Omicron Boötis

In this article we are going to delve into Omicron Boötis, a topic/person/date that has captured the attention of many over time. Omicron Boötis has been the subject of debate, study and interest in various areas, and along these lines we will explore its multiple facets and its impact on different aspects of society. From its historical relevance to its influence on the present, we will dive into a detailed analysis of Omicron Boötis to better understand its importance and meaning in today's world. Join us on this fascinating journey towards the discovery of Omicron Boötis and all it has to offer.

ο Boötis
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Boötes
Right ascension 14h 45m 14.46026s[1]
Declination +16° 57′ 51.4078″[1]
Apparent magnitude (V) +4.60[2]
Characteristics
Spectral type G8.5 III[3]
U−B color index +0.75[2]
B−V color index +0.98[2]
Astrometry
Radial velocity (Rv)−9.18[4] km/s
Proper motion (μ) RA: −60.69[1] mas/yr
Dec.: −50.56[1] mas/yr
Parallax (π)13.42±0.24 mas[1]
Distance243 ± 4 ly
(75 ± 1 pc)
Absolute magnitude (MV)0.70[5]
Details
Mass2.05[4] M☉
Radius11[6] R☉
Luminosity85[4] L☉
Surface gravity (log g)2.7[6] cgs
Temperature4,864±25[4] K
Metallicity −0.10[6] dex
Rotational velocity (v sin i)3.6[6] km/s
Age2.72[4] Gyr
Other designations
ο Boo, 35 Boötis, BD+17° 2780, GC 19858, GJ 9493, HD 129972, HIP 72125, HR 5502, SAO 101184[7]
Database references
SIMBADdata

Omicron Boötis (ο Boötis) is a yellow-hued star in the northern constellation of Boötes. With an apparent visual magnitude of +4.60,[2] it is a fifth magnitude star that is visible to the naked eye. Based upon an annual parallax shift of 13.42 mas as seen from the Earth,[1] it is located about 243 light years from the Sun. The star is moving closer to the Sun with a radial velocity of −9 km/s.[6]

At the age of 2.72 billion years,[4] this is an evolved G-type giant star with a stellar classification of G8.5 III.[3] It belongs to the so-called "red clump", which indicates it is generating energy through helium fusion at its core.[8] Although it displays a higher abundance of barium than is normal for a star of its type, Williams (1975) considers its status as a barium star to be "very doubtful".[9] The star has double[4] the mass of the Sun and has expanded to 11[6] times the Sun's radius. It is radiating 85 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,864 K.[4]

References

  1. ^ 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.
  2. ^ 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.
  3. ^ 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.
  4. ^ a b c d e f g h Luck, R. Earle (September 2015), "Abundances in the Local Region. I. G and K Giants", The Astronomical Journal, 150 (3): 23, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114, 88.
  5. ^ McWilliam, Andrew (December 1990), "High-resolution spectroscopic survey of 671 GK giants. I - Stellar atmosphere parameters and abundances", Astrophysical Journal Supplement Series, 74: 1075–1128, Bibcode:1990ApJS...74.1075M, doi:10.1086/191527.
  6. ^ a b c d e f 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.
  7. ^ "omi Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-09.
  8. ^ 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.
  9. ^ Williams, P. M. (February 1975), "Stellar compositions from narrow-band photometry - V. Barium abundances for 200 evolved stars", Monthly Notices of the Royal Astronomical Society, 170 (2): 343–362, Bibcode:1975MNRAS.170..343W, doi:10.1093/mnras/170.2.343.
  • Hoffleit; et al. (1991), "HR 5502", Bright Star Catalogue (5th Revised ed.), retrieved 2017-09-12.
  • "omi Boo", Aladin previewer, Centre de Données astronomiques de Strasbourg, retrieved 2017-09-12.