Mu Persei
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Perseus |
| Right ascension | 04h 14m 53.86253s[1] |
| Declination | +48° 24′ 33.5912″[1] |
| Apparent magnitude (V) | +4.16[2] |
| Characteristics | |
| Spectral type | G0Ib[3] |
| Astrometry | |
| Radial velocity (Rv) | 26.46[4] 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 | 900 ± 50 ly (280 ± 20 pc) |
| Orbit[5] | |
| 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) | 2420062 |
| Argument of periastron (ω) (secondary) | 302° |
| Details | |
| Radius | ~53[6] R☉ |
| Luminosity | ~2030[6] L☉ |
| Surface gravity (log g) | 1.74[7] cgs |
| Temperature | 5418[7] K |
| Metallicity [Fe/H] | 0.09[7] dex |
| Rotational velocity (v sin i) | 12[8] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Mu Persei (Mu Per, μ Persei, μ Per) is a binary star in the constellation of Perseus, with an apparent magnitude of +4.16. The primary component is a yellow G-type supergiant. It is approximately 900 light years from Earth. With an effective temperature of about 5400 kelvins and a radius of 53 solar radii, this star has the luminosity of about 2030 times that of the Sun.[6] Mu Persei is a spectroscopic binary with an orbital period of 284 days and an eccentricity of about 0.06.[5]
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.[9]
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.[9]
Naming
In Chinese, 天船 (Tiān Chuán), 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 天船七 (Tiān Chuán qī, Template:Lang-en.)[10]
References
- ^ a b c d e 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.
- ^ 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.
- ^ "* mu. Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 23 February 2017.
- ^ 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.
- ^ a b 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 c MU PER (Mu Persei)
- ^ a b c Luck, R. Earle (2014). "Parameters and Abundances in Luminous Stars". The Astronomical Journal. 147 (6). Bibcode:2014AJ....147..137L. doi:10.1088/0004-6256/147/6/137.
- ^ 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.
- ^ a b Mu Persei (HIP 19812) Archived 2013-04-14 at archive.today
- ^ Template:Zh icon AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
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