Observation data Epoch J2000.0 Equinox J2000.0 | |
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Constellation | Capricornus |
Right ascension | 20 32 23.695 |
Declination | −09° 51′ 12.18″ |
Apparent magnitude (V) | 5.65 |
Characteristics | |
Spectral type | G2 V |
U−B color index | +0.20 |
B−V color index | +0.68 |
Astrometry | |
Radial velocity (Rv) | +9.58 km/s |
Proper motion (μ) | RA: +309.736 mas/yr Dec.: +109.910 mas/yr |
Parallax (π) | 40.4241 ± 0.0497 mas |
Distance | 80.68 ± 0.10 ly (24.74 ± 0.03 pc) |
Details | |
HD 195564 A | |
Mass | 1.097 M☉ |
Radius | 1.867±0.083 R☉ |
Luminosity | 2.705±0.047 L☉ |
Surface gravity (log g) | 3.74 cgs |
Temperature | 5421±118 K |
Metallicity | +0.06 dex |
Rotational velocity (v sin i) | 1.91 km/s |
Age | 8.2 Gyr |
HD 195564 B | |
Mass | 0.55 M☉ |
Other designations | |
BD−10° 5423, FK5 1536, GJ 792.1, HD 195564, HIP 101345, HR 