HR 5553

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HR 5553
Observation data
Epoch 2000      Equinox 2000
Constellation Boötes
Right ascension  14h 53m 23.76674s[1]
Declination +19° 09′ 10.0813″[1]
Apparent magnitude (V) 6.00[2]
Spectral type K0 V[3]
U−B color index +0.49[3]
B−V color index +0.84[3]
Radial velocity (Rv)29.82 ± 0.15[4] km/s
Proper motion (μ) RA: −442.23[1] mas/yr
Dec.: +217.61[1] mas/yr
Parallax (π)86.88 ± 0.46[1] mas
Distance37.5 ± 0.2 ly
(11.51 ± 0.06 pc)
Absolute magnitude (MV)5.69[5]
Period (P)125.396 ± 0.001 d
Semi-major axis (a)0.19 ± 0.03 AU
Eccentricity (e)0.51 ± 0.001
Inclination (i)93.4 ± 4.2°
Longitude of the node (Ω)248.3° ± 3.6°
Argument of periastron (ω)
219° ± 0.1°
HR 5553 A
Mass0.84[6] M
Radius0.86[6] R
Luminosity0.498[6] L
Surface gravity (log g)4.57[7] cgs
Temperature5,313[7] K
Metallicity [Fe/H]0.10[7] dex
Rotational velocity (v sin i)4.0[7] km/s
Age0.7–1.3[8] Gyr
HR 5553 B
Mass0.45[3] M
Other designations
DE Boötis, BD+19 2881, GJ 567, HD 131511, HIP 72848, LHS 5279.
Database references

HR 5553 is a binary star system located thirty-eight light-years away, in the constellation Boötes. The combined spectrum of the pair matches that of a K-type main sequence star with a stellar classification of K0 V. The two stars orbit each other with a period of 125 days and a large eccentricity of 0.51.[3]

An infrared excess has been detected around this star, most likely indicating the presence of a circumstellar disk at a radius of 34.2 AU. The temperature of this dust is 40 K.[7] The estimated mass of the dust is 0.0002 times the mass of the Earth.[6]

Observational history[edit]

A spectroscopic binary orbit was first calculated in 1981 using radial velocity measurements from David Dunlap Observatory combined with older measurements from Mount Wilson Observatory and Dominion Astrophysical Observatory.[9]


  1. ^ a b c d e van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752v1, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
  2. ^ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data.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. ^ a b c d e f Kennedy, Grant M. (February 2015), "Nature or nurture of coplanar Tatooines: the aligned circumbinary Kuiper belt analogue around HD 131511", Monthly Notices of the Royal Astronomical Society: Letters, 447 (1): L75–L79, arXiv:1412.0674, Bibcode:2015MNRAS.447L..75K, doi:10.1093/mnrasl/slu190.
  4. ^ Karataş, Y.; et al. (April 2004), "Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution", Monthly Notices of the Royal Astronomical Society, 349 (3): 1069–1092, arXiv:astro-ph/0404219, Bibcode:2004MNRAS.349.1069K, doi:10.1111/j.1365-2966.2004.07588.x.
  5. ^ Holmberg, J.; et al. (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.
  6. ^ a b c d Marshall, J. P.; et al. (October 2014), "Interpreting the extended emission around three nearby debris disc host stars", Astronomy & Astrophysics, 570: 13, arXiv:1408.5649, Bibcode:2014A&A...570A.114M, doi:10.1051/0004-6361/201424517, A114.
  7. ^ a b c d e f Eiroa, C.; et al. (July 2013), "DUst around NEarby Stars. The survey observational results", Astronomy & Astrophysics, 555: A11, arXiv:1305.0155, Bibcode:2013A&A...555A..11E, doi:10.1051/0004-6361/201321050.
  8. ^ Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal, 687 (2): 1264–1293, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785.
  9. ^ Kamper, K. W.; Lyons, R. W. (1981). "The Spectroscopic Orbits of HD131511". Journal of the Royal Astronomical Society of Canada. 75: 56–58. Bibcode:1981JRASC..75...56K.

External links[edit]