B-type giant star in the constellation Pyxis
Alpha Pyxidis ,Latinised fromα Pyxidis , is agiant star in theconstellation Pyxis . It is the brightest star in Pyxis, and is easily visible to thenaked eye . It has astellar classification of B1.5III and is aBeta Cephei variable . This star has more than ten times themass of the Sun and is more than six times theSun's radius . The surface temperature is 24,300 K and the star is about 10,000 times asluminous as the Sun .[ 3] [ 4] [ 8] Stars such as this with more than 10 solar masses are expected to end their life by exploding as asupernova .[ 11]
Alight curve for Alpha Pyxidis, plotted fromTESS data.[ 12] InChinese ,天狗 (Tiān Gǒu ), meaningCelestial Dog , refers to anasterism consisting of α Pyxidis,e Velorum ,f Velorum ,β Pyxidis ,γ Pyxidis andδ Pyxidis . Consequently, α Pyxidis itself is known as天狗五 (Tiān Gǒu wǔ , English:the Fifth Star of Celestial Dog ).[ 13]
^a b c d e van 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 ^a b c Fernie, J. D. (May 1983)."New UBVRI photometry for 900 supergiants" .Astrophysical Journal Supplement Series .52 :7– 22.Bibcode :1983ApJS...52....7F .doi :10.1086/190856 . ^a b Hiltner, W. A.; Garrison, R. F.; Schild, R. E. (July 1969)."MK Spectral Types for Bright Southern OB Stars" .Astrophysical Journal .157 : 313.Bibcode :1969ApJ...157..313H .doi :10.1086/150069 . ^a b c d Hubrig, S.; et al. (January 2009). "New magnetic field measurements of beta Cephei stars and Slowly Pulsating B stars".Astronomische Nachrichten .330 (4): 317.arXiv :0902.1314 .Bibcode :2009AN....330..317H .doi :10.1002/asna.200811187 .S2CID 17497112 . ^ Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities".Carnegie Institute Washington D.C. Publication .Carnegie Institute of Washington D.C. Bibcode :1953GCRV..C......0W . ^ 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 . ^ Hubrig, S.; Ilyin, I.; Schöller, M.; Briquet, M.; Morel, T.; De Cat, P. (January 2011),"First Magnetic Field Models for Recently Discovered Magnetic β Cephei and Slowly Pulsating B Stars" (PDF) ,The Astrophysical Journal Letters ,726 (1): L5,arXiv :1012.3019 ,Bibcode :2011ApJ...726L...5H ,doi :10.1088/2041-8205/726/1/L5 ,hdl :2268/81132 ,S2CID 119195567 ^a b c d Kilian, J. (February 1994). "Chemical abundances in early B-type stars. 5: Metal abundances and LTE/NLTE comparison".Astronomy and Astrophysics .282 (3):867– 873.Bibcode :1994A&A...282..867K . ^ Nieva, M. F.; Przybilla, N. (April 2008). "Carbon abundances of early B-type stars in the solar vicinity. Non-LTE line-formation for C II/III/IV and self-consistent atmospheric parameters".Astronomy and Astrophysics .481 (1):199– 216.arXiv :0711.3783 .Bibcode :2008A&A...481..199N .doi :10.1051/0004-6361:20078203 .S2CID 10281324 . ^ "alf Pyx" .SIMBAD .Centre de données astronomiques de Strasbourg . Retrieved2021-07-29 .{{cite web }}
: CS1 maint: postscript (link )^ Reed, B. Cameron (June 28, 2005). "New Estimates of the Solar-Neighborhood Massive-Stars Birthrate and the Galactic Supernova Rate".The Astronomical Journal .130 (4):1652– 1657.arXiv :astro-ph/0506708 .Bibcode :2005AJ....130.1652R .doi :10.1086/444474 .S2CID 119515135 . ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes" . Space Telescope Science Institute. Retrieved29 September 2024 .^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 17 日 Archived 2012-02-04 at theWayback Machine