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 144.5 light-years (44.3 parsecs) from Earth.[1] This is sufficiently close that the magnitude of the star is only reduced by 0.05 due to extinction.[4] In Chinese astronomy, Psi Ursae Majoris is called Tien Tsan or Ta Tsun, "Extremely Honorable".[10] The name was possibly derived from the word 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).
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.[8]
ReferencesEdit
^ abcdefvan 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
^ abcdJennens, 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, Bibcode:1975MNRAS.172..667J, doi:10.1093/mnras/172.3.667
^ abcdefFrasca, 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, arXiv:0911.0760, Bibcode:2009A&A...508.1313F, doi:10.1051/0004-6361/200913327, S2CID 118361131
^ abFamaey, 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, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID 17804304
^Cardini, D. (January 2005), "Mg II chromospheric radiative loss rates in cool active and quiet stars", Astronomy and Astrophysics, 430: 303–311, arXiv:astro-ph/0409683, Bibcode:2005A&A...430..303C, doi:10.1051/0004-6361:20041440, S2CID 12136256.
^ abcdePiau, L.; et al. (February 2011), "Surface convection and red-giant radius measurements", Astronomy and Astrophysics, 526: A100, arXiv:1010.3649, Bibcode:2011A&A...526A.100P, doi:10.1051/0004-6361/201014442, S2CID 118533297
^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. Bibcode:2008AJ....135..209M. doi:10.1088/0004-6256/135/1/209. S2CID 121883397.
^ abSoubiran, 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
^"psi UMa -- Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-16
^Allen, Richard Hinckley (1963), Star Names — Their Lore and Meaning: Ursa Major (Dover ed.), University of Chicago
^, 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
October 17, 2023
ursae, majoris, ursae, majoris, star, northern, circumpolar, constellation, ursa, major, apparent, visual, magnitude, making, third, magnitude, star, brighter, members, constellation, parallax, measurements, place, distance, light, years, parsecs, from, earth,. Psi Ursae Majoris Psi UMa ps Ursae Majoris ps 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 144 5 light years 44 3 parsecs from Earth 1 This is sufficiently close that the magnitude of the star is only reduced by 0 05 due to extinction 4 In Chinese astronomy Psi Ursae Majoris is called Tien Tsan or Ta Tsun Extremely Honorable 10 The name was possibly derived from the word 太尊 Pinyin Taizun meaning Royals because this star stands alone as the only member of the Royals asterism within the Purple Forbidden enclosure see Chinese constellation Psi Ursae MajorisLocation of ps Ursae Majoris circled Observation dataEpoch J2000 0 Equinox J2000 0 ICRS Constellation Ursa MajorRight ascension 11h 09m 39 80868s 1 Declination 44 29 54 5520 1 Apparent magnitude V 3 01 2 CharacteristicsSpectral type K1 III 3 U B color index 1 12 2 B V color index 1 14 2 AstrometryRadial velocity Rv 3 39 4 km sProper motion m RA 62 02 1 mas yr Dec 27 41 1 mas yrParallax p 22 57 0 14 mas 1 Distance144 5 0 9 ly 44 3 0 3 pc Absolute magnitude MV 0 27 5 DetailsRadius19 7 0 6 6 R Luminosity148 12 6 L Surface gravity log g 2 36 3 cgsTemperature4 520 3 KMetallicity Fe H 0 13 6 to 0 16 3 dexRotational velocity v sin i 5 5 7 km sAge1 11 0 39 8 GyrOther designationsps Ursae Majoris ps UMa Psi UMa 52 Ursae Majoris BD 45 1897 FK5 420 GC 15340 HD 96833 HIP 54539 HR 4335 PPM 52277 SAO 43629 9 Database referencesSIMBADdataThe spectrum of this star matches a stellar classification of K1 III 3 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 6 times the radius of the Sun It is radiating roughly 148 6 times the luminosity of the Sun from its enlarged outer envelope at an effective temperature of 4 520 K 3 At this heat the star glows with the orange hue of a K type star 11 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 8 References Edit a b c d e f van Leeuwen F November 2007 Validation of the new Hipparcos reduction Astronomy and Astrophysics 474 2 653 664 arXiv 0708 1752 Bibcode 2007A amp A 474 653V doi 10 1051 0004 6361 20078357 S2CID 18759600 a b c d 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 Bibcode 1975MNRAS 172 667J doi 10 1093 mnras 172 3 667 a b c d e f 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 arXiv 0911 0760 Bibcode 2009A amp A 508 1313F doi 10 1051 0004 6361 200913327 S2CID 118361131 a b 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 arXiv astro ph 0409579 Bibcode 2005A amp A 430 165F doi 10 1051 0004 6361 20041272 S2CID 17804304 Cardini D January 2005 Mg II chromospheric radiative loss rates in cool active and quiet stars Astronomy and Astrophysics 430 303 311 arXiv astro ph 0409683 Bibcode 2005A amp A 430 303C doi 10 1051 0004 6361 20041440 S2CID 12136256 a b c d e Piau L et al February 2011 Surface convection and red giant radius measurements Astronomy and Astrophysics 526 A100 arXiv 1010 3649 Bibcode 2011A amp A 526A 100P doi 10 1051 0004 6361 201014442 S2CID 118533297 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 Bibcode 2008AJ 135 209M doi 10 1088 0004 6256 135 1 209 S2CID 121883397 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 amp A 480 91S doi 10 1051 0004 6361 20078788 S2CID 16602121 psi UMa Star SIMBAD Centre de Donnees astronomiques de Strasbourg retrieved 2012 01 16 Allen Richard Hinckley 1963 Star Names Their Lore and Meaning Ursa Major Dover ed University of Chicago 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 Retrieved from https en wikipedia org w index php title Psi Ursae Majoris amp oldid 1179808408, wikipedia, wiki, book, books, library,
