Movatterモバイル変換

[0]ホーム
URL:

Jump to content
WikipediaThe Free Encyclopedia
Search

Upsilon Serpentis

From Wikipedia, the free encyclopedia
Star in the constellation Serpens
Upsilon Serpentis
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationSerpens[1]
Right ascension15h 47m 17.31882s[2]
Declination+14° 06′ 55.2617″[2]
Apparent magnitude (V)+5.70[3]
Characteristics
Spectral typeA3 V[4]
U−Bcolor index+0.09[3]
B−Vcolor index+0.10[3]
Astrometry
Radial velocity (Rv)−34.2±2.9[5] km/s
Proper motion (μ)RA: −55.49[2]mas/yr
Dec.: +32.42[2]mas/yr
Parallax (π)13.04±0.84 mas[2]
Distance250 ± 20 ly
(77 ± 5 pc)
Absolute magnitude (MV)+1.30[1]
Details
Mass2.9±0.23[6] M☉
Radius2.2[7] R☉
Luminosity23[8] L☉
Surface gravity (log g)4.0±0.14[6] cgs
Temperature8,917±303[6] K
Rotational velocity (v sin i)133[9] km/s
Age403+70
−75[6] Myr
Other designations
υ Ser,31 Serpentis,BD+14°2939,HD 141187,HIP 77336,HR 5870,SAO 101739[10]
Database references
SIMBADdata

Upsilon Serpentis,Latinized from υ Serpentis, is astar in the Serpens Caput section of theconstellationSerpens. Based upon an annualparallax shift of 13.04 mas as seen from Earth, it is located around 250 light years from theSun. The star is bright enough to be faintly visible to the naked eye, having anapparent visual magnitude of +5.70.[3] It is a member of theHyades group, a stream of stars that share a similar trajectory to theHyades cluster.[11]

This is anA-type main sequence star with astellar classification of A3 V.[4] It has an estimated 2.9 times themass of the Sun[6] and around 2.2 times theSun's radius.[7] With an age of 403 million years,[6] it has a high rate of spin with aprojected rotational velocity of 133 km/s.[9] It is radiating 23 times thesolar luminosity[8] from itsphotosphere at aneffective temperature of 8,917 K.[6]

Upsilon Serpentis is a suspectedastrometric binary,[12] which means an undetected companion isperturbing the motion of the visible star. AnX-ray emission has been detected from this system with a luminosity of247.8×1020 W. This may be coming from the companion, since A-type stars are not expected to emit X-rays.[13]

References

[edit]
  1. ^abAnderson, 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.
  2. ^abcdevan 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.
  3. ^abcdMermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)",Catalogue of Eggen's UBV Data,SIMBAD,Bibcode:1986EgUBV........0M.
  4. ^abCowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications",Astronomical Journal,74:375–406,Bibcode:1969AJ.....74..375C,doi:10.1086/110819.
  5. ^de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project",Astronomy & Astrophysics,546: 14,arXiv:1208.3048,Bibcode:2012A&A...546A..61D,doi:10.1051/0004-6361/201219219,S2CID 59451347, A61.
  6. ^abcdefgGullikson, Kevin; et al. (August 2016), "The Close Companion Mass-ratio Distribution of Intermediate-mass Stars",The Astronomical Journal,152 (2): 13,arXiv:1604.06456,Bibcode:2016AJ....152...40G,doi:10.3847/0004-6256/152/2/40,S2CID 119179065, 40.
  7. ^abPasinetti 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.
  8. ^abMcDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars",Monthly Notices of the Royal Astronomical Society,427 (1):343–57,arXiv:1208.2037,Bibcode:2012MNRAS.427..343M,doi:10.1111/j.1365-2966.2012.21873.x,S2CID 118665352.
  9. ^abRoyer, F.; et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions",Astronomy and Astrophysics,463 (2):671–682,arXiv:astro-ph/0610785,Bibcode:2007A&A...463..671R,doi:10.1051/0004-6361:20065224,S2CID 18475298.
  10. ^"phi Ser".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2017-03-23.{{cite web}}: CS1 maint: postscript (link)
  11. ^Eggen, O. J. (October 1982), "The Hyades main sequence",Astrophysical Journal Supplement Series,50:221–239,Bibcode:1982ApJS...50..221E,doi:10.1086/190826.
  12. ^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.
  13. ^Schröder, C.; Schmitt, J. H. M. M. (November 2007), "X-ray emission from A-type stars",Astronomy and Astrophysics,475 (2):677–684,Bibcode:2007A&A...475..677S,doi:10.1051/0004-6361:20077429.
Stars
Bayer
Flamsteed
Variable
HR
HD
Other
Exoplanets
Star
clusters
NGC
Other
Nebulae
Other
Galaxies
NGC
Other
Galaxy clusters
Retrieved from "https://en.wikipedia.org/w/index.php?title=Upsilon_Serpentis&oldid=1287064401"
Categories:
Hidden categories:
[8]ページ先頭
©2009-2025 Movatter.jp