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36 Serpentis

From Wikipedia, the free encyclopedia
Star in the constellation Serpens
This article is about b Serpentis. Not to be confused withβ (Beta) Serpentis.
36 Serpentis
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationSerpens
Right ascension15h 51m 15.59418s[1]
Declination−03° 05′ 25.7938″[1]
Apparent magnitude (V)5.09[2](5.2 + 7.8)[3]
Characteristics
Spectral typeA3Vn[4] or A2IV-Vn[5](A7 + G0)[6]
U−Bcolor index+0.07[7]
B−Vcolor index+0.12[7]
Astrometry
Radial velocity (Rv)−8[8] km/s
Proper motion (μ)RA: −91.09[1]mas/yr
Dec.: −28.21[1]mas/yr
Parallax (π)20.10±0.33 mas[1]
Distance162 ± 3 ly
(49.8 ± 0.8 pc)
Absolute magnitude (MV)1.61[2]
Orbit[6]
Period (P)50.6±1.5yr
Semi-major axis (a)0.400±0.006″
Eccentricity (e)0.8323±0.0047
Inclination (i)98.08±0.31°
Longitude of the node (Ω)74.00±0.31°
Periastronepoch (T)2002.78±0.17
Argument of periastron (ω)
(secondary)		72.84±0.91°
Details
36 Ser A
Mass2.04[9] M☉
Radius1.65[10] R☉
Luminosity19.13[2] L☉
Surface gravity (log g)3.89[11] cgs
Temperature8246[11] K
Metallicity [Fe/H]−2.00[11] dex
Rotational velocity (v sin i)229[12] km/s
Age723[9] Myr
Other designations
b Ser,36 Ser,BD−02°4058,FK5 2249,GC 4210,HD 141851,HIP 77660,HR 5895,SAO 140801,WDS J15513-0305[13]
Database references
SIMBADdata

36 Serpentis is abinary star[14] system in theequatorialconstellation ofSerpens. It has theBayer designationb Serpentis, while36 Serpentis is theFlamsteed designation.[13] The system is visible to the naked eye as a dim, white-hued point of light with a combinedapparent visual magnitude of 5.09.[2] It is located 162 light years away from the Sun based onparallax,[1] and is moving closer with aradial velocity of −8 km/s.[8]

This is aspectroscopic binary star system with a longorbital period of 52.8 years and a higheccentricity of 0.83. The combined mass of the pair is3.09±0.28 M☉.[6] Gray et al. (2017) found a mergedstellar classification of A2IV-Vn for this system,[5] while Cowley et al. matched it with a class of A3Vn,[4] where the 'n' indicates "nebulous"lines caused by rapid rotation.

The primary component is aLambda Boötis star, meaning that it has solar-like amounts ofcarbon,nitrogen, andoxygen, while containing very low amounts ofiron peak elements.[15] It is an A7[6] classmain sequence star of visual magnitude 5.2[3] that is spinning rapidly, showing aprojected rotational velocity of 229.[12] The star is 723[9] million years old with around double themass of the Sun. It is radiating 19[2] times theSun's luminosity from itsphotosphere at aneffective temperature of 8,246 K.[11]

The cooler secondary component, a G0 star,[6] is the source for theX-ray emission that has been detected coming from this system.[6] It has a visual magnitude of 7.8.[3]

References

[edit]
  1. ^abcdefvan 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.
  2. ^abcdeAnderson, 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. ^abcDocobo, José A.; et al. (2010)."EMCCD Speckle Interferometry with the 6 m Telescope: Astrometric Measurements, Differential Photometry, and Orbits".The Astronomical Journal.140 (4):1078–1083.Bibcode:2010AJ....140.1078D.doi:10.1088/0004-6256/140/4/1078.
  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. ^abGray, R. O.; et al. (July 2017)."The Discovery of λ Bootis Stars: The Southern Survey I".The Astronomical Journal.154 (1): 11.Bibcode:2017AJ....154...31G.doi:10.3847/1538-3881/aa6d5e. 31.
  6. ^abcdefMason, Brian D.; et al. (September 2010)."Binary Star Orbits. IV. Orbits of 18 Southern Interferometric Pairs".The Astronomical Journal.140 (3):735–743.Bibcode:2010AJ....140..735M.doi:10.1088/0004-6256/140/3/735.
  7. ^abJohnson, H. L. (1966). "UBVRIJKL Photometry of the Bright Stars".Communications of the Lunar and Planetary Laboratory.4: 99.Bibcode:1966CoLPL...4...99J.
  8. ^abWilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities".Carnegie Institute Washington D.C. Publication.Bibcode:1953GCRV..C......0W.
  9. ^abcDavid, 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,arXiv:1501.03154,Bibcode:2015ApJ...804..146D,doi:10.1088/0004-637X/804/2/146,S2CID 33401607.
  10. ^Pasinetti Fracassini, L. E.; et al. (2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)".Astronomy & Astrophysics.367 (Third ed.):521–24.arXiv:astro-ph/0012289.Bibcode:2001A&A...367..521P.doi:10.1051/0004-6361:20000451.S2CID 425754.
  11. ^abcdPrugniel, Ph.; et al. (1986). "The atmospheric parameters and spectral interpolator for the MILES stars".Astronomy & Astrophysics.531: A165.arXiv:1104.4952.Bibcode:2011A&A...531A.165P.doi:10.1051/0004-6361/201116769.S2CID 54940439.
  12. ^abRoyer, F.; et al. (2007). "Rotational velocities of A-type stars. III. Velocity distributions".Astronomy & Astrophysics.463 (2):671–682.arXiv:astro-ph/0610785.Bibcode:2007A&A...463..671R.doi:10.1051/0004-6361:20065224.S2CID 18475298.
  13. ^ab"36 Ser".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2019-07-14.
  14. ^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.
  15. ^Nikolov, G.; et al. (April 2008). "Spectroscopic orbit determination of two metal-weak dwarf stars: HD64491 and HD141851".Contributions of the Astronomical Observatory Skalnaté Pleso.38 (2):433–434.Bibcode:2008CoSka..38..433N.
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