Astronomy:Psi Persei

From HandWiki
Revision as of 13:08, 14 February 2024 by BotanyGa (talk | contribs) (linkage)
(diff) ← Older revision | Latest revision (diff) | Newer revision → (diff)
Short description: Star in the constellation Perseus
ψ Persei
Perseus constellation map.svg
Red circle.svg
Location of ψ Persei (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Perseus
Right ascension  03h 36m 29.37982s[1]
Declination +48° 11′ 33.4789″[1]
Apparent magnitude (V) 4.17 - 4.28[2]
Characteristics
Spectral type B5Ve[3]
U−B color index −0.56[4]
B−V color index −0.06[4]
Variable type γ Cas[5]
Astrometry
Radial velocity (Rv)−1.1[6] km/s
Proper motion (μ) RA: +22.55[1] mas/yr
Dec.: −27.78[1] mas/yr
Parallax (π)5.59 ± 0.22[1] mas
Distance580 ± 20 ly
(179 ± 7 pc)
Absolute magnitude (MV)−2.03[7]
Details
Mass4.8[8] M☉
Radius5.5/7.26[9] R☉
Luminosity2,042[10] L☉
Surface gravity (log g)3.65[11] cgs
Temperature15,654[10] K
Rotational velocity (v sin i)275[11] km/s
Age63.1[12] Myr
Other designations
ψ Persei, ψ Per, Psi Per, 37 Persei, BD+47°857, GC 4287, HD 22192, HIP 16826, HR 1087, PPM 46127, SAO 46366[13]
Database references
SIMBADdata

Psi Persei (Psi Per, ψ Persei, ψ Per) is a single[7] Be star in the northern constellation of Perseus. It has an apparent visual magnitude of about 4.2, so it is visible to the naked eye at night under suitably dark skies. Based on parallax measurements, it is located at a distance of roughly 580 light-years (180 parsecs) from the Earth.

Properties

A light curve for Psi Persei, plotted from TESS data,[14] with the period derived by Percy et al.[5] shown in red.

This star has a stellar classification of B5Ve,[3] which indicates it is a B-type main sequence star that is generating energy at its core through the nuclear fusion of hydrogen. It is a shell star with a circumstellar disc of gas surrounding the equator and extending out to about 11 times the radius of the star.[15] As a result of this disc, the spectrum of this star shows emission lines (as indicated by the 'e' in the stellar class) and its magnitude varies over a period 1.021 days.[5] The General Catalog of Variable Stars classifies Psi Persei as a gamma Cassiopeiae variable star, whose visual band brightness varies from magnitude 4.17 to 4.28.[16]

Psi Persei is rotating rapidly with a projected rotational velocity (v sin i) along the equator of 390 km/s or more.[17] The axis of rotation is inclined about 75° ± 8° to the line of sight from the Earth, so this velocity is close to the actual azimuthal velocity along the star's equator. It is expelling mass at the rate of about 5.0 × 10−8 times the mass of the Sun per year, or the equivalent of the Sun's mass every 20 million years.[15] The rapid rotation causes Psi Persei to be an oblate shape, with the equatorial radius being 7.3 R☉ and the polar radius to be 5.5 R☉.[9]

This star may be a member of the Alpha Persei Cluster, although its proper motion is high compared to other members.[18] Membership probabilities of 26% and 50% have been published from GALAH plus APOGEE data and from Gaia Data Release 2 data respectively.[19][20]

Name and etymology

This star, together with δ Per, σ Per, α Per, γ Per and η Per, has been called the Segment of Perseus.[21]

