Astronomy:Psi Octantis

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Short description: Star in the constellation Octans
ψ Octantis
Octans IAU.svg
Red circle.svg
Location of ψ Oct (circled)
Observation data
Epoch J2000.0   Equinox (celestial coordinates)
Constellation Octans
Right ascension  22h 17m 50.5954s[1]
Declination −77° 30′ 41.599″[1]
Apparent magnitude (V) 5.47±0.01[2]
Characteristics
Evolutionary stage main sequence[1]
Spectral type F0IIp[3] (F4V:kA5)[4]
U−B color index +0.12[5]
B−V color index +0.31[5]
Astrometry
Radial velocity (Rv)17.0±1.6[6] km/s
Proper motion (μ) RA: −37.392[1] mas/yr
Dec.: +13.788[1] mas/yr
Parallax (π)25.7575 ± 0.0505[1] mas
Distance126.6 ± 0.2 ly
(38.82 ± 0.08 pc)
Absolute magnitude (MV)+2.56[7]
Details
Mass1.49±0.07[8] M☉
Radius1.74±0.04[8] R☉
Luminosity7.82[7] L☉
Surface gravity (log g)4.13±0.05[8] cgs
Temperature7,244[8] K
Metallicity [Fe/H]−0.04[9] dex
Age1.41[9] Gyr
Other designations
ψ Oct, CPD−78°1442, FK5 3779, GC 31133, HD 210853, HIP 110078, HR 8471, SAO 258020[10]
Database references
SIMBADdata

Psi Octantis, Latinized from ψ Octantis, is a solitary[11] star in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.47,[2] allowing it to be seen with the naked eye under ideal conditions. The star is relatively close at a distance of 126 light years[1] but is receding with a heliocentric radial velocity of 17 km/s.[6]

Psi Octantis has a spectral classification of F0IIp, suggesting that it is a bright giant but with peculiarities. Other assessments give a luminosity class of III (giant),[12] III-IV (intermediate between giant and subgiant),[13] or V: (approximately main sequence).[4] One paper gives a spectral class of F4V:kA5, indicating that it is a probable F-type main-sequence star with the calcium K-lines of an A5 star, including sharp absorption lines of metals.[4] Analysis of its evolutionary stage show it to be a somewhat evolved main sequence star.[1]

It has 149% the mass of the Sun and 1.74 times the radius of the Sun.[8] It shines at 7.82 times the luminosity of the Sun[7] from its photosphere at an effective temperature of 7,244 K,[8] giving it a yellowish white glow. Psi Octantis has an iron abundance 91% that of the Sun and is estimated to be 1.41 billion years old.[9]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 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 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. ISSN 0004-6361. Bibcode: 2000A&A...355L..27H. 
  3. ↑ Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (2 June 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc--The Southern Sample". The Astronomical Journal 132 (1): 161–170. doi:10.1086/504637. ISSN 0004-6256. Bibcode: 2006AJ....132..161G. 
  4. ↑ 4.0 4.1 4.2 Hoffleit, Dorrit (1953). "The spectra and absolute magnitudes of 500 A3 - G2 stars". Annals of Harvard College Observatory 0119: 1–35. Bibcode: 1953AnHar.119....1H. 
  5. ↑ 5.0 5.1 Johnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars". Communications of the Lunar and Planetary Laboratory 4: 99–110. Bibcode: 1966CoLPL...4...99J. 
  6. ↑ 6.0 6.1 Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. ISSN 1063-7737. Bibcode: 2006AstL...32..759G. 
  7. ↑ 7.0 7.1 7.2 Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation" (in en). Astronomy Letters 38 (5): 331–346. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 8.5 Allende Prieto, C.; Lambert, D. L. (December 1999). "Fundamental parameters of nearby stars from the comparison with evolutionary calculations: masses, radii and effective temperatures". Astronomy and Astrophysics 352: 555–562. ISSN 0004-6361. Bibcode: 1999A&A...352..555A. 
  9. ↑ 9.0 9.1 9.2 Gontcharov, G. A. (December 2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters 38 (12): 771–782. doi:10.1134/S1063773712120031. ISSN 0320-0108. Bibcode: 2012AstL...38..771G. 
  10. ↑ "Psi oct". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Psi+oct. 
  11. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869–879. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E. 
  12. ↑ Houk, N.; Cowley, A. P. (1975). University of Michigan Catalogue of two-dimensional spectral types for the HD stars. Volume I. Declinations −90° to −53°. Bibcode: 1975mcts.book.....H. 
  13. ↑ Abt, Helmut A.; Morrell, Nidia I. (July 1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". The Astrophysical Journal Supplement Series 99: 135. doi:10.1086/192182. ISSN 0067-0049. Bibcode: 1995ApJS...99..135A. 
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