Mu Persei
Location of μ Persei (circled) | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Perseus |
| Right ascension | Template:RA[1] |
| Declination | Template:DEC[1] |
| Apparent magnitude (V) | +4.16[2] |
| Characteristics | |
| Spectral type | G0Ib[3] + B9.5[4] |
| B−V color index | 0.935±0.002[5] |
| Astrometry | |
| Radial velocity (Rv) | 26.46[6] km/s |
| Proper motion (μ) | RA: 5.52[1] mas/yr Dec.: −17.37[1] mas/yr |
| Parallax (π) | 3.62±0.20 mas[1] |
| Distance | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Absolute magnitude (MV) | −3.11[7] |
| Orbit[8] | |
| Period (P) | 284 d |
| Semi-major axis (a) | 18.8 ± 8.8 mas |
| Eccentricity (e) | 0.062 |
| Inclination (i) | 74 ± 24° |
| Longitude of the node (Ω) | 296 ± 18° |
| Periastron epoch (T) | 2,420,062 |
| Argument of periastron (ω) (secondary) | 302° |
| Details | |
| Mass | 4.7[7] M☉ |
| Radius | 42.9[7] R☉ |
| Luminosity | ~2030[9] L☉ |
| Surface gravity (log g) | 1.90[7] cgs |
| Temperature | 5,412±23[7] K |
| Metallicity [Fe/H] | 0.09[10] dex |
| Rotational velocity (v sin i) | 12[11] km/s |
| Other designations | |
| Template:Odlist[12] | |
| Database references | |
| SIMBAD | data |
Mu Persei, Latinised from μ Persei, is a binary star system in the northern constellation of Perseus. It is visible to the naked eye as a point of light with a combined apparent visual magnitude of +4.16.[2] The distance to this system is approximately 900 light-years based on parallax measurements.[1] It is drifting further away with a radial velocity of +26 km/s.[6]
Mu Persei is a spectroscopic binary with an orbital period of 284 days and an eccentricity of about 0.06.[8] The primary component is a yellow G-type supergiant star, with an effective temperature of about 5,412 K, a radius of 42.9 solar radii,[7] and a luminosity 2,030 times solar.[9] The companion is a B-type star with a class of B9.5[4]
Mu Persei is moving through the galaxy at a speed of 35.6 km/s relative to the Sun. Its projected galactic orbit carries it between 23,900 and 32,400 light-years from the center of the galaxy.[13]
Mu Persei came closest to the Sun 5.6 million years ago when it had brightened to magnitude 3.25 from a distance of 600 light-years.[13]
Naming
In Chinese, Script error: No such module "Lang". (Script error: No such module "Lang".), meaning Celestial Boat, refers to an asterism consisting of μ Persei, η Persei, γ Persei, α Persei, ψ Persei, δ Persei, 48 Persei and HD 27084. Consequently, μ Persei itself is known as Script error: No such module "Lang". (Script error: No such module "Lang"., Template:Langx).[14]
References
Page Template:Reflist/styles.css has no content.
- ^ a b c d e f Page Module:Citation/CS1/styles.css has no content.van Leeuwen, F.; et al. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
- ^ a b Page Module:Citation/CS1/styles.css has no content.Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
- ^ Page Module:Citation/CS1/styles.css has no content.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.
- ^ a b Page Module:Citation/CS1/styles.css has no content.Pantaleoni González, M.; Maíz Apellániz, J.; Barbá, R. H.; Negueruela, I. (January 2020). "A Catalog of Galactic Multiple Systems with a Red Supergiant and a B Star". Research Notes of the AAS. 4 (1): 12. arXiv:2001.11680. Bibcode:2020RNAAS...4...12P. doi:10.3847/2515-5172/ab712b. S2CID 211003674. 12.
- ^ Page Module:Citation/CS1/styles.css has no content.Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- ^ a b Page Module:Citation/CS1/styles.css has no content.Soubiran, C.; Bienaymé, O.; Mishenina, T. V.; Kovtyukh, V. V. (2008). "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants". Astronomy and Astrophysics. 480 (1): 91–101. arXiv:0712.1370. Bibcode:2008A&A...480...91S. doi:10.1051/0004-6361:20078788. S2CID 16602121.
- ^ a b c d e f Page Module:Citation/CS1/styles.css has no content.Usenko, I. A. (April 2017). "Spectroscopic studies of yellow supergiants in the Cepheid instability strip". Astronomy Letters. 43 (4): 265–283. Bibcode:2017AstL...43..265U. doi:10.1134/S1063773717040090. ISSN 1063-7737.
- ^ a b Page Module:Citation/CS1/styles.css has no content.Alden, Harold L. (1925). "Apparent orbit of μ Persei". Astronomical Journal. 36 (851): 81–82. Bibcode:1925AJ.....36...81A. doi:10.1086/104676.
- ^ a b MU PER (Mu Persei)
- ^ Page Module:Citation/CS1/styles.css has no content.Luck, R. Earle (2014). "Parameters and Abundances in Luminous Stars". The Astronomical Journal. 147 (6): 137. Bibcode:2014AJ....147..137L. doi:10.1088/0004-6256/147/6/137.
- ^ Page Module:Citation/CS1/styles.css has no content.de Medeiros, J. R.; Udry, S.; Burki, G.; Mayor, M. (2002). "A catalog of rotational and radial velocities for evolved stars. II. Ib supergiant stars" (PDF). Astronomy and Astrophysics. 395: 97–98. Bibcode:2002A&A...395...97D. doi:10.1051/0004-6361:20021214.
- ^ Page Module:Citation/CS1/styles.css has no content."* mu. Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 23 February 2017.
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- ^ Template:In lang AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日 Script error: No such module "webarchive".
