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Omicron Serpentis

Topic: Astronomy

 From HandWiki - Reading time: 4 min
Short description: Star in the constellation Serpens
Omicron Serpentis
Observation data
Equinox J2000.0]] (ICRS)
Constellation Serpens
Right ascension  17h 41m 24.87286s[1]
Declination −12° 52′ 31.1086″[1]
Apparent magnitude (V) 4.26[2]
Characteristics
Spectral type A2 Va[3]
U−B color index +0.08[2]
B−V color index +0.07[2]
Variable type δ Sct[4]
Astrometry
Radial velocity (Rv)−30.2±1.2[5] km/s
Proper motion (μ) RA: −72.90[1] mas/yr
Dec.: −55.55[1] mas/yr
Parallax (π)18.83 ± 0.25[1] mas
Distance173 ± 2 ly
(53.1 ± 0.7 pc)
Absolute magnitude (MV)+0.760[6]
Details
Mass2.13[7] M☉
Radius2.2[8] R☉
Luminosity42.6[9] L☉
Surface gravity (log g)3.82±0.14[7] cgs
Temperature8,972±305[7] K
Rotational velocity (v sin i)112.6±1.2[10] km/s
Age518[7] Myr
Other designations
ο Ser, 56 Ser, BD−12° 4808, FK5 3405, HD 160613, HIP 86565, HR 6581, SAO 160747.[11]
Database references
SIMBADdata

Omicron Serpentis (ο Ser, ο Serpentis) is a solitary[12] star in the Serpens Cauda (tail) section of the equatorial constellation Serpens. Based upon an annual parallax shift of 18.83 mas as seen from Earth,[1] it is located around 173 light years from the Sun. The star is visible to the naked eye with a base apparent visual magnitude of +4.26.[2]

This is a white-hued A-type main sequence star with a stellar classification of A2 Va.[3] It is located on the lower instability strip[6] and is classified as a Delta Scuti type variable star. The apparent magnitude of the star varies in the range 4.26−4.27 with a period of 76 minutes, or 0.053 days.[6][13]

The star has an estimated 2.13[7] times the mass of the Sun and about 2.2[8] times the Sun's radius. It is about half a billion[7] years old and is spinning with a projected rotational velocity of 112.6 km/s.[10] Omicron Serpentis is radiating 42.6[9] times the solar luminosity from its photosphere at an effective temperature of 8,972 K.[7]

In 1909, the symbiotic nova[14] RT Serpentis appeared near Omicron, although it only reached a maximum magnitude of 10.[15]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 2.3 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data (SIMBAD), Bibcode: 1986EgUBV........0M. 
  3. ↑ 3.0 3.1 Houk, N. (1988), Michigan catalogue of two-dimensional spectral types for the HD stars, 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode: 1988mcts.book.....H. 
  4. ↑ Samus, N. N. et al. (2009), "General Catalogue of Variable Stars (Samus+ 2007-2013)", VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1, Bibcode: 2009yCat....102025S. 
  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, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D. 
  6. ↑ 6.0 6.1 6.2 Garcia, J. R. et al. (February 1995), "A catalogue of variable stars in the lower instability strip", Astronomy and Astrophysics Supplement 109: 201–262, Bibcode: 1995A&AS..109..201G. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D. 
  8. ↑ 8.0 8.1 Pasinetti Fracassini, L. E. et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics 367: 521–524, doi:10.1051/0004-6361:20000451, Bibcode: 2001A&A...367..521P. 
  9. ↑ 9.0 9.1 McDonald, I. et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society 427 (1): 343–57, doi:10.1111/j.1365-2966.2012.21873.x, Bibcode: 2012MNRAS.427..343M. 
  10. ↑ 10.0 10.1 Díaz, C. G. et al. (July 2011), "Accurate stellar rotational velocities using the Fourier transform of the cross correlation maximum", Astronomy & Astrophysics 531: A143, doi:10.1051/0004-6361/201016386, Bibcode: 2011A&A...531A.143D. 
  11. ↑ "omi Ser". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=omi+Ser. 
  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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  13. ↑ Chang, S.-W. et al. (2013), "Statistical Properties of Galactic δ Scuti Stars: Revisited", The Astronomical Journal 145 (5): 132, doi:10.1088/0004-6256/145/5/132, Bibcode: 2013AJ....145..132C. 
  14. ↑ Pavlenko, E. P.; Bochkov, V. V.; Vasil'yanovskaya, O. P. (1996). "9,6-Year periodicity of symbiotic nova RT Ser (1909) during the outburst decay from 1940 to 1994". Astrophysics 39 (1): 15–19. doi:10.1007/BF02044949. Bibcode: 1996Ap.....39...15P. 
  15. ↑ "RT Serpentis". AAVSO Website. American Association of Variable Star Observers. 1 April 2014. http://www.aavso.org/vsx/index.php?view=detail.top&oid=34603. 



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