Mu Persei

From Wikipedia, the free encyclopedia
Jump to: navigation, search
Mu Persei
Perseus constellation map.svg
Red circle.svg

Location of μ Persei (circled)
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[1] mas
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
μ Persei, 51 Persei, BD+48 1063, CCDM J04149+4824A, FK5 1117, GC 5099, HD 26630, HIP 19812, HR 1303, PPM 46912, SAO 39404, WDS J04149+4825A
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 Kelvin 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[edit]

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, English: the Seventh Star of Celestial Boat.)[10]

References[edit]

  1. ^ 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:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. 
  2. ^ 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. 
  3. ^ "* mu. Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 23 February 2017. 
  4. ^ 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:0712.1370Freely accessible. Bibcode:2008A&A...480...91S. doi:10.1051/0004-6361:20078788. 
  5. ^ 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. 
  6. ^ a b c MU PER (Mu Persei)
  7. ^ 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. 
  8. ^ 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". Astronomy and Astrophysics. 395: 97–98. Bibcode:2002A&A...395...97D. doi:10.1051/0004-6361:20021214. 
  9. ^ a b Mu Persei (HIP 19812)
  10. ^ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日