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Theta Sculptoris

From Wikipedia, the free encyclopedia
Star in the constellation Sculptor
Theta Sculptoris
Location of θ Sculptoris (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
ConstellationSculptor
Right ascension00h 11m 44.02079s[1]
Declination−35° 07′ 59.2320″[1]
Apparent magnitude (V)+5.236±0.005[2]
Characteristics
Evolutionary stagemain sequence
Spectral typeF5V[3]
B−Vcolor index0.459±0.002[4]
Astrometry
Radial velocity (Rv)−21.1±0.3[4] km/s
Proper motion (μ)RA: +171.529[1]mas/yr
Dec.: +126.670[1]mas/yr
Parallax (π)46.1936±0.1565 mas[1]
Distance70.6 ± 0.2 ly
(21.65 ± 0.07 pc)
Absolute magnitude (MV)3.52[2]
Details[2]
Mass1.25 M
Radius1.40±0.05 R
Luminosity3.09[4] L
Surface gravity (log g)4.25±0.10 cgs
Temperature6,395±80 K
Metallicity[Fe/H]−0.07±0.07 dex
Rotational velocity (v sin i)1.0±1.0 km/s
Age1.6+2.4
−0.5
[4] Gyr
Other designations
θ Scl,CD−35°4,FK5 6,GC 202,GJ 3013,HD 739,HIP 950,HR 35,SAO 192388,LTT 79,GSC 06995-01262[5]
Database references
SIMBADdata

θ Sculptoris,Latinized asTheta Sculptoris, is astar in the southernconstellation ofSculptor. This object is visible to the naked eye as a dim, yellow-white hued star with anapparent visual magnitude of +5.24.[2] It is located 71 light years from the Sun based onparallax.[1] The object is drifting closer with aradial velocity of −21 km/s, and may come to within 49 light-years in half a million years.[4]

This is anastrometric binary system.[6] The visible component is an ordinaryF-type main-sequence star with astellar classification of F5V.[3] It is around 1.6[4] billion years old with 1.25 times themass of the Sun and 1.40 times theSun's radius. The star is radiating three[4] times theluminosity of the Sun from itsphotosphere at aneffective temperature of 6,395 K.[2]

References

[edit]
  1. ^abcdefBrown, 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.
  2. ^abcdeFuhrmann, K.; Chini, R. (2012), "Multiplicity among F-type Stars",The Astrophysical Journal Supplement,203 (2): 20,Bibcode:2012ApJS..203...30F,doi:10.1088/0067-0049/203/2/30, 30.
  3. ^abGray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (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,arXiv:astro-ph/0603770,Bibcode:2006AJ....132..161G,doi:10.1086/504637,S2CID 119476992.
  4. ^abcdefgAnderson, 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.
  5. ^"tet Scl".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2019-09-03.{{cite web}}: CS1 maint: postscript (link)
  6. ^Fuhrmann, K.; Chini, R. (August 2015), "Multiplicity among F-type stars. II",The Astrophysical Journal,809 (1): 19,Bibcode:2015ApJ...809..107F,doi:10.1088/0004-637X/809/1/107, 107.
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