  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Serpens |
| Right ascension | 15h 49m 37.20696s[1] |
| Declination | −03° 25′ 48.7358″[1] |
| Apparent magnitude (V) | 3.543[2] |
| Characteristics | |
| Spectral type | A0 V[3] |
| U−B color index | −0.025[2] |
| B−V color index | −0.032[2] |
| Astrometry | |
| Radial velocity (Rv) | −9.4±2.7[4] km/s |
| Proper motion (μ) | RA: −100.28[1] mas/yr Dec.: +25.99[1] mas/yr |
| Parallax (π) | 19.23±0.38 mas[1] |
| Distance | 170 ± 3 ly (52 ± 1 pc) |
| Absolute magnitude (MV) | −0.04[5] |
| Orbit[6] | |
| Period (P) | 36±2 yr |
| Semi-major axis (a) | 0.110±0.010″ |
| Eccentricity (e) | 0.4±0.3 |
| Inclination (i) | 103±28° |
| Longitude of the node (Ω) | 296±28° |
| Periastron epoch (T) | 1988.9±1.8 |
| Argument of periastron (ω) (secondary) | 308±32° |
| Details | |
| μ Ser A | |
| Mass | 2.4 ± 0.4[6] M☉ |
| Luminosity | 92[7] L☉ |
| Temperature | 9,487[7] K |
| Rotational velocity (v sin i) | 96[8] km/s |
| μ Ser B | |
| Mass | 2.3 ± 0.4 M☉ |
| Other designations | |
| μ Ser, 32 Serpentis, BD−02°4052, FK5 585, HD 141513, HIP 77516, HR 5881, SAO 140787[9] | |
| Database references | |
| SIMBAD | data |
Mu Serpentis, Latinized from μ Serpentis, is a binary star[6] in the Serpens Caput (head) section of the equatorial constellation Serpens. It is visible to the naked eye with an apparent visual magnitude of 3.543.[2] Based upon an annual parallax shift of 19.23 mas as seen from Earth,[1] it is located around 170 light years from the Sun.
This is an astrometric binary for which coarse orbital elements have been determined based on interferometric observations. The pair orbit each other with a period of around 36 years and an eccentricity of roughly 0.4.[6] The primary member, component A, is a white-hued A-type main sequence star with a stellar classification of A0 V.[3] The nature of the secondary, component B, is less certain – it may be a class A or F type star of unknown luminosity class.[6]
In Chinese astronomy, Mu Serpentis is called 天乳, Pinyin: Tiānrǔ, meaning Celestial Milk, because this star is marking itself and stand alone in Celestial Milk asterism, Root mansion (see : Chinese constellation).[10]
References
- ^ a b c d e f van Leeuwen, F. (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 c d Gutierrez-Moreno, Adelina; et al. (1966), "A System of photometric standards", Publications of the Department of Astronomy University of Chile, 1, Publicaciones Universidad de Chile, Department de Astronomy: 1–17, Bibcode:1966PDAUC...1....1G.
- ^ a b Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
- ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
- ^ 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 c d e Gontcharov, G. A.; Kiyaeva, O. V. (March 2010), "Photocentric orbits from a direct combination of ground-based astrometry with Hipparcos II. Preliminary orbits for six astrometric binaries", New Astronomy, 15 (3): 324–331, arXiv:1606.08182, Bibcode:2010NewA...15..324G, doi:10.1016/j.newast.2009.09.006, S2CID 119252073.
- ^ a b McDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–57, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
- ^ Royer, F.; Zorec, J.; Gómez, A. E. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298.
- ^ "mu. Ser". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-03-31.
{{cite web}}: CS1 maint: postscript (link) - ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 29 日 Archived 2021-06-05 at the Wayback Machine
| Stars |
| ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||||
| Star clusters |
| ||||||||||||
| Nebulae |
| ||||||||||||
| Galaxies |
| ||||||||||||
| |||||||||||||
