Astronomy:HR 5553

From HandWiki
Short description: Binary star system in the constellation Boötes
HR 5553
DEBooLightCurve.png
A visual band light curve for DE Boötes, adapted from Henry et al. (1995)[1]
Observation data
Equinox J2000.0]] (ICRS)
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[2] mas
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 astronomical unit|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]

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. ↑ 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. doi:10.1086/117740. Bibcode: 1995AJ....110.2926H. https://ui.adsabs.harvard.edu/abs/1995AJ....110.2926H. Retrieved 5 November 2021. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  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. ↑ 4.0 4.1 4.2 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. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 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, doi:10.1093/mnrasl/slu190, Bibcode: 2015MNRAS.447L..75K. 
  6. ↑ 6.0 6.1 Karataș, Yüksel; Bilir, Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R. et al. (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. doi:10.1111/j.1365-2966.2004.07588.x. Bibcode: 2004MNRAS.349.1069K. 
  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, doi:10.1051/0004-6361/200811191, Bibcode: 2009A&A...501..941H. 
  8. ↑ 8.0 8.1 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. doi:10.1093/mnrasl/slu190. Bibcode: 2015MNRAS.447L..75K. 
  9. ↑ 9.0 9.1 9.2 9.3 9.4 9.5 Marshall, J. P. et al. (October 2014), "Interpreting the extended emission around three nearby debris disc host stars", Astronomy & Astrophysics 570: 13, doi:10.1051/0004-6361/201424517, A114, Bibcode: 2014A&A...570A.114M. 
  10. ↑ 10.0 10.1 10.2 10.3 10.4 10.5 10.6 10.7 Eiroa, C. et al. (July 2013), "DUst around NEarby Stars. The survey observational results", Astronomy & Astrophysics 555: A11, doi:10.1051/0004-6361/201321050, Bibcode: 2013A&A...555A..11E. 
  11. ↑ 11.0 11.1 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, doi:10.1086/591785, Bibcode: 2008ApJ...687.1264M. 
  12. ↑ "DE Boo". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=DE+Boo. 
  13. ↑ Bailer-Jones, C.A.L. et al. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics 616: A37. doi:10.1051/0004-6361/201833456. Bibcode: 2018A&A...616A..37B. 
  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. 

External links



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:HR_5553&oldid=3423921"