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HR 5553

HR 5553

A visual band light curve for DE Boötes, adapted from Henry et al. (1995)[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Boötes
Right ascension 14h 53m 23.76674s[2]
Declination +19° 09′ 10.0813″[2]
Apparent magnitude (V) 6.00[3] (5.97 to 6.04)[4]
Characteristics
Spectral type K0 V[5]
U−B color index +0.49[5]
B−V color index +0.84[5]
Variable type RS CVn[4]
Astrometry
Radial velocity (Rv)−29.82±0.15[6] km/s
Proper motion (μ) RA: −442.23[2] mas/yr
Dec.: +217.61[2] mas/yr
Parallax (π)86.88 ± 0.46 mas[2]
Distance37.5 ± 0.2 ly
(11.51 ± 0.06 pc)
Absolute magnitude (MV)5.69[7]
Orbit[8]
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[9] M☉
Radius0.86[9] R☉
Luminosity0.498[9] L☉
Surface gravity (log g)4.57[10] cgs
Temperature5,313[10] K
Metallicity [Fe/H]0.10[10] dex
Rotation10.4[10]
Rotational velocity (v sin i)4.0[10] km/s
Age0.7–1.3[11] Gyr
HR 5553 B
Mass0.45[5] M☉
Other designations
DE Boo, BD+19°2881, GJ 567, HD 131511, HIP 72848, LHS 5279[12]
Database references
SIMBADdata

HR 5553 is a binary star system located thirty-eight light-years away from the Sun, in the northern constellation Boötes. It has the variable star designation DE Boötis, and is classified as an RS Canum Venaticorum variable that ranges in apparent visual magnitude from 5.97 down to 6.04,[4] which is bright enough to be dimly visible to the naked eye. The system is drifting closer to the Sun with a radial velocity of −30 km/s,[6] and is expected to come as close as 26.9 light-years in 210,000 years.[13]

Orbital elements for this single-lined spectroscopic binary 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.[14] The two stars orbit each other with a period of 125 days and a large eccentricity of 0.51.[5]

Marcel Golay listed the star as a suspected variable star in 1973.[15] Gregory W. Henry et al. confirmed that it is a variable star in 1995.[1] It was given its variable star designation, DE Boötis, in 1997.[16]

The primary, designated component A, is a K-type main sequence star with a stellar classification of K0 V. It is around one[11] billion years old and is spinning with a projected rotational velocity of 4 km/s.[10] The star has 84% of the mass of the Sun and 86% of the Sun's radius.[9] It is radiating 50%[9] of the luminosity of the Sun from its photosphere at an effective temperature of 5,313 K.[10] Component B has an estimated 45% of the mass of the Sun.[5]

An infrared excess has been detected around this system, most likely indicating the presence of a circumstellar disk at a radius of 34.2 AU. The temperature of this dust is 40 K.[10] The estimated mass of the dust is 0.0002 times the mass of the Earth. It is aligned to within 10° of the plane of the binary system.[9][8]

References

  1. ^ a b Henry, Gregory W.; Fekel, Francis C.; Hall, Douglas S. (December 1995). "An Automated Search for Variability in Chromospherically Active Stars". The Astronomical Journal. 110 (6): 2926–2967. Bibcode:1995AJ....110.2926H. doi:10.1086/117740. Retrieved 5 November 2021.
  2. ^ 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, S2CID 18759600.
  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.
  4. ^ a b c Samus', N. N; Kazarovets, E. V; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  5. ^ 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, S2CID 53686506.
  6. ^ a b Karataș, Yüksel; Bilir, Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (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. S2CID 15290475.
  7. ^ 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, S2CID 118577511.
  8. ^ a b Kennedy, G. 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. 447 (1): L75 – L79. arXiv:1412.0674. Bibcode:2015MNRAS.447L..75K. doi:10.1093/mnrasl/slu190.
  9. ^ a b c d e f 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, S2CID 119232172, A114.
  10. ^ a b c d e f g h 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, S2CID 377244.
  11. ^ a b 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, S2CID 27151456.
  12. ^ "DE Boo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-07.
  13. ^ Bailer-Jones, C.A.L.; et al. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics. 616: A37. arXiv:1805.07581. Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456. S2CID 56269929.
  14. ^ 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.
  15. ^ Golay, M. (1973). "Problems of Calibration of Absolute Magnitudes and Temperature of Stars. Proceedings of IAU Symposium no. 54 Held in Geneva, Switzerland, Sept. 12-15, 1972". Problems of Calibration of Absolute Magnitudes and Temperature of Stars. 54. Boston: Reidel: 275–297. Bibcode:1973IAUS...54..275G. doi:10.1007/978-94-010-2645-1_33. Retrieved 6 December 2024.
  16. ^ Kazarovets, E. V.; Samus, N. N. (April 1997). "The 73rd Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 4471: 1–45. Bibcode:1997IBVS.4471....1K. Retrieved 6 December 2024.
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