In Chinese, 天船 (Tiān Chuán), meaning Celestial Boat, refers to an asterism consisting of ψ Persei, η Persei, α Persei, γ Persei, δ Persei, 48 Persei, μ Persei and HD 27084. Consequently, the Chinese name for ψ Persei itself is 天船四 (Tiān Chuán sì, English: the Fourth Star of Celestial Boat.)[22]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 Samus, N. N. et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. GCVS 5.1 61 (1): 80–88. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S. 
  3. ↑ 3.0 3.1 3.2 Lesh, Janet Rountree (December 1968). "The Kinematics of the Gould Belt: an Expanding Group?". Astrophysical Journal Supplement 17: 371. doi:10.1086/190179. Bibcode: 1968ApJS...17..371L. 
  4. ↑ 4.0 4.1 4.2 Johnson, H. L. et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99): 99. Bibcode: 1966CoLPL...4...99J. 
  5. ↑ 5.0 5.1 5.2 5.3 Percy, John R.; Ivans, Inese I.; Fried, Robert E.; Paparo, Margit (February 1994). "Short-term photometric variability of Psi Persei and Zeta Tauri". Publications of the Astronomical Society of the Pacific 106 (696): 131–133. doi:10.1086/133356. Bibcode: 1994PASP..106..131P. 
  6. ↑ 6.0 6.1 Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". in Batten, Alan Henry. University of Toronto: International Astronomical Union. 1967. pp. 57–63. Bibcode: 1967IAUS...30...57E. 
  7. ↑ 7.0 7.1 7.2 Hutter, D. J.; Tycner, C.; Zavala, R. T.; Benson, J. A.; Hummel, C. A.; Zirm, H. (2021). "Surveying the Bright Stars by Optical Interferometry. III. A Magnitude-limited Multiplicity Survey of Classical be Stars". The Astrophysical Journal Supplement Series 257 (2): 69. doi:10.3847/1538-4365/ac23cb. Bibcode: 2021ApJS..257...69H. 
  8. ↑ 8.0 8.1 Sheikhi, Najmeh et al. (March 2016). "The binary fraction and mass segregation in Alpha Persei open cluster". Monthly Notices of the Royal Astronomical Society 457 (1): 1028–1036. doi:10.1093/mnras/stw059. Bibcode: 2016MNRAS.457.1028S. 
  9. ↑ 9.0 9.1 9.2 Klement, R.; Carciofi, A. C.; Rivinius, T.; Matthews, L. D.; Vieira, R. G.; Ignace, R.; Bjorkman, J. E.; Mota, B. C. et al. (2017). "Revealing the structure of the outer disks of be stars". Astronomy and Astrophysics 601: A74. doi:10.1051/0004-6361/201629932. Bibcode: 2017A&A...601A..74K. 
  10. ↑ 10.0 10.1 10.2 Silaj, J.; Landstreet, J. D. (2014). "Accurate age determinations of several nearby open clusters containing magnetic Ap stars". Astronomy & Astrophysics 566: A132. doi:10.1051/0004-6361/201321468. Bibcode: 2014A&A...566A.132S. 
  11. ↑ 11.0 11.1 11.2 Zorec, J. et al. (November 2016). "Critical study of the distribution of rotational velocities of Be stars. I. Deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity". Astronomy & Astrophysics 595: 26. doi:10.1051/0004-6361/201628760. Bibcode: 2016A&A...595A.132Z. 
  12. ↑ 12.0 12.1 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society 410 (1): 190–200. doi:10.1111/j.1365-2966.2010.17434.x. Bibcode: 2011MNRAS.410..190T. 
  13. ↑ 13.0 13.1 "psi Per -- Be Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Psi+Persei. 
  14. ↑ 14.0 14.1 "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  15. ↑ 15.0 15.1 15.2 Delaa, O. et al. (May 2011). "Kinematics and geometrical study of the Be stars 48 Persei and ψ Persei with the VEGA/CHARA interferometer". Astronomy & Astrophysics 529: A87. doi:10.1051/0004-6361/201015639. Bibcode: 2011A&A...529A..87D. 
  16. ↑ 16.0 16.1 "psi Per". Sternberg Astronomical Institute. http://www.sai.msu.su/gcvs/cgi-bin/search2.cgi?search=psi+Per. 
  17. ↑ 17.0 17.1 Bernacca, P. L.; Perinotto, M. (1970). "A Catalogue of Stellar Rotational Velocities". Contributi Osservatorio Astronomico di Padova in Asiago 239 (1): 1. Bibcode: 1970CoAsi.239....1B. 
  18. ↑ 18.0 18.1 Morrell, Nidia; Abt, Helmut A. (July 10, 1992). "Spectroscopic binaries in the Alpha Persei cluster". Astrophysical Journal, Part 1 393 (2): 666–673. doi:10.1086/171534. Bibcode: 1992ApJ...393..666M. 
  19. ↑ 19.0 19.1 Spina, L. et al. (2021). "The GALAH survey: Tracing the Galactic disc with open clusters". Monthly Notices of the Royal Astronomical Society 503 (3): 3279. doi:10.1093/mnras/stab471. Bibcode: 2021MNRAS.503.3279S. 
  20. ↑ 20.0 20.1 Cantat-Gaudin, T.; Jordi, C.; Vallenari, A.; Bragaglia, A.; Balaguer-Núñez, L.; Soubiran, C.; Bossini, D.; Moitinho, A. et al. (2018). "A Gaia DR2 view of the open cluster population in the Milky Way". Astronomy and Astrophysics 618: A93. doi:10.1051/0004-6361/201833476. Bibcode: 2018A&A...618A..93C. 
  21. ↑ 21.0 21.1 Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York: Dover Publications Inc. p. 331. ISBN 0-486-21079-0. https://archive.org/details/starnamestheirlo00alle/page/331. Retrieved 2012-09-04. 
  22. ↑ 22.0 22.1 (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
  23. ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. 
  24. ↑ Underhill, A. B. et al. (November 1979). "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars". Monthly Notices of the Royal Astronomical Society 189 (3): 601–605. doi:10.1093/mnras/189.3.601. Bibcode: 1979MNRAS.189..601U. 



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Psi_Persei&oldid=3670834"