Astronomy:Psi Ursae Majoris

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Short description: Star in the constellation Ursa Major

Coordinates: Sky map 11h 09m 39s, +44° 29′ 54″

Psi Ursae Majoris
Diagram showing star positions and boundaries of the Ursa Major constellation and its surroundings
Diagram showing star positions and boundaries of the Ursa Major constellation and its surroundings

Location of ψ Ursae Majoris (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Ursa Major
Right ascension  11h 09m 39.8083s[1]
Declination +44° 29′ 54.556″[1]
Apparent magnitude (V) +3.01[2]
Characteristics
Evolutionary stage horizontal branch[3]
Spectral type K1 III[4]
U−B color index +1.12[2]
B−V color index +1.14[2]
Astrometry
Radial velocity (Rv)–3.39[5] km/s
Proper motion (μ) RA: –62.02[1] mas/yr
Dec.: –27.78[1] mas/yr
Parallax (π)23.2272 ± 0.2513[1] mas
Distance140 ± 2 ly
(43.1 ± 0.5 pc)
Absolute magnitude (MV)−0.27[6]
Details[7]
Mass2.31±0.13 M☉
Radius19.12[7]–20.79[8] R☉
Luminosity140±3 L☉
Surface gravity (log g)2.12±0.05 cgs
Temperature4,543±6 K
Metallicity [Fe/H]−0.11±0.03 dex
Rotational velocity (v sin i)5.5[9] km/s
Other designations
ψ UMa, 52 UMa, BD+45 1897, FK5 420, GC 15340, HD 96833, HIP 54539, HR 4335, SAO 43629, PPM 52277[10]
Database references
SIMBADdata

Psi Ursae Majoris (Psi UMa, ψ Ursae Majoris, ψ UMa) is a star in the northern circumpolar constellation of Ursa Major. It has an apparent visual magnitude of +3.01,[2] making it a third magnitude star and one of the brighter members of the constellation. Parallax measurements place it at a distance of 140 light-years (43 parsecs) from Earth.[1] This is sufficiently close that the magnitude of the star is only reduced by 0.05 due to extinction.[5] In Chinese astronomy, Psi Ursae Majoris is called 太尊, Pinyin: Tàizūn, meaning Royals, because this star stands alone as the only member of the Royals asterism within the Purple Forbidden enclosure (see Chinese constellation).[11] In R. H. Allen's Star Names, this was transliterated as Tien Tsan or Ta Tsun, meaning "Extremely Honorable".[12]

The spectrum of this star matches a stellar classification of K1 III,[4] with the luminosity class of 'III' indicating this is an evolved giant star that has exhausted the supply of hydrogen at its core. As a consequence, it has expanded to around 20 times the radius of the Sun.[8][7] It is radiating roughly 140 times the luminosity of the Sun from its enlarged outer envelope at an effective temperature of 4,543 K.[7] At this heat, the star glows with the orange hue of a K-type star.[13]

Psi Ursae Majoris is a member of the thin disk population of the Milky Way. It is following an orbit through the galaxy with a low eccentricity of 0.02 that will carry it between 26.5–27.8 kly (8.1–8.5 kpc) from the Galactic Center. The low inclination of its orbit means the star will only stray 130 ly (40 pc) from the galactic plane.[14]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 Jennens, P. A.; Helfer, H. L. (September 1975), "A new photometric metal abundance and luminosity calibration for field G and K giants.", Monthly Notices of the Royal Astronomical Society 172 (3): 667–679, doi:10.1093/mnras/172.3.667, Bibcode: 1975MNRAS.172..667J 
  3. ↑ Stock, Stephan; Reffert, Sabine; Quirrenbach, Andreas (2018). "Precise radial velocities of giant stars. X. Bayesian stellar parameters and evolutionary stages for 372 giant stars from the Lick planet search". Astronomy and Astrophysics 616: A33. doi:10.1051/0004-6361/201833111. Bibcode: 2018A&A...616A..33S. 
  4. ↑ 4.0 4.1 Frasca, A. et al. (December 2009), "REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion. Rotation periods and starspot parameters", Astronomy and Astrophysics 508 (3): 1313–1330, doi:10.1051/0004-6361/200913327, Bibcode: 2009A&A...508.1313F 
  5. ↑ 5.0 5.1 Famaey, B. et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics 430: 165–186, doi:10.1051/0004-6361:20041272, Bibcode: 2005A&A...430..165F 
  6. ↑ Cardini, D. (January 2005), "Mg II chromospheric radiative loss rates in cool active and quiet stars", Astronomy and Astrophysics 430: 303–311, doi:10.1051/0004-6361:20041440, Bibcode: 2005A&A...430..303C. 
  7. ↑ 7.0 7.1 7.2 7.3 Soubiran, C.; Creevey, O. L.; Lagarde, N.; Brouillet, N.; Jofré, P.; Casamiquela, L.; Heiter, U.; Aguilera-Gómez, C. et al. (2024-02-01). "Gaia FGK benchmark stars: Fundamental Teff and log g of the third version". Astronomy and Astrophysics 682: A145. doi:10.1051/0004-6361/202347136. ISSN 0004-6361. Bibcode: 2024A&A...682A.145S.  Psi Ursae Majoris' database entry at VizieR.
  8. ↑ 8.0 8.1 Gray, David F.; Kaur, Taranpreet (2019-09-01). "A Recipe for Finding Stellar Radii, Temperatures, Surface Gravities, Metallicities, and Masses Using Spectral Lines". The Astrophysical Journal 882 (2): 148. doi:10.3847/1538-4357/ab2fce. ISSN 0004-637X. Bibcode: 2019ApJ...882..148G. 
  9. ↑ Massarotti, Alessandro et al. (January 2008). "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity". The Astronomical Journal 135 (1): 209–231. doi:10.1088/0004-6256/135/1/209. Bibcode: 2008AJ....135..209M. 
  10. ↑ "psi UMa -- Star", SIMBAD (Centre de Données astronomiques de Strasbourg), http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Psi+Ursae+Majoris, retrieved 2012-01-16 
  11. ↑ Ridpath, Ian. "Star Tales – Ursa Major 2". http://www.ianridpath.com/startales/ursamajor2.html. 
  12. ↑ Allen, Richard Hinckley (1963), Star Names — Their Lore and Meaning: Ursa Major (Dover ed.), University of Chicago, https://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Ursa_Major*.html 
  13. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-01-16 
  14. ↑ 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, doi:10.1051/0004-6361:20078788, Bibcode: 2008A&A...480...91S 



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