Star in the constellation Pegasus
33 Pegasi is theFlamsteed designation for avisual binary star in the northernconstellation ofPegasus . It has anapparent visual magnitude of 6.2,[ 2] near the limit of naked eye visibility. Measurements show an annualparallax shift of″ [ 1] radial velocity of 24 km/s.[ 2]
The primary component of this system is amain sequence star with a visual magnitude of 6.4[ 3] stellar classification of F7 V.[ 4] [ 6] [ 7] stellar atmosphere has aneffective temperature of 6,169 K,[ 9] F-type star .[ 11]
A faint, magnitude 9.3 companion star is located at an angular separation of 0.420 arc seconds along aposition angle of 0.0°.[ 3] projected separation ofAU [ 6] orbital period of about 250 years.[ 12]
^a b c d e 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 atVizieR .^a b c d e f Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs",Astronomy and Astrophysics ,418 :989– 1019,arXiv :astro-ph/0405198 Bibcode :2004A&A...418..989N ,doi :10.1051/0004-6361:20035959 ,S2CID 11027621 . ^a b c Fabricius, C.; Makarov, V. V. (April 2000), "Two-colour photometry for 9473 components of close Hipparcos double and multiple stars",Astronomy and Astrophysics ,356 :141– 145,Bibcode :2000A&A...356..141F . ^a b Harlan, E. A.; Taylor, D. C. (March 1970), "MK classification for F- and G-type stars. II",Astronomical Journal ,75 (2):165– 166,Bibcode :1970AJ.....75..165H ,doi :10.1086/110956 ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation",Astronomy Letters ,38 (5): 331,arXiv :1108.4971 Bibcode :2012AstL...38..331A ,doi :10.1134/S1063773712050015 ,S2CID 119257644 . ^a b c d Tokovinin, A.; Kiyaeva, O. (2015), "Eccentricity distribution of wide binaries",Monthly Notices of the Royal Astronomical Society ,456 (2): 2070,arXiv :1512.00278 Bibcode :2016MNRAS.456.2070T ,doi :10.1093/mnras/stv2825 S2CID 1615080 . ^a b c Brown, A. G. A. ; et al. (Gaia collaboration) (August 2018)."Gaia Data Release 2: Summary of the contents and survey properties" .Astronomy & Astrophysics 616 . A1.arXiv :1804.09365 Bibcode :2018A&A...616A...1G doi :10.1051/0004-6361/201833051 Gaia DR2 record for this source atVizieR .^ Boesgaard, Ann Merchant; et al. (2004), "The Correlation of Lithium and Beryllium in F and G Field and Cluster Dwarf Stars",The Astrophysical Journal ,613 (2):1202– 1212,Bibcode :2004ApJ...613.1202B ,doi :10.1086/423194 ^a b c d Casagrande, L.; et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey",Astronomy & Astrophysics ,530 : A138,arXiv :1103.4651 Bibcode :2011A&A...530A.138C ,doi :10.1051/0004-6361/201016276 ,S2CID 56118016 . ^ "* 33 Peg" .SIMBAD Centre de données astronomiques de Strasbourg . Retrieved2013-12-31 .^ "The Colour of Stars" ,Australia Telescope, Outreach and Education ,Commonwealth Scientific and Industrial Research Organisation , December 21, 2004, archived fromthe original on March 18, 2012, retrieved2012-01-16 .^ Tokovinin, Andrei (April 2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs",The Astronomical Journal ,147 (4): 14,arXiv :1401.6827 Bibcode :2014AJ....147...87T ,doi :10.1088/0004-6256/147/4/87 ,S2CID 56066740 , 87.
