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  3. Mu Pictoris
Mu Pictoris
From Wikipedia, the free encyclopedia
Mu Pictoris
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Pictor
μ Pic A
Right ascension 06h 31m 58.31011s[1]
Declination −58° 45′ 13.8114″[1]
Apparent magnitude (V) 5.71[2]
μ Pic B
Right ascension 06h 31m 58.0685s[3]
Declination −58° 45′ 15.4103″[3]
Apparent magnitude (V) 9.43[2]
Characteristics
Spectral type B9 Ve[4] or B9 IVn + A8 V:p?[5]
U−B color index −0.17[6]
B−V color index −0.06[6]
Astrometry
μ Pic A
Radial velocity (Rv)+0.40±1.00[7] km/s
Proper motion (μ) RA: −1.302 mas/yr[1]
Dec.: +1.637 mas/yr[1]
Parallax (π)5.3553±0.0358 mas[1]
Distance609 ± 4 ly
(187 ± 1 pc)
Absolute magnitude (MV)0.20[8]
μ Pic B
Proper motion (μ) RA: +0.881 mas/yr[3]
Dec.: +0.918 mas/yr[3]
Parallax (π)5.3644±0.0286 mas[3]
Distance608 ± 3 ly
(186.4 ± 1.0 pc)
Absolute magnitude (MV)3.75[8]
Details
μ Pic A
Mass3.32[1] M☉
Radius4.43[1] R☉
Luminosity205[1] L☉
Surface gravity (log g)3.612[1] cgs
Temperature10,375[1] K
Rotational velocity (v sin i)228[9] km/s
Age258[1] Myr
μ Pic B
Mass1.18[10] M☉
Radius1.26[11] R☉
Luminosity5.23[11] L☉
Surface gravity (log g)4.25[10] cgs
Temperature7,770[11] K
Other designations
μ Pic, CPD−58°722, HD 46860, HIP 31137, HR 2412, SAO 234564[12]
Database references
SIMBADμ Pic A
μ Pic B

μ Pictoris, Latinised as Mu Pictoris, is a binary star[2] system in the southern constellation Pictor. It is bright enough to be dimly visible to the naked eye, having a combined apparent visual magnitude of 5.69.[6] Based upon an annual parallax shift of 5.4 mas as seen from Earth,[1] the system is located roughly 610 light years distant from the Sun. As of 2010, the pair have an angular separation of 2.46 arc seconds along a position angle of 221°.[4]

The primary, designated component A, is a blue-white star with a visual magnitude of 5.71[2] and a stellar classification of B9 Ve[4] or B9 IVn.[5] The first classification suggests is a B-type main-sequence star, with the 'e' suffix indicating a Be star. The second may instead indicate a somewhat more evolved B-type star that is spinning rapidly, resulting in "nebulous" absorption lines. Photometrically, it shows a pulsation period of 0.397 days, which is likely the same as the rotation period.[13]

The secondary companion, component B, is a white-hued star of magnitude 9.43[2] with a classification of A8 V:p?.[5] This indicates it is an A-type main-sequence star, with the 'p?' suffix suggesting it may be chemically peculiar while the ':' notation says there is some uncertainty about the general classification. The star has a radius of 1.26 R☉ and a luminosity around 5.2 L☉,[11] values unusually low compared to the average for an A8-type dwarf star.[14]

References

[edit]
  1. ^ a b c d e f g h i j k Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c d e 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  3. ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875. Gaia DR3 record for this source at VizieR.
  4. ^ a b c Oudmaijer, René D.; Parr, Andrew M. (July 2010), "The binary fraction and mass ratio of Be and B stars: a comparative Very Large Telescope/NACO study", Monthly Notices of the Royal Astronomical Society, 405 (4): 2439–2446, arXiv:1003.0618, Bibcode:2010MNRAS.405.2439O, doi:10.1111/j.1365-2966.2010.16609.x, S2CID 119209332.
  5. ^ a b c Corbally, C. J. (1984), "Close visual binaries. I - MK classifications", Astrophysical Journal Supplement Series, 55: 657, Bibcode:1984ApJS...55..657C, doi:10.1086/190973.
  6. ^ a b c Hurly, P. R. (1975), "Combined-light UBV Photometry of 103 Bright Southern Visual Doubles", Monthly Notes of the Astronomical Society of Southern Africa, 34: 7, Bibcode:1975MNSSA..34....7H.
  7. ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  8. ^ a b Corbally, C. J. (December 1984), "Close visual binaries. III - Parameters and evolutionary status", Astronomical Journal, 89: 1887–1896, Bibcode:1984AJ.....89.1887C, doi:10.1086/113700.
  9. ^ Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  10. ^ a b Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevič, G.; Monari, G.; Cantat-Gaudin, T.; Weiler, M.; Khan, S.; Miglio, A.; Carrillo, I.; Romero-Gómez, M.; Minchev, I.; De Jong, R. S.; Antoja, T.; Ramos, P.; Steinmetz, M.; Enke, H. (2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics. 628: A94. arXiv:1904.11302. Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765.
  11. ^ a b c d 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 at VizieR.
  12. ^ "mu. Pic". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-08-08.{{cite web}}: CS1 maint: postscript (link)
  13. ^ Balona, L. A. (December 1995), "Tests of the Pulsation and Starspot Models for the Periodic Be-Stars", Monthly Notices of the Royal Astronomical Society, 277 (4): 1547, Bibcode:1995MNRAS.277.1547B, doi:10.1093/mnras/277.4.1547.
  14. ^ Mamajek, Eric (2 March 2021), A Modern Mean Dwarf Stellar Color and Effective Temperature Sequence, University of Rochester, Department of Physics and Astronomy, retrieved 5 July 2021.
Retrieved from "https://en.wikipedia.org/w/index.php?title=Mu_Pictoris&oldid=1328888103"
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