Psi Boötis
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Boötes |
| Right ascension | 15h 04m 26.743s[1] |
| Declination | +26° 56′ 51.53″[1] |
| Apparent magnitude (V) | +4.55[2] |
| Characteristics | |
| Evolutionary stage | red clump[3] |
| Spectral type | K2 III[4] |
| U−B color index | +1.34[2] |
| B−V color index | +1.23[2] |
| Astrometry | |
| Radial velocity (Rv) | −25.72±0.18[5] km/s |
| Proper motion (μ) | RA: −174.718 mas/yr[1] Dec.: −5.036 mas/yr[1] |
| Parallax (π) | 12.6144±0.0896 mas[1] |
| Distance | 259 ± 2 ly (79.3 ± 0.6 pc) |
| Absolute magnitude (MV) | +0.16[6] |
| Details | |
| Mass | 1.38[7] M☉ |
| Radius | 20[5] R☉ |
| Luminosity | 135[7] L☉ |
| Surface gravity (log g) | 2.2[5] cgs |
| Temperature | 4,302±22[7] K |
| Metallicity [Fe/H] | −0.35[5] dex |
| Rotational velocity (v sin i) | 3.5[5] km/s |
| Age | 4.16[7] Gyr |
| Other designations | |
| Aulad al Nathlat[8], ψ Boo, 43 Boötis, BD+27°2447, FK5 557, GC 20285, HD 133582, HIP 73745, HR 5616, SAO 83645[9] | |
| Database references | |
| SIMBAD | data |
Psi Boötis is a single,[10] orange-hued star in the northern constellation of Boötes. Its name is a Bayer designation that is Latinized from ψ Boötis, and abbreviated Psi Boo or ψ Boo. This is a dim star that is visible to the naked eye with an apparent visual magnitude of +4.55.[2] Based upon an annual parallax shift of 12.6 mas as seen from the Earth, it is located about 259 light-years (79 pc) from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.09 due to interstellar dust.[6] It is traversing the sky with a net proper motion of 0.176 arc seconds per year,[11] and has a radial velocity toward the Sun of −25.72 km/s.[5]
This star has a stellar classification of K2 III,[4] matching an evolved K-type giant star. It belongs to the so-called red clump,[3] indicating that it is generating energy through helium fusion at its core. This star is about four[7] billion years old and is spinning with a projected rotational velocity of 3.5 km/s.[5] It has an estimated 1.38[7] times the mass of the Sun and has expanded to 20[5] times the Sun's radius. Psi Boötis radiating 135[7] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,302 K.[7]
Name
[edit]This star, according to Assemani, with another in the right arm that may have been ε Boo (Izar), constituted the Arabs' Al Aulād al Nadhlāt, which he rendered filii altercationis (sons of contention); but the original signifies "the Low, or Mean, Little Ones".[12]
Al Aulād al Nadhlāt or Aulad al Nathlat was the title of this star in the catalogue of stars in Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars.[8]
References
[edit]- ^ 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.
- ^ a b c d Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
- ^ a b Alves, David R. (August 2000), "K-Band Calibration of the Red Clump Luminosity", The Astrophysical Journal, 539 (2): 732–741, arXiv:astro-ph/0003329, Bibcode:2000ApJ...539..732A, doi:10.1086/309278, S2CID 16673121.
- ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
- ^ a b c d e f g h Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209, S2CID 121883397.
- ^ a b Famaey, B.; et al. (2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430: 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID 17804304.
- ^ a b c d e f g h Luck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants", The Astronomical Journal, 150 (3): 88, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114.
- ^ a b Rhoads, Jack W. (November 15, 1971), Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars, Jet Propulsion Laboratory, California Institute of Technology, retrieved 2025-06-06.
- ^ "psi Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-09.
- ^ 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.
- ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv:astro-ph/0412070, Bibcode:2005AJ....129.1483L, doi:10.1086/427854, S2CID 2603568.
- ^ Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York, NY: Dover Publications Inc. p. 106. ISBN 0-486-21079-0. Retrieved 2010-12-12.
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References
[edit]- Hoffleit; et al. (1991), "HR 5616", Bright Star Catalogue (5th Revised ed.), retrieved 2017-09-11.
- "psi Boo", Aladin previewer, Centre de Données astronomiques de Strasbourg, retrieved 2017-09-11.
