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Mu Cephei

Coordinates: Sky map 21h 43m 30.46s, +58° 46′ 48.2″
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Not to be confused with MY Cephei.
μ Cephei
Location of μ Cep (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cepheus
Right ascension 21h 43m 30.4609s[1]
Declination +58° 46′ 48.166″[1]
Apparent magnitude (V) +4.08[2] (3.43 - 5.1[3])
Characteristics
Evolutionary stage Red supergiant or hypergiant[4]
Spectral type M2-Ia[5] (M2e Ia[6] or M2 Ia+[7])
U−B color index +2.42[2]
B−V color index +2.35[2]
Variable type SRc[3]
Astrometry
Radial velocity (Rv)+20.63[8] km/s
Proper motion (μ) RA: 2.740±0.884[9] mas/yr
Dec.: −5.941±0.922[9] mas/yr
Parallax (π)0.55 ± 0.20 mas[10]
Distance2,090 – 3,060 ly
(641+148
−144[11]–940+140
−40[12] pc)
Absolute magnitude (MV)–7.63[13]
Details
Mass25[14] M☉
Radius972±228[11] or 1,259[15] – 1,420[13] R☉
Luminosity269,000+111,000
−40,000[12] (135,000[11] – 340,000[13]) L☉
Surface gravity (log g)–0.36[15][14] cgs
Temperature3,750[15] K
Age10.0±0.1[16] Myr
Other designations
Erakis, Herschel's Garnet Star, μ Cep, HD 206936, HR 8316, BD+58°2316, HIP 107259, SAO 33693
Database references
SIMBADdata

Mu Cephei (Latinized from μ Cephei, abbreviated Mu Cep or μ Cep), also known as Herschel's Garnet Star, Erakis, or HD 206936, is a red supergiant or hypergiant[4][7] star in the constellation Cepheus. It appears garnet red and is located at the edge of the IC 1396 nebula. 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 also one of the largest known stars 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 orbit of Mars and Jupiter.

History

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1785 portrait of William Herschel
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 al-Rāqis [arˈraːqis] in Arabic.[21]

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 diameer 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.[5][25]

Distance

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Mu Cephei (circled) as can be seen in binoculars. The bright star on the right is Alderamin (Alpha Cephei).
Mu Cephei and surrounding nebulosity, imaged at H-alpha and OIII wavelengths (north is towards top left)

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.[11] Averaging the distances of nearby luminous stars with similar reddening and reliable Gaia Data Release 2 parallaxes gives a distance of 940 pc.[12]

Surroundings

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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.

Variability

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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

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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,[16] and has been described as a hypergiant.[4]

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.[12] Its effective temperature of 3,750 K, determined from colour index relations, implies a radius of 1,259 R☉.[15] 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☉.[13] 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☉,[30] 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 3660 K and the 111,200 L☉ luminosity estimate.[31]

A 2019 paper measurement based on the 641+148
−144 pc distance gives the star a lower luminosity below 140,000 L☉ and a correspondingly lower 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.[11]

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☉.[11][15] The star currently has a mass loss rate of (4.9±1.0)×10−7 M☉ per year.[11]

Supernova

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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.[32]

Components

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There are several faint stars within two arc-minutes of Mu Cephei, and listed in multiple star catalogues.

NAME Right ascension Declination Apparent magnitude (V) Database references
μ Cep B (CCDM J21435+5847B) 21h 43m 27.8s +58° 46′ 45″ 12.3
μ Cep C (CCDM J21435+5847C) 21h 43m 25.6s +58° 47′ 08″ 12.7 Simbad

