HR 5553

HR 5553
DEBooLightCurve.png
A visual bandlight 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]

주성분 A는 K형 주계열성으로 분류는 K0 V이다.그것은 약 10억[11] 년 된 것으로 예상 회전 속도 4km/[10]s로 회전하고 있다.이 별의 질량은 태양의 84%, 반지름은 [9]태양의 86%입니다.이 행성은 유효 온도 5,313 [10]K의 광구에서 태양 [9]광도의 50%를 방출하고 있습니다.성분 B의 [5]질량은 태양 질량의 45%로 추정됩니다.

이 시스템 주변에서 적외선 초과가 감지되었으며, 이는 반지름 34.2AU에 별 주위 원반이 존재함을 나타냅니다. 이 먼지의 온도는 40K입니다.[10]먼지의 추정 질량은 지구의 0.0002배이다.2진법 [9][8]평면에서 10° 이내로 정렬됩니다.

레퍼런스

  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. 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.

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