HR 5553

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]
Characteristics
Spectral type K0 V[3]
U−B color index +0.49[3]
B−V color index +0.84[3]
Astrometry
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]
Orbit[3]
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)
(secondary)		219° ± 0.1°
Details
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
Rotation10.4[7]
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
SIMBADdata

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]

References

  1. 1 2 3 4 5 van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, Bibcode:2007A&A...474..653V, arXiv:0708.1752v1 Freely accessible, 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 ↑ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data.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. 1 2 3 4 5 6 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, Bibcode:2015MNRAS.447L..75K, arXiv:1412.0674 Freely accessible, 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, Bibcode:2004MNRAS.349.1069K, arXiv:astro-ph/0404219 Freely accessible, 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, Bibcode:2009A&A...501..941H, arXiv:0811.3982 Freely accessible, doi:10.1051/0004-6361/200811191.
  6. 1 2 3 4 Marshall, J. P.; et al. (October 2014), "Interpreting the extended emission around three nearby debris disc host stars", Astronomy & Astrophysics, 570: 13, Bibcode:2014A&A...570A.114M, arXiv:1408.5649 Freely accessible, doi:10.1051/0004-6361/201424517, A114.
  7. 1 2 3 4 5 6 Eiroa, C.; et al. (July 2013), "DUst around NEarby Stars. The survey observational results", Astronomy & Astrophysics, 555: A11, Bibcode:2013A&A...555A..11E, arXiv:1305.0155 Freely accessible, 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, Bibcode:2008ApJ...687.1264M, arXiv:0807.1686 Freely accessible, doi:10.1086/591785.


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