To install click the Add extension button. That's it.

The source code for the WIKI 2 extension is being checked by specialists of the Mozilla Foundation, Google, and Apple. You could also do it yourself at any point in time.

How to transfigure the Wikipedia

Would you like Wikipedia to always look as professional and up-to-date? We have created a browser extension. It will enhance any encyclopedic page you visit with the magic of the WIKI 2 technology.

Try it — you can delete it anytime.

Install in 5 seconds
4,5
Kelly Slayton
Congratulations on this excellent venture… what a great idea!
Alexander Grigorievskiy
I use WIKI 2 every day and almost forgot how the original Wikipedia looks like.
Live Statistics
English Articles
Improved in 24 Hours
Added in 24 Hours
Languages
Recent
Show all languages
What we do. Every page goes through several hundred of perfecting techniques; in live mode. Quite the same Wikipedia. Just better.
Great Wikipedia has got greater.
.
Leo
Newton
Brights
Milds

89 Leonis

From Wikipedia, the free encyclopedia

89 Leonis
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Leo
Right ascension 11h 34m 21.94862s[1]
Declination +03° 03′ 36.5931″[1]
Apparent magnitude (V) 5.70[2]
Characteristics
Spectral type F5.5V[3]
B−V color index 0.480±0.005[4]
Astrometry
Radial velocity (Rv)+4.775±0.0006[5] km/s
Proper motion (μ) RA: −183.582[1] mas/yr
Dec.: −102.903[1] mas/yr
Parallax (π)36.9527 ± 0.0817 mas[1]
Distance88.3 ± 0.2 ly
(27.06 ± 0.06 pc)
Absolute magnitude (MV)3.53[2]
Details
Mass1.29[2] M☉
Radius1.38±0.04[1] R☉
Luminosity2.990+0.009
−0.010[1] L☉
Surface gravity (log g)4.22[3] cgs
Temperature6,461+93
−90[1] K
Metallicity [Fe/H]−0.04[3] dex
Rotational velocity (v sin i)15.1[2] km/s
Age1.13[2] Gyr
Other designations
89 Leonis, BD+03°2521, FK5 2924, GJ 9367, HD 100563, HIP 56445, HR 4455, SAO 118929[6]
Database references
SIMBADdata

89 Leonis is a single[7] star in the equatorial constellation of Leo, the lion. It has a yellow-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 5.70.[2] Based upon parallax measurements, it is located at a distance of 88 light years from the Sun. The star has a high proper motion[8] and is moving further away with a radial velocity of +4.8 km/s.[5] It is a candidate member of the TW Hydrae stellar kinematic group.[8]

This is an F-type main-sequence star with a stellar classification of F5.5V.[3] It is an estimated 1.13[2] billion years old and is spinning with a rotation period of 7.73 days.[9] It shows evidence of a short-term activity cycle lasting 222.5±3.3 days.[9] The star has 1.3[2] times the mass of the Sun and 1.4[1] times the Sun's radius. It is radiating three[1] times the luminosity of the Sun from its photosphere at an effective temperature of 6,461 K.[1]

References

  1. ^ a b c d e f g h i j k 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.
  2. ^ a b c d e f g h Luck, R. Earle (January 2017), "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants", The Astronomical Journal, 153 (1): 19, arXiv:1611.02897, Bibcode:2017AJ....153...21L, doi:10.3847/1538-3881/153/1/21, S2CID 119511744, 21.
  3. ^ a b c d Gray, R. O.; et al. (2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc--The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
  4. ^ 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.
  5. ^ a b Soubiran, C.; et al. (2018), "Gaia Data Release 2. The catalogue of radial velocity standard stars", Astronomy and Astrophysics, 616: A7, arXiv:1804.09370, Bibcode:2018A&A...616A...7S, doi:10.1051/0004-6361/201832795, S2CID 52952408.
  6. ^ "89 Leo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-10-05.
  7. ^ 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.
  8. ^ a b Nakajima, Tadashi; Morino, Jun-Ichi (2012), "Potential Members of Stellar Kinematic Groups within 30 pc of the Sun", The Astronomical Journal, 143 (1): 2, Bibcode:2012AJ....143....2N, doi:10.1088/0004-6256/143/1/2.
  9. ^ a b Mittag, M.; et al. (January 2019), "Discovery of short-term activity cycles in F-type stars", Astronomy & Astrophysics, 621: 7, Bibcode:2019A&A...621A.136M, doi:10.1051/0004-6361/201834319, A136.0{{citation}}: CS1 maint: postscript (link)
This page was last edited on 29 November 2023, at 23:06
Basis of this page is in Wikipedia. Text is available under the CC BY-SA 3.0 Unported License. Non-text media are available under their specified licenses. Wikipedia® is a registered trademark of the Wikimedia Foundation, Inc. WIKI 2 is an independent company and has no affiliation with Wikimedia Foundation.
Contact WIKI 2
Introduction
Terms of Service
Privacy Policy