperature of 2,055±25 K. This outer shell appears to contain molecular gases such as CO, H2O, and SiO.[26] Infrared observations suggest the presence of a wide ring of dust and water with an inner radius about twice that of the star itself, extending to about four times the radius of the star.[27][28]

The star is surrounded by a spherical shell of ejected material that extends outward to an angular distance of 6″ with an expansion velocity of 10 km s−1. This indicates an age of about 2,000–3,000 years for the shell. Closer to the star, this material shows a pronounced asymmetry, which may be shaped as a torus.[citation needed]

Variability

File:MuCepLightCurve.png
A visual band light curve for Mu Cephei, adapted from Brelstaff et al. (1997)[22]

Mu Cephei is a variable star and the prototype of the obsolete class of the Mu Cephei variables. It is now considered to be a semiregular variable of type SRc. Its apparent brightness varies erratically between magnitude 3.4 and 5.1. Many different periods have been reported, but they are consistently near 860 days or 4,400 days.[29]

Properties

Size comparison of μ Cephei and the Sun

A very luminous red supergiant, Mu Cephei is among the largest stars visible to the naked eye, and one of the largest known cool supergiants. It is a runaway star with a peculiar velocity of 80.7±17.7 km/s,[14] and has been described as a hypergiant.[30][31]

The bolometric luminosity, summed over all wavelengths, is calculated from integrating the spectral energy distribution (SED) to be 269,000 L☉, making μ Cephei one of the most luminous red supergiants in the Milky Way.[10] Its effective temperature of 3,750 K, determined from colour index relations, implies a radius of 1,259 R☉.[13] Other recent publications give similar effective temperatures. Calculation of the luminosity from a visual and infrared colour relation give 340,000 L☉ and a corresponding radius of 1,420 R☉.[11] An estimate made based on its angular diameter and an assumed distance of 2,400 light years gives it a radius of 1,650 R☉,[32] however the angular diameter used later turned out to be the diameter of the molecular layer around the star.[24]

The radius has been estimated to be 830 R☉ in 2010 based on the star's effective temperature of 3,660 K and the 111,200 L☉ luminosity estimate.[33]

A 2019 paper measurement based on the 641+148
−144 pc distance gives the star a luminosity below 140,000 L☉ and a correspondingly radius of 972±228 R☉, and as well as a lower temperature of 3,551±136 K. These parameters are all consistent with those estimated for Betelgeuse.[9]

The initial mass of Mu Cephei has been estimated from its position relative to theoretical stellar evolutionary tracks to be between 15 M☉ and 25 M☉.[9][13] The star currently has a mass loss rate of (4.9±1.0)×10−7 M☉ per year.[9]

Supernova

Mu Cephei is nearing death. It has begun to fuse helium into carbon, whereas a main sequence star fuses hydrogen into helium. When a supergiant star has converted elements in its core to iron, the core collapses to produce a supernova and the star is destroyed, leaving behind a vast gaseous cloud and a small, dense remnant. For a star as massive as Mu Cephei, the remnant is likely to be a black hole. The most massive red supergiants will evolve back to blue supergiants, Luminous blue variables, or Wolf-Rayet stars before their cores collapse, and Mu Cephei appears to be massive enough for this to happen. A post-red supergiant will produce a type IIn or type II-b supernova, while a Wolf–Rayet star will produce a type Ib or Ic supernova.[34]

Components

There are several faint stars within two arc-minutes of Mu Cephei and listed in multiple star catalogues (eg. WDS J21435+5847 and CCDM J21435+5847).[35]

Component Right ascension Declination Apparent magnitude Database reference
B Template:RA Template:DEC 12.3 Gaia DR3
C Template:RA Template:DEC 12.7 Simbad
D Template:RA Template:DEC 13.0 Gaia DR3
E Template:RA Template:DEC 13.0 Gaia DR3
F Template:RA Template:DEC 13.0 Gaia DR3
G Template:RA Template:DEC 11.0 Simbad

See also

References

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  5. ^ Page Module:Citation/CS1/styles.css has no content.Shenavrin, V. I.; et al. (2011). "Search for and study of hot circumstellar dust envelopes". Astronomy Reports. 55 (1): 31. Bibcode:2011ARep...55...31S. doi:10.1134/S1063772911010070. S2CID 122700080.
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