Psi Boötis
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Boötes |
| Right ascension | 15h 04m 26.74234s[1] |
| Declination | +26° 56′ 51.5399″[1] |
| Apparent magnitude (V) | +4.55[2] |
| Characteristics | |
| Spectral type | K2 III[3] |
| U−B color index | +1.34[2] |
| B−V color index | +1.23[2] |
| Astrometry | |
| Radial velocity (Rv) | −25.72±0.18[4] km/s |
| Proper motion (μ) | RA: −175.42[1] mas/yr Dec.: −4.06[1] mas/yr |
| Parallax (π) | 13.26 ± 0.26 mas[1] |
| Distance | 246 ± 5 ly (75 ± 1 pc) |
| Absolute magnitude (MV) | +0.16[5] |
| Details | |
| Mass | 1.38[6] M☉ |
| Radius | 20[4] R☉ |
| Luminosity | 135[6] L☉ |
| Surface gravity (log g) | 2.2[4] cgs |
| Temperature | 4,302±22[6] K |
| Metallicity [Fe/H] | −0.35[4] dex |
| Rotational velocity (v sin i) | 3.5[4] km/s |
| Age | 4.16[6] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Psi Boötis (ψ Boötis) is a single,[9] orange-hued star in the northern constellation of Boötes. It 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 13.26 mas as seen from the Earth, it is located about 246 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction of 0.09 due to interstellar dust.[5] It is traversing the sky with a net proper motion of 0.176 arc seconds per year,[10] and has a radial velocity toward the Sun of −25.72 km/s.[4]
This star has a stellar classification of K2 III,[3] matching an evolved K-type giant star. It belongs to the so-called "red clump",[11] indicating that it is generating energy through helium fusion at its core. This star is about four[6] billion years old and is spinning with a projected rotational velocity of 3.5 km/s.[4] It has an estimated 1.38[6] times the mass of the Sun and has expanded to 20[4] times the Sun's radius. Psi Boötis radiating 135[6] times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,302 K.[6]
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.[7]
References
[edit]- ^ a b c d e 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 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 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 (PDF), Jet Propulsion Laboratory, California Institute of Technology.
- ^ "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.
- ^ 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.
- ^ 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.
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.
