Mu Pictoris
In this article, we will analyze the role of Mu Pictoris in today's society and explore its impact on different aspects of everyday life. From Mu Pictoris as a public figure to his influence on topics such as technology, economics and popular culture, we will delve into his relevance in diverse contexts. We will also examine how Mu Pictoris has evolved over time and how its presence remains significant today. Through this analysis, we will seek to better understand the role that Mu Pictoris plays in the contemporary world and its importance in individual and collective experiences.
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Pictor |
| Right ascension | 06h 31m 58.31021s[1] |
| Declination | −58° 45′ 13.8117″[1] |
| Apparent magnitude (V) | 5.69[2] (5.71 + 9.43)[3] |
| Characteristics | |
| Spectral type | B9 Ve[4] or B9 IVn + A8 V:p?[5] |
| U−B color index | −0.17[2] |
| B−V color index | −0.06[2] |
| Astrometry | |
| Radial velocity (Rv) | +0.40±1.00[6] km/s |
| Proper motion (μ) | RA: −1.34[1] mas/yr Dec.: +1.77[1] mas/yr |
| Parallax (π) | 4.31±0.38 mas[1] |
| Distance | 760 ± 70 ly (230 ± 20 pc) |
| Absolute magnitude (MV) | 0.20/3.75[7] |
| Details | |
| μ Pic A | |
| Mass | 3.60±0.09[8] M☉ |
| Luminosity | 355[8] L☉ |
| Temperature | 10,568[8] K |
| Rotational velocity (v sin i) | 228[8] km/s |
| Other designations | |
| μ Pic, CPD−58° 722, HD 46860, HIP 31137, HR 2412, SAO 234564[9] | |
| Database references | |
| SIMBAD | data |
μ Pictoris, Latinised as Mu Pictoris, is a binary star[3] 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.[2] Based upon an annual parallax shift of 4.31 mas as seen from Earth,[1] the system is located roughly 760 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[3] 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.[10]
The secondary companion, component B, is a white-hued star of magnitude 9.43[3] 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.
References
- ^ a b c d e f van Leeuwen, F. (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 d 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.
- ^ a b c d 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ a b c d 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.
- ^ "mu. Pic". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-08-08.
{{cite web}}: CS1 maint: postscript (link) - ^ 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.
