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]
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
Distance 37.5 ± 0.2 ly
(11.51 ± 0.06 pc)
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
Mass 0.84[5] M
Radius 0.86[5] R
Luminosity 0.498[5] L
Surface gravity (log g) 4.57[6] cgs
Temperature 5,313[6] K
Metallicity [Fe/H] 0.10[6] dex
Rotation 10.4[6]
Rotational velocity (v sin i) 4.0[6] km/s
Age 0.7–1.3[7] Gyr
HR 5553 B
Mass 0.45[3] M
Other designations
DE Boötis, BD+19 2881, GJ 567, HD 131511, HIP 72848, LHS 5279.

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.[6] The estimated mass of the dust is 0.0002 times the mass of the Earth.[5]

References[edit]

  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 ^ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data.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. ^ 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. 
  6. ^ 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. 
  7. ^ 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. 

External links[edit]