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Upsilon Ursae Majoris, Latinized from υ Ursae Majoris, is a binary star[12] in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye with an apparent visual magnitude of +3.79.[4] Based upon an annual parallax shift of 13.24 mas,[1] it is located roughly 246 light-years from the Sun.

A light curve for Upsilon Ursae Majoris, plotted from TESS data[13]
A light curve for Upsilon Ursae Majoris, plotted from TESS data[13]
Upsilon Ursae Majoris
Location of υ Ursae Majoris (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Ursa Major
Right ascension 09h 50m 59.35700s[1]
Declination +59° 02′ 19.4486″[1]
Apparent magnitude (V) 3.68 – 3.86[2]
Characteristics
Spectral type F2 IV[3]
U−B color index +0.09[4]
B−V color index +0.29[4]
Variable type δ Sct[2]
Astrometry
Radial velocity (Rv)27.3±4.1[5] km/s
Proper motion (μ) RA: +42.97[1] mas/yr
Dec.: −23.62[1] mas/yr
Parallax (π)28.06 ± 0.20 mas[1]
Distance116.2 ± 0.8 ly
(35.6 ± 0.3 pc)
Absolute magnitude (MV)+1.11[6]
Details
υ UMa A
Mass1.57[7] or 2.20[3] M☉
Radius2.79±0.40[8] R☉
Luminosity29.5[9] L☉
Surface gravity (log g)3.79±0.14[7] cgs
Temperature7,211±245[7] K
Rotation1.2±0.30 d[8]
Rotational velocity (v sin i)124.2[10] km/s
Age1.168[7] Gyr
υ UMa B
Mass0.44[3] M☉
Other designations
υ UMa, WDS J09510+5902[11]
A: 29 Ursae Majoris, BD+59°1268, FK5 368, HD 84999, HIP 48319, HR 3888, SAO 27401[11]
Database references
SIMBADdata

The primary member of the system, component A, is an F-type subgiant star. It is a Delta Scuti variable[8] with a period of 0.1327 day and an amplitude of 0.050 magnitude.[14] With an estimated age of 1.168[7] billion years, it is spinning rapidly with a projected rotational velocity of 124.2 km/s[10] and a rotation period of 1.2 days.[8] The star has about 1.57[7] times the mass of the Sun and 2.79[8] times the Sun's radius. (De Rosa and colleagues give a mass estimate of 2.2[3] times the Sun's mass.) It is radiating around 29.5[9] times the solar luminosity from its outer atmosphere at an effective temperature of 7,211 K.[7]

The companion, component B, is a magnitude +11.0 star.[12] As of 2008, it has an angular separation of 11.78 arcseconds along a position angle of 295.4°. This corresponds to a projected separation of 419.8 AU.[3] It has a mass around 40% that of the Sun.[3]


Naming


With τ, h, φ, θ, e and f, it composed the Arabic asterism Sarīr Banāt al-Na'sh, the Throne of the daughters of Na'sh, and Al-Haud, the Pond.[15] According to the catalogue of stars in the Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars, Al-Haud were the title for seven stars : f as Alhaud I, τ as Alhaud II, e as Alhaud III, h as Alhaud IV, θ as Alhaud V, this star (υ) as Alhaud VI and φ as Alhaud VII .[16]

In Chinese, 文昌 (Wén Chāng), meaning Administrative Center, refers to an asterism consisting of υ Ursae Majoris, φ Ursae Majoris, θ Ursae Majoris, 15 Ursae Majoris and 18 Ursae Majoris. Consequently, the Chinese name for υ Ursae Majoris itself is 文昌一 (Wén Chāng yī, English: the first Star of Administrative Center.).[17]


References


  1. 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.
  2. Samus, N. N.; Durlevich, O. V.; et al. (2009), "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)", VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S, 1, Bibcode:2009yCat....102025S.
  3. De Rosa, R. J.; et al. (2013), "The VAST Survey – III. The multiplicity of A-type stars within 75 pc", Monthly Notices of the Royal Astronomical Society, 437 (2): 1216, arXiv:1311.7141, Bibcode:2014MNRAS.437.1216D, doi:10.1093/mnras/stt1932, S2CID 88503488.
  4. Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  5. 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.
  6. 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, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672.
  7. 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, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  8. Korzennik, S. G.; et al. (April 1995), "Nightly variations of nonradial oscillations in the Delta Scuti star upsilon Ursae Majoris", Astrophysical Journal, Part 2, 443 (1): L25–L28, Bibcode:1995ApJ...443L..25K, doi:10.1086/187827.
  9. Balona, L. A.; Dziembowski, W. A. (October 1999), "Excitation and visibility of high-degree modes in stars", Monthly Notices of the Royal Astronomical Society, 309 (1): 221–232, Bibcode:1999MNRAS.309..221B, doi:10.1046/j.1365-8711.1999.02821.x.
  10. Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377
  11. "ups UMa", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-02-22.
  12. 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.
  13. MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, retrieved 8 December 2021.
  14. Rodríguez, E.; et al. (June 2000), "A revised catalogue of delta Sct stars", Astronomy and Astrophysics Supplement, 144 (3): 469–474, Bibcode:2000A&AS..144..469R, doi:10.1051/aas:2000221.
  15. Allen, Richard Hinckley (1899), Star-Names and Their Meanings, New York: G. E. Stechert, p. 442.
  16. Rhoads, Jack W. (November 15, 1971), Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars (PDF), Jet Propulsion Laboratory, California Institute of Technology.
  17. (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 16 日

На других языках

- [en] Upsilon Ursae Majoris

[es] Ípsilon Ursae Majoris

Ípsilon Ursae Majoris (υ UMa / 29 Ursae Majoris / HD 84999)[1] es una estrella de magnitud aparente +3,80 situada en la constelación de la Osa Mayor. En China era conocida —junto a θ Ursae Majoris y φ Ursae Majoris— como Wan Chang, «la iluminación literaria».[2] Se encuentra a 115 años luz del Sistema Solar.

[ru] Ипсилон Большой Медведицы

Ипсилон Большой Медведицы (лат. υ Ursae Majoris), 29 Большой Медведицы (лат. 29 Ursae Majoris), HD 84999 — двойная звезда в созвездии Большой Медведицы на расстоянии приблизительно 112 световых лет (около 34 парсеков) от Солнца. Видимая звёздная величина звезды — от +3,86m до +3,68m[11]. Возраст звезды оценивается как около 1,168 млрд лет[12].


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