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.

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.
.
Leo
Newton
Brights
Milds

From Wikipedia, the free encyclopedia

42 Librae
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Libra
Right ascension 15h 34m 16.89835s[1]
Declination −10° 03′ 05.07536″[1]
Apparent magnitude (V) 4.97[2]
Characteristics
Spectral type K3-III CN2[3]
B−V color index 1.302±0.056[2]
Astrometry
Radial velocity (Rv)−21.8±2.8[2] km/s
Proper motion (μ) RA: −16.872[1] mas/yr
Dec.: −17.820[1] mas/yr
Parallax (π)8.7152 ± 0.2628 mas[1]
Distance370 ± 10 ly
(115 ± 3 pc)
Absolute magnitude (MV)−0.37[2]
Details
Radius25.9±0.4[1] R
Luminosity213.6±7.3[1] L
Surface gravity (log g)2.30[4] cgs
Temperature4,332±34[1] K
Metallicity [Fe/H]−0.03±0.06[2] dex
Other designations
42 Lib, CD−23°12458, FK5 3239, GJ 9526, HD 139663, HIP 76742, HR 5824, SAO 183686[5]
Database references
SIMBADdata

42 Librae is a single[6] star located around 370[1] light years distant from the Sun in the southern zodiac constellation of Libra.[5] It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.97.[2] This object is drifting closer to the Earth with a heliocentric radial velocity of −22 km/s.[2]

This is an aging giant star with a stellar classification of K3-III CN2,[3] where the suffix notation indicates this is a strong CN star with a high overabundance of cyanogen in its spectrum. Having exhausted the supply of hydrogen at its core, this star has expanded to 26 times the Sun's radius.[1] Within the margin of error it has near-solar abundances of iron,[2] suggesting a Sun–like metallicity. The star is radiating 214[1] times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,332 K.[1]

References

  1. ^ a b c d e f g h i j k l 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 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.
  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. ^ 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.
  5. ^ a b "42 Lib". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-07-17.
  6. ^ 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.
This page was last edited on 13 August 2023, at 02:48
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.