See also

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References

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  1. ^ a b Perryman, M. A. C.; et al. (April 1997). "The HIPPARCOS Catalogue". Astronomy and Astrophysics. 323: L49–L52. Bibcode:1997A&A...323L..49P.
  2. ^ a b c Nicolet, B. (October 1978). "Catalogue of homogeneous data in the UBV photoelectric photometric system". Astronomy & Astrophysics Supplement Series. 34: 1–49. Bibcode:1978A&AS...34....1N.
  3. ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  4. ^ a b c Shenoy, Dinesh; Humphreys, Roberta M; Terry Jay Jones; Marengo, Massimo; Gehrz, Robert D; Andrew Helton, L; Hoffmann, William F; Skemer, Andrew J; Hinz, Philip M (2015). "Searching for Cool Dust in the Mid-to-Far Infrared: The Mass Loss Histories of the Hypergiants μ Cep, VY CMa, IRC+10420, and ρ Cas". The Astronomical Journal. 151 (3): 51. arXiv:1512.01529. Bibcode:2016AJ....151...51S. doi:10.3847/0004-6256/151/3/51. S2CID 119281306.
  5. ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373. S2CID 123149047.
  6. ^ Shenavrin, V. I.; Taranova, O. G.; Nadzhip, A. E. (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.
  7. ^ a b Garrison, Robert F.; Kormendy, John (1976). "Some Characteristics of the Young Open Cluster Trumpler 37". Publications of the Astronomical Society of the Pacific. 88 (526): 865–869. Bibcode:1976PASP...88..865G. doi:10.1086/130037. ISSN 0004-6280. JSTOR 40676037.
  8. ^ Famaey, B.; et al. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430 (1): 165–186. arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID 17804304.
  9. ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
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  11. ^ a b c d e f g Montargès, M.; Homan, W.; Keller, D.; Clementel, N.; Shetye, S.; Decin, L.; Harper, G. M.; Royer, P.; Winters, J. M.; Le Bertre, T.; Richards, A. M. S. (2019). "NOEMA maps the CO J = 2 − 1 environment of the red supergiant μ Cep". Monthly Notices of the Royal Astronomical Society. 485 (2): 2417–2430. arXiv:1903.07129. Bibcode:2019MNRAS.485.2417M. doi:10.1093/mnras/stz397. S2CID 119423161.
  12. ^ a b c d Davies, Ben; Beasor, Emma R. (March 2020). "The 'red supergiant problem': the upper luminosity boundary of Type II supernova progenitors". MNRAS. 493 (1): 468–476. arXiv:2001.06020. Bibcode:2020MNRAS.493..468D. doi:10.1093/mnras/staa174. S2CID 210714093.
  13. ^ a b c d Table 4 in Emily M. Levesque; Philip Massey; K. A. G. Olsen; Bertrand Plez; Eric Josselin; Andre Maeder & Georges Meynet (2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. S2CID 15109583.
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  17. ^ Herschel, W. (1783). "Stars newly come to be visible". Philosophical Transactions: 257.
  18. ^ Allen, R. H. (1899). Star Names: Their Lore and Meaning. G. E. Stechert. p. 158. editions:CmkItwtawcMC.
  19. ^ Piazzi, G., ed. (1803). Præcipuarum Stellarum Inerrantium Positiones Mediæ Ineunte Seculo XIX: ex Observationibus Habitis in Specula Panormitana ab anno 1792 ad annum 1802. Panormi.
  20. ^ Piazzi, G., ed. (1814). Praecipuarum Stellarum Inerrantium Positiones Mediae Ineunte Saeculo XIX: ex Observationibus Habitis in Specula Panormitana ab anno 1792 ad annum 1813. Panormi. p. 159. ISBN 978-1-02-230635-6.
  21. ^ Laffitte, R. (2005). Héritages arabes: Des noms arabes pour les étoiles (2éme revue et corrigée ed.). Paris: Librairie Orientaliste Paul Geunthner / Les Cahiers de l'Orient. p. 156, note 267.
  22. ^ a b Brelstaff, T.; Lloyd, C.; Markham, T.; McAdam, D. (June 1997). "The periods of MU Cephei". Journal of the British Astronomical Association. 107 (3): 135–140. Bibcode:1997JBAA..107..135B.
  23. ^ Mozurkewich, D.; Armstrong, J. T.; Hindsley, R. B.; Quirrenbach, A.; Hummel, C. A.; Hutter, D. J.; Johnston, K. J.; Hajian, A. R.; Elias, Nicholas M.; Buscher, D. F.; Simon, R. S. (2003). "Angular Diameters of Stars from the Mark III Optical Interferometer". The Astronomical Journal. 126 (5): 2502. Bibcode:2003AJ....126.2502M. doi:10.1086/378596. S2CID 67789347.
  24. ^ a b Perrin, G.; Ridgway, S. T.; Verhoelst, T.; Schuller, P. A.; Traub, W. A.; Millan-Gabet, R.; Lacasse, M. G. (2005-06-01). "Study of molecular layers in the atmosphere of the supergiant star μ Cep by interferometry in the K band". Astronomy & Astrophysics. 436 (1): 317–324. doi:10.1051/0004-6361:20042313. ISSN 0004-6361.
  25. ^ Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society, 25: 1319, Bibcode:1993AAS...183.1710G
  26. ^ a b Perrin, G.; et al. (2005). "Study of molecular layers in the atmosphere of the supergiant star μ Cep by interferometry in the K band". Astronomy & Astrophysics. 436 (1): 317–324. arXiv:astro-ph/0502415. Bibcode:2005A&A...436..317P. doi:10.1051/0004-6361:20042313. S2CID 13980310.
  27. ^ Tsuji, Takashi (2000). "Water in Emission in the Infrared Space Observatory Spectrum of the Early M Supergiant Star μ Cephei". The Astrophysical Journal Letters. 540 (2): 99–102. arXiv:astro-ph/0008058. Bibcode:2000ApJ...540L..99T. doi:10.1086/312879. S2CID 14881959.
  28. ^ Tsuji, T. (2000). "Water on the Early M Supergiant Stars α Orionis and μ Cephei". The Astrophysical Journal. 538 (2): 801–807. Bibcode:2000ApJ...538..801T. doi:10.1086/309185.
  29. ^ Kiss, L. L.; Szabó, G. M.; Bedding, T. R. (2006). "Variability in red supergiant stars: Pulsations, long secondary periods and convection noise". Monthly Notices of the Royal Astronomical Society. 372 (4): 1721–1734. arXiv:astro-ph/0608438. Bibcode:2006MNRAS.372.1721K. doi:10.1111/j.1365-2966.2006.10973.x. S2CID 5203133.
  30. ^ "Jim Kaler-Garnet star".
  31. ^ De Beck, E.; Decin, L.; de Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. M. (November 2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles - II. CO line survey of evolved stars: derivation of mass-loss rate formulae". Astronomy & Astrophysics. 523: A18. arXiv:1008.1083. Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771. ISSN 0004-6361. S2CID 16131273.
  32. ^ Meynet, G.; Chomienne, V.; Ekström, S.; Georgy, C.; Granada, A.; Groh, J.; Maeder, A.; Eggenberger, P.; Levesque, E.; Massey, P. (2015). "Impact of mass-loss on the evolution and pre-supernova properties of red supergiants". Astronomy & Astrophysics. 575 (60): A60. arXiv:1410.8721. Bibcode:2015A&A...575A..60M. doi:10.1051/0004-6361/201424671. S2CID 38736311.
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