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
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

HD 130948

From Wikipedia, the free encyclopedia

HD 130948

The visual band light curve of HP Boötes, plotted from data published by Gaidos et al. (2000)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Boötes
Right ascension 14h 50m 15.8112s[2]
Declination +23° 54′ 42.639″[2]
Apparent magnitude (V) 5.9949[3]
Characteristics
Spectral type G1V[4]
U−B color index +0.01[5]
B−V color index 0.576[3]
Variable type BY Dra
Astrometry
Radial velocity (Rv)−1.5[6] km/s
Proper motion (μ) RA: 143.91[3] mas/yr
Dec.: 32.69[3] mas/yr
Parallax (π)55.03 ± 0.34 mas[3]
Distance59.3 ± 0.4 ly
(18.2 ± 0.1 pc)
Details
Mass0.97[4] M☉
Surface gravity (log g)4.18[4] cgs
Temperature5,780[4] K
Metallicity[Fe/H] = -0.20[4] or 0.00[7]
Age4.7[8] or 0.5[7] Gyr
Other designations
HP Boötis, GJ 564, BD+24° 2786, HD 130948, FK5 3172, HIP 72567, HR 5534, SAO 83553.[5]
Database references
SIMBADdata

HD 130948 or HP Boötis is a variable star with 2 brown dwarfs in the constellation Boötes. It has a stellar classification of G1V, which means it is a main sequence star with a mass and surface temperature that are similar to the Sun. The estimated age of this star is also similar to the Sun at 4.7 billion years (Gyr) old, but it has a lower proportion of elements (63%) other than hydrogen or helium. However, a separate study in 2009 gave a much younger age of 0.5 ± 0.3 Gyr and a higher metallicity that is very similar to the Sun.[7]

In 2002, a pair of co-orbiting brown dwarfs were discovered in orbit around this star. They were found using an adaptive optics instrument on the Gemini North 8m telescope in Hawaii.[9] The pair have a 10-year orbital period about the primary star, and their combined mass is 10.9% of the Sun's mass.[7]

The space velocity components of this star through the Milky Way galaxy are (U, V, W) = (−14.0, 14.7, −0.1).[4]

References

  1. ^ Gaidos, E. J.; Henry, G. W.; Henry, S. M. (August 2000). "Spectroscopy and Photometry of Nearby Young Solar Analogs". The Astronomical Journal. 120 (2): 1006–1013. Bibcode:2000AJ....120.1006G. doi:10.1086/301488. S2CID 16930014.
  2. ^ a b Perryman, M. A. C.; et al. (April 1997). "The HIPPARCOS Catalogue". Astronomy & Astrophysics. 323: L49–L52. Bibcode:1997A&A...323L..49P.
  3. ^ a b c d e van Leeuwen, F. (November 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.
  4. ^ a b c d e f Chen, Y. Q.; Nissen, P. E.; Zhao, G.; Zhang, H. W.; Benoni, T. (February 2000). "Chemical composition of 90 F and G disk dwarfs". Astronomy and Astrophysics Supplement. 141 (3): 491–506. arXiv:astro-ph/9912342. Bibcode:2000A&AS..141..491C. doi:10.1051/aas:2000124. S2CID 16273589.
  5. ^ a b "V* HP Boo -- Variable of BY Dra type". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2010-10-03.
  6. ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: International Astronomical Union. Bibcode:1967IAUS...30...57E.
  7. ^ a b c d Dupuy, Trent J.; Liu, Michael C.; Ireland, Michael J. (February 2009). "Dynamical Mass of the Substellar Benchmark Binary HD 130948BC". The Astrophysical Journal. 692 (1): 729–752. arXiv:0807.2450. Bibcode:2009ApJ...692..729D. doi:10.1088/0004-637X/692/1/729. S2CID 119237470.
  8. ^ Holmberg, J.; Nordstrom, B.; Andersen, J. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics. 501 (3): 941–947. arXiv:0811.3982. Bibcode:2009A&A...501..941H. doi:10.1051/0004-6361/200811191. S2CID 118577511.
  9. ^ Potter, Daniel; Martín, Eduardo L.; Cushing, Michael C.; Baudoz, Pierre; Brandner, Wolfgang; Guyon, Olivier; Neuhäuser, Ralph (March 2002). "Hokupa'a-Gemini Discovery of Two Ultracool Companions to the Young Star HD 130948". The Astrophysical Journal. 567 (2): L133–L136. arXiv:astro-ph/0201431. Bibcode:2002ApJ...567L.133P. doi:10.1086/339999. S2CID 16249194.
Stub icon

This variable star–related article is a stub. You can help Wikipedia by expanding it.

This page was last edited on 4 March 2024, at 18:23
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