13 Boötis
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Boötes |
| Right ascension | 14h 08m 17.30243s[2] |
| Declination | +49° 27′ 29.3993″[2] |
| Apparent magnitude (V) | 5.26[3] (5.29 to 5.38)[4] |
| Characteristics | |
| Spectral type | M1.5III[5] |
| U−B color index | +1.92[6] |
| B−V color index | +1.637±0.010[3] |
| Variable type | Lb[4] |
| Astrometry | |
| Radial velocity (Rv) | −13.92±0.06[3] km/s |
| Proper motion (μ) | RA: −58.584[2] mas/yr Dec.: 59.801[2] mas/yr |
| Parallax (π) | 4.6635 ± 0.1756 mas[2] |
| Distance | 700 ± 30 ly (214 ± 8 pc) |
| Absolute magnitude (MV) | −0.87[3] |
| Details | |
| Mass | 0.8-2.6[7] M☉ |
| Radius | 74+10 −12[2] R☉ |
| Luminosity | 1,114±48[2] L☉ |
| Temperature | 3,889+379 −248[2] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
13 Boötis is a solitary[9] variable star in the northern constellation of Boötes, and is positioned near the western constellation border with Ursa Major. In 1977 it was given the variable star designation CF Boötis,[10] often abbreviated CF Boo, while 13 Boötis is the star's Flamsteed designation. This star has a reddish hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 5.26.[3] It is located at a distance of approximately 700 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −14 km/s.[3]
The variability of the brightness of 13 Boötis was announced by Joel Stebbins and Charles Morse Huffer in 1928, based on observations made at Washburn Observatory.[11] This is an aging red giant star on the asymptotic giant branch[12] with a stellar classification of M1.5III,[5] which is interpreted by stellar evolutionary models to mean it has exhausted the supply of hydrogen at its core then cooled and expanded off the main sequence. It is classified as a slow irregular variable of the Lb type, and its brightness has been observed to vary from +5.29 down to +5.38.[4] The star has ~74 times the girth of the Sun and is radiating 1,114 times the Sun's luminosity from its swollen photosphere at an effective temperature of 3,889 K.[2]
There is a magnitude 11.05 visual companion located at an angular separation of 76.40 arcseconds from the brighter star, along a position angle of 270°. This was first reported by William Herschel in 1783.[13]
Possible planetary system
[edit]In 1991, Duquennoy & Mayor[14] reported the possible presence of a low-mass object (of likely substellar nature) orbiting the red giant 13 Bootis. They set a minimum mass of 30 times that of Jupiter (likely a brown dwarf) and estimated an orbital period of 1.35 years. So far there has been no confirmation about the presence a substellar object.
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | ≥30 MJ | ≥1.25 | 494 | 0.21 | — | — |
References
[edit]- ^ EAS (1997). "The HIPPARCOS and TYCHO catalogues". Astrometric and Photometric Star Catalogues Derived from the ESA Hipparcos Space Astrometry Mission. ESA SP Series. 1200. Noordwijk, Netherlands: ESA Publications Division. Bibcode:1997HIP...C......0E. ISBN 9290923997. Retrieved 15 October 2022.
- ^ a b c d e f g h i 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.
- ^ a b c d e f 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. S2CID 119257644.
- ^ a b c Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
- ^ 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.
- ^ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
- ^ Alvarez, R.; Mennessier, M. -O. (1997). "Determination of Miras temperatures from TiO and VO bands. Estimates of distances". Astronomy and Astrophysics. 317: 761–768. Bibcode:1997A&A...317..761A.
- ^ "* 13 Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 25 May 2017.
- ^ 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.
- ^ Kukarkin, B. V.; Kholopov, P. N.; Fedorovich, V. P.; Kireyeva, N. N.; Kukarkina, N. P.; Medvedeva, G. I.; Perova, N. B. (March 1977). "62nd Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 1248: 1–25. Bibcode:1977IBVS.1248....1K. Retrieved 5 December 2024.
- ^ Stebbins, Joel; Huffer, C. M. (1928). "The Constancy of the Light of Red Stars". Publications of the Washburn Observatory. 15: 137–174. Bibcode:1928PWasO..15..137S. Retrieved 5 December 2024.
- ^ Eggen, Olin J. (July 1992). "Asymptotic giant branch stars near the sun". Astronomical Journal. 104 (1): 275–313. Bibcode:1992AJ....104..275E. doi:10.1086/116239.
- ^ Mason, B. D.; et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
- ^ Duquennoy, A.; Mayor, M. (1991). "Multiplicity among solar-type stars in the solar neighbourhood. II - Distribution of the orbital elements in an unbiased sample". Astronomy and Astrophysics. 248 (2): 485–524. Bibcode:1991A&A...248..485D.
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