Omicron Ursae Majoris (ο Ursae Majoris, abbreviated Omicron UMa, ο UMa), formally named Muscida /ˈmjuːsɪdə/,[12][13] is a star system in the northern circumpolar constellation of Ursa Major. It has an apparent visual magnitude of +3.35[2] and is located at a distance of around 179 light-years (55 parsecs) from the Sun.[1] In 2012, an exoplanet designated Omicron Ursae Majoris Ab was found to be orbiting the primary.[9]
  Location of ο Ursa Major (circled) | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Ursa Major |
| Right ascension | 08h 30m 15.87064s[1] |
| Declination | +60° 43′ 05.4115″[1] |
| Apparent magnitude (V) | +3.35[2] |
| Characteristics | |
| Spectral type | G5III:[3] |
| U−B color index | +0.52[4] |
| B−V color index | +0.85[4] |
| Astrometry | |
| Radial velocity (Rv) | +19.8[5] km/s |
| Proper motion (μ) | RA: -133.644[6] mas/yr Dec.: -107.664[6] mas/yr |
| Parallax (π) | 17.9335 ± 0.1456 mas[6] |
| Distance | 182 ± 1 ly (55.8 ± 0.5 pc) |
| Absolute magnitude (MV) | –0.40[7] |
| Details[8] | |
| Mass | 2.72 M☉ |
| Radius | 13.84 R☉ |
| Luminosity | 116 L☉ |
| Surface gravity (log g) | 2.58 cgs |
| Temperature | 5,242[7] K |
| Metallicity [Fe/H] | −0.16+0.08 −0.1 dex |
| Rotational velocity (v sin i) | 3.83[9] km/s |
| Age | 360 ± 30[10] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Nomenclature
editο Ursae Majoris (Latinised to Omicron Ursae Majoris) is the star's Bayer designation.
The traditional name Muscida was shared with the optical double star Pi Ursae Majoris. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[14] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[15] included a table of the first two batches of names approved by the WGSN; which included Muscida for this star.
In Chinese, 內階 (Nèi Jiē), meaning Inner Steps, refers to an asterism consisting of ο Ursae Majoris, 16 Ursae Majoris, 6 Ursae Majoris, 23 Ursae Majoris, 5 Ursae Majoris and 17 Ursae Majoris. Consequently, the Chinese name for ο Ursae Majoris itself is 內階一 (Nèi Jiē yī, English: the First Star of Inner Steps.).[16]
Properties and observations
editThe stellar classification of this star, G5 III, indicates that it is in the giant stage of its evolution. The interferometry-measured angular diameter of this star is about 2.42 mas,[17] which, at its estimated distance, equates to a physical radius of about 14 times the radius of the Sun.[18] It has about three times the mass of the Sun and radiates 116 times the Sun's luminosity from its outer atmosphere[8] at an effective temperature of 5,282 K,[2] giving it the yellowish hue of a G-type star.[19]
In 1963, East German astronomer Gerhard Jakisch reported this star as a variable with a period of 358 days and an amplitude of 0.08 magnitude. The 1982 edition of the New Catalogue of Suspected Variable Stars listed it with a variability from 3.30 to 3.36 in the visual band. However, in 1992 American astronomer Dorrit Hoffleit noted that the two comparison stars used to determine the variability may themselves be variable. Hence the actual variability of this star may be suspect.[20]
Muscida has a magnitude 15.2 common proper motion companion at an angular separation of 7.1 arcseconds.[21] With a probability of 99.4%, this companion is the source for the X-ray emission from the system.[22] Omicron Ursae Majoris is sometimes listed with two more companions, but, based on proper motion data, these appear to be optical companions. No other companions were detected by 2016.[23]
This system is a member of the thin disk population and is following an orbit through the Milky Way galaxy with an eccentricity of 0.12. It comes as close to the Galactic Center as 23.5 kly (7.2 kpc) and as distant as 30.2 kly (9.3 kpc). This orbit carries it no more than about 330 ly (100 pc) above the galactic plane.[10] It is considered a runaway star because it has a high peculiar velocity of 35.5 km s−1 relative to the typical motion of stars in its vicinity.[24]
The star has no detectable magnetic fields.[25]
Planetary system
editIn 2012, an exoplanet designated Omicron Ursae Majoris Ab and orbiting the primary at 3.9 astronomical units, was found. This gas giant (4.1 times as massive as Jupiter) completes an orbit in 1630 days.[9]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | >4.1 MJ | 3.9 | 1630±35 | 0.130 ± 0.065 | — | — |
References
edit- ^ a b c van Leeuwen, F. (November 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 Mallik, Sushma V. (December 1999). "Lithium abundance and mass". Astronomy and Astrophysics. 352: 495–507. Bibcode:1999A&A...352..495M.
