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

5 Vulpeculae

From Wikipedia, the free encyclopedia

5 Vulpeculae
5 Vul in the constellation Vulpecula (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Vulpecula
Right ascension 19h 26m 13.2463s[1]
Declination +20° 05′ 51.8394″[1]
Apparent magnitude (V) 5.65±0.010[2]
Characteristics
Spectral type A0 V[3]
Apparent magnitude (U) 5.62±0.012[2]
Apparent magnitude (B) 5.66±0.011[2]
Astrometry
Radial velocity (Rv)−20.9±2.9[4] km/s
Proper motion (μ) RA: +3.395±0.114[1] mas/yr
Dec.: −34.787±0.137[1] mas/yr
Parallax (π)13.8921 ± 0.0900 mas[1]
Distance235 ± 2 ly
(72.0 ± 0.5 pc)
Absolute magnitude (MV)1.29[5]
Details[3]
Mass2.33±0.02 M☉
Radius2.7[6] R☉
Luminosity34±2 L☉
Surface gravity (log g)4.0[7] cgs
Temperature9,840+91
−90 K
Rotational velocity (v sin i)154 km/s
Age198[7] Myr
Other designations
5 Vul, BD+19° 4015, HD 182919, HIP 95560, HR 7390, SAO 104831[8]
Database references
SIMBADdata

5 Vulpeculae is a single,[9] white-hued star in the northern constellation of Vulpecula.[8] It is situated amidst a random concentration of bright stars designated Collinder 399,[10] or Brocchi's Cluster. This is a faint star that is just visible to the naked eye with an apparent visual magnitude of 5.60.[4] Based upon an annual parallax shift of 13.8921±0.0900 mas,[1] it is located around 235 light years from the Sun. It is moving closer with a heliocentric radial velocity of −21 km/s,[4] and will make its closest approach in 2.5 million years at a separation of around 120 ly (36.89 pc).[5]

This is a young A-type main-sequence star with a stellar classification of A0 V.[3] It is a rapidly rotating star[11] with a projected rotational velocity of 154 km/s.[3] The star has an estimated 2.33[3] times the mass of the Sun and about 2.7[6] times the Sun's radius. It is radiating 34 times the Sun's luminosity from its photosphere at an effective temperature of 8,940 K.[3]

A warm debris disk was detected by the Spitzer Space Telescope at a temperature of 206 K (−89 °F; −67 °C), orbiting 13 Astronomical units from the host star.[12] Although this finding has not been directly detected, the emission signature indicates the disk is in the form of a thin ring. The emission displays weak transient absorption features that are indicative of kilometer-sized exocomets that are undergoing evaporation as they approach the host star.[11] These absorption features have been observed to vary on time scales of hours, days, or months.[13]

References

  1. ^ a b c d e f 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 Harmanec, P.; et al. (2020). "A new study of the spectroscopic binary 7 Vul with a Be star primary". Astronomy and Astrophysics. 639. Table A.1. arXiv:2005.11089. Bibcode:2020A&A...639A..32H. doi:10.1051/0004-6361/202037964. S2CID 218862853.
  3. ^ a b c d e f Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  4. ^ a b c Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
  5. ^ a b 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.
  6. ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (2) (3rd ed.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  7. ^ a b Chen, Christine H.; et al. (2014), "The Spitzer Infrared Spectrograph Debris Disk Catalog. I. Continuum Analysis of Unresolved Targets", The Astrophysical Journal Supplement, 211 (3): 22, Bibcode:2014ApJS..211...25C, doi:10.1088/0067-0049/211/2/25, 25.
  8. ^ a b "5 Vul". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-04-13.
  9. ^ 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.
  10. ^ Baumgardt, H. (December 1998), "The nature of some doubtful open clusters as revealed by HIPPARCOS", Astronomy and Astrophysics, 340: 402–414, Bibcode:1998A&A...340..402B.
  11. ^ a b Montgomery, Sharon L.; Welsh, Barry Y. (October 2012), "Detection of Variable Gaseous Absorption Features in the Debris Disks Around Young A-type Stars", Publications of the Astronomical Society of the Pacific, 124 (920): 1042, Bibcode:2012PASP..124.1042M, doi:10.1086/668293
  12. ^ Morales, Farisa Y.; et al. (2009), "Spitzer mid-Ir Spectra of Dust Debris Around A and Late B Type Stars: Asteroid Belt Analogs and Power-Law Dust Distributions" (PDF), The Astrophysical Journal, 699 (2): 1067–1086, Bibcode:2009ApJ...699.1067M, doi:10.1088/0004-637X/699/2/1067, S2CID 45235873.
  13. ^ Montgomery, Sharon L.; Welsh, B.; Lallement, R.; Timbs, B. W. (January 2014), "Exocomet Gas: Now You See It, Now You Don't", American Astronomical Society, AAS Meeting #223, 223: 401.02, Bibcode:2014AAS...22340102M, 401.02.

External links

This page was last edited on 25 February 2023, at 12:38
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