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 | |
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
- 1 2 3 4 5 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. - ↑ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data. SIMBAD, Bibcode:1986EgUBV........0M.
- 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, arXiv:1412.0674, Bibcode:2015MNRAS.447L..75K, doi:10.1093/mnrasl/slu190.
- ↑ 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.
- 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, arXiv:1408.5649, Bibcode:2014A&A...570A.114M, doi:10.1051/0004-6361/201424517, A114.
- 1 2 3 4 5 6 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.
- ↑ 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
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