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Pi Boötis

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Pi Boötis
Observation data
Epoch J2000      Equinox J2000
Constellation Boötes[1]
Right ascension 14h 40m 43.559s[2]
Declination +16° 25′ 05.98″[2]
Apparent magnitude (V) 4.49[1] (4.893 + 5.761)[3]
Characteristics
Spectral type B9 IIIp (MnHgSi) + A6 V[4]
U−B color index −0.31[5]
B−V color index −0.002±0.010[1]
R−I color index −0.02[citation needed]
Astrometry
Radial velocity (Rv)−1.1±0.8[6] km/s
Proper motion (μ) RA: +13.922 mas/yr[2]
Dec.: +15.566 mas/yr[2]
Parallax (π)10.3357±0.1199 mas[2]
Distance316 ± 4 ly
(97 ± 1 pc)
Absolute magnitude (MV)–0.39[7]
Details
π1 Boo
Mass3.49±0.14[7] M☉
Radius3.2±0.4[7] R☉
Luminosity214[7] L☉
Surface gravity (log g)3.99±0.18[8] cgs
Temperature12,052±456[8] K
Metallicity [Fe/H]+0.18±0.17[8] dex
Rotational velocity (v sin i)14.0[9] km/s
π2 Boo
Surface gravity (log g)3.60±0.01[10] cgs
Temperature7504+21
−17[10] K
Metallicity [Fe/H]0.580[10] dex
Rotational velocity (v sin i)144[11] km/s
Other designations
π Boo, 29 Boötis, BD+17°2768, HIP 71762, ADS 9338[12]
π1 Boötis: HD 129174, HR 5475, SAO 101138
π2 Boötis: HD 129175, HR 5476, SAO 101139
Database references
π1 Boo
SIMBADdata
π1 Boo
SIMBADdata
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

Pi Boötis is a candidate triple star[13] system in the northern constellation of Boötes. Its name is a Bayer designation that is Latinized from π Boötis, and abbreviated Pi Boo or π Boo. This system is visible to the naked eye as a point of light with a combined apparent visual magnitude of 4.50.[14] Based upon an annual parallax shift of 10.67 mas[2] as seen from Earth, it is located roughly 316 light years from the Sun.

The brighter primary, component π1 Boötis, has a visual magnitude of 4.89[3] and a stellar classification of B9 IIIp (MnHgSi),[4] which suggests it is an evolved blue-white hued B-type giant star. It is a chemically peculiar star of the HgMn type,[9] with a spectrum that displays anomalous overabundances of mercury, manganese, and silicon.[4] This component is most likely a single-lined spectroscopic binary with an unknown companion.[13]

Its magnitude 5.76[3] visible companion, π2 Boötis, is a white-hued A-type main-sequence star with a class of A6 V.[4] It is spinning rapidly with a projected rotational velocity of 144 km/s.[11] As of 2010, the pair were separated by 5.537±0.003 arcseconds on the sky along a position angle of 110.5°±0.5°. This corresponds to a projected separation of 538.6±47.7 AU. The odds that is a mere chance alignment is 0.85%.[13]

Pi Boötis has the Chinese traditional star name 左攝提二 (Zuǒ shè tí èr).

References

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  1. ^ a b c Anderson, 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. XHIP record for this object at VizieR.
  2. ^ a b c d e 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.
  3. ^ a b c Høg, E.; et al. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy and Astrophysics, 355: L27, Bibcode:2000A&A...355L..27H, doi:10.1888/0333750888/2862.
  4. ^ a b c d Abt, H. A.; Cardona, O. (January 1, 1984), "The nature of the visual companions of Ap and Am stars", Astrophysical Journal, Part 1, 276: 266–269, Bibcode:1984ApJ...276..266A, doi:10.1086/161610.
  5. ^ Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode:1978A&AS...34....1N.
  6. ^ Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
  7. ^ a b c d North, P. (June 1998), "Do SI stars undergo any rotational braking?", Astronomy and Astrophysics, 334: 181–187, arXiv:astro-ph/9802286, Bibcode:1998A&A...334..181N.
  8. ^ a b c Prugniel, P.; et al. (2011), "The atmospheric parameters and spectral interpolator for the MILES stars", Astronomy & Astrophysics, 531: A165, arXiv:1104.4952, Bibcode:2011A&A...531A.165P, doi:10.1051/0004-6361/201116769, S2CID 54940439.
  9. ^ a b Ghazaryan, S.; Alecian, G. (August 2016), "Statistical analysis from recent abundance determinations in HgMn stars", Monthly Notices of the Royal Astronomical Society, 460 (2): 1912–1922, Bibcode:2016MNRAS.460.1912G, doi:10.1093/mnras/stw911
  10. ^ a b c Royer, P.; et al. (January 2024), "MELCHIORS. The Mercator Library of High Resolution Stellar Spectroscopy", Astronomy & Astrophysics, 681, id. A107, arXiv:2311.02705, Bibcode:2024A&A...681A.107R, doi:10.1051/0004-6361/202346847.
  11. ^ a b Royer, F.; et al. (May 2002), "Rotational velocities of A-type stars II. Measurement of vsini in the northern hemisphere", Astronomy & Astrophysics, 393: 897–912, arXiv:astro-ph/0205255, Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943, S2CID 14070763.
  12. ^ "pi Boo", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-10-18.
  13. ^ a b c Schöller, M.; et al. (November 2010), "Multiplicity of late-type B stars with HgMn peculiarity", Astronomy and Astrophysics, 522: 12, arXiv:1010.3643, Bibcode:2010A&A...522A..85S, doi:10.1051/0004-6361/201014246, S2CID 119273467, A85
  14. ^ 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.
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