- ^ 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 Johnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4 (99): 99. Bibcode:1966CoLPL...4...99J.
- ^ Wilson, Ralph Elmer (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Washington: Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W.
- ^ a b c Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b Takeda, Yoichi; Sato, Bun'ei; Murata, Daisuke (August 2008). "Stellar parameters and elemental abundances of late-G giants". Publications of the Astronomical Society of Japan. 60 (4): 781–802. arXiv:0805.2434. Bibcode:2008PASJ...60..781T. doi:10.1093/pasj/60.4.781. S2CID 16258166.
- ^ a b Teng, Huan-Yu; Sato, Bun'ei; et al. (August 2023). "Revisiting planetary systems in the Okayama Planet Search Program: A new long-period planet, RV astrometry joint analysis, and a multiplicity-metallicity trend around evolved stars". Publications of the Astronomical Society of Japan. 75 (6): 1030–1071. arXiv:2308.05343. Bibcode:2023PASJ...75.1030T. doi:10.1093/pasj/psad056.
- ^ a b c d Sato, Bun'ei; et al. (2012). "Substellar Companions to Seven Evolved Intermediate-Mass Stars". Publications of the Astronomical Society of Japan. 64 (6). 135. arXiv:1207.3141. Bibcode:2012PASJ...64..135S. doi:10.1093/pasj/64.6.135. S2CID 119197073.
- ^ a b Soubiran, C.; et al. (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.
- ^ "bet CMi". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-01-09.
- ^ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts: Sky Pub. ISBN 978-1-931559-44-7.
- ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
- ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
- ^ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
- ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 16 日
- ^ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005). "CHARM2: An updated Catalog of High Angular Resolution Measurements". Astronomy and Astrophysics. 431 (2): 773–777. Bibcode:2005A&A...431..773R. doi:10.1051/0004-6361:20042039.
- ^ Lang, Kenneth R. (2006). Astrophysical formulae. Astronomy and astrophysics library. Vol. 1 (3rd ed.). Birkhäuser. ISBN 3-540-29692-1.. The radius (R*) is given by:
- ^ "The Colour of Stars". Australia Telescope, Outreach and Education. Commonwealth Scientific and Industrial Research Organisation. December 21, 2004. Archived from the original on March 18, 2012. Retrieved 2012-01-16.
- ^ Hoffleit, D. (October 1992). "Do all Three Vary: omicron UMa, 23 UMa and HR 3245?". Information Bulletin on Variable Stars. 3789: 1. Bibcode:1992IBVS.3789....1H.
- ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976.
- ^ Haakonsen, Christian Bernt; Rutledge, Robert E. (September 2009). "XID II: Statistical Cross-Association of ROSAT Bright Source Catalog X-ray Sources with 2MASS Point Source Catalog Near-Infrared Sources". The Astrophysical Journal Supplement. 184 (1): 138–151. arXiv:0910.3229. Bibcode:2009ApJS..184..138H. doi:10.1088/0067-0049/184/1/138. S2CID 119267456.
- ^ Ginski, C.; Mugrauer, M.; Seeliger, M.; Buder, S.; Errmann, R.; Avenhaus, H.; Mouillet, D.; Maire, A.-L.; Raetz, S. (2016). "A lucky imaging multiplicity study of exoplanet host stars II". Monthly Notices of the Royal Astronomical Society. 457 (2): 2173–2191. arXiv:1601.01524. Bibcode:2016MNRAS.457.2173G. doi:10.1093/mnras/stw049. S2CID 53626523.
- ^ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1): 190–200. arXiv:1007.4883. Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID 118629873.
- ^ Joshi, Santosh; Semenko, Eugene; Moiseeva, A.; Sharma, Kaushal; Joshi, Y. C.; Sachkov, M.; Singh, Harinder P.; Kumar, Yerra Bharat (2017). "High-resolution Spectroscopy and Spectropolarimetry of Selected δ-Sct Pulsating Variables". Monthly Notices of the Royal Astronomical Society: stx087. arXiv:1701.02891. doi:10.1093/mnras/stx087. S2CID 119006112.
