Astronomy:78 Ursae Majoris
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Ursa Major |
| Right ascension | 13h 00m 43.69949s[1] |
| Declination | +56° 21′ 58.8102″[1] |
| Apparent magnitude (V) | 4.93[2] (5.02 + 7.88)[3] |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | F2V[4] + G6V[5] |
| U−B color index | +0.00[6] |
| B−V color index | +0.368±0.010[2] |
| Astrometry | |
| Radial velocity (Rv) | −5.1±0.9[2] km/s |
| Proper motion (μ) | RA: 107.94[1] mas/yr Dec.: 2.05[1] mas/yr |
| Parallax (π) | 39.30 ± 0.38[1] mas |
| Distance | 83.0 ± 0.8 ly (25.4 ± 0.2 pc) |
| Absolute magnitude (MV) | +2.84[7] |
| Orbit[8] | |
| Period (P) | 104.9±0.6 yr |
| Semi-major axis (a) | 1.208±0.010″ |
| Eccentricity (e) | 0.388±0.009 |
| Inclination (i) | 46.9±0.9° |
| Longitude of the node (Ω) | 88.0±1.1° |
| Periastron epoch (T) | B 1921.224±0.403 |
| Argument of periastron (ω) (secondary) | 119.2±1.5° |
| Details | |
| 78 UMa A | |
| Mass | 1.34[9] M☉ |
| Radius | 1.62±0.24[10] R☉ |
| Luminosity | 5.75[2] L☉ |
| Surface gravity (log g) | 4.26±0.14[9] cgs |
| Temperature | 6,908±235[9] K |
| Metallicity [Fe/H] | 0.01±0.05[11] dex |
| Rotation | 19.2 ± 2.9 h[10] |
| Rotational velocity (v sin i) | 91.7±4.6[12] km/s |
| Age | 785[9] Myr |
| Other designations | |
| Database references | |
| SIMBAD | The system |
| A | |
| B | |
78 Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.93.[13] Parallax estimates by Hipparcos put it at a distance of 83 light-years (25 pc),[1] but it is drifting closer with a radial velocity of −5 km/s.[2] The system is a candidate member of the Ursa Major Moving Group.[14]
The binary nature of this system was announced by S. W. Burnham in 1894.[15] The pair orbit each other with a period of 105 years and an eccentricity of 0.39. Their semimajor axis has an angular size of 1.2″ and the orbital plane is inclined by 47°.[8]
The primary member, designated component A, has a magnitude of 5.02[3] and is an F-type main-sequence star with a stellar classification of F2V.[4] It is 785[9] million years old and is spinning with a projected rotational velocity of 92 km/s.[12] The star has 1.34[9] times the mass of the Sun and is radiating 5.75[2] times the Sun's luminosity from its photosphere at an effective temperature of 6,908 K.[9]
The secondary, designated component B, has a visual magnitude of 7.88.[3] It is a G-type main-sequence star with a class of G6V.[5] The star is a suspected variable.[16]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 3.2 Fabricius, C. et al. (2002). "The Tycho double star catalogue". Astronomy and Astrophysics 384: 180–189. doi:10.1051/0004-6361:20011822. Bibcode: 2002A&A...384..180F.
- ↑ 4.0 4.1 Gray, R. O. et al. (2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I". The Astronomical Journal 126 (4): 2048. doi:10.1086/378365. Bibcode: 2003AJ....126.2048G.
- ↑ 5.0 5.1 Edwards, T. W. (April 1976), "MK classification for visual binary components", Astronomical Journal 81: 245–249, doi:10.1086/111879, Bibcode: 1976AJ.....81..245E.
- ↑ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode: 1986EgUBV........0M.
- ↑ Eggen, Olin J. (August 1998), "The Sirius Supercluster and Missing Mass near the Sun", The Astronomical Journal 116 (2): 782–788, doi:10.1086/300465, Bibcode: 1998AJ....116..782E.
- ↑ 8.0 8.1 Drummond, Jack D. (March 2014), "Binary Stars Observed with Adaptive Optics at the Starfire Optical Range", The Astronomical Journal 147 (3): 10, doi:10.1088/0004-6256/147/3/65, 65, Bibcode: 2014AJ....147...65D.
- ↑ 9.0 9.1 9.2 9.3 9.4 9.5 9.6 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ 10.0 10.1 Justesen, A. B.; Albrecht, S. (October 2020). "The spin-orbit alignment of visual binaries". Astronomy & Astrophysics 642: 10. doi:10.1051/0004-6361/202039138. A212. Bibcode: 2020A&A...642A.212J.
- ↑ Gáspár, András et al. (2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal 826 (2): 171, doi:10.3847/0004-637X/826/2/171, Bibcode: 2016ApJ...826..171G.
- ↑ 12.0 12.1 Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics 542: A116, doi:10.1051/0004-6361/201118724, Bibcode: 2012A&A...542A.116A.
- ↑ 13.0 13.1 "* 78 UMa". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+78+UMa.
- ↑ Nakajima, Tadashi; Morino, Jun-Ichi (2012), "Potential Members of Stellar Kinematic Groups within 30 pc of the Sun", The Astronomical Journal 143 (1): 2, doi:10.1088/0004-6256/143/1/2, Bibcode: 2012AJ....143....2N.
- ↑ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/orb6.
- ↑ Baize, P.; Petit, M. (March 1989), "Etoiles doubles orbitales à composantes variables", Astronomy and Astrophysics, Supplemental Series 77: 497–511, Bibcode: 1989A&AS...77..497B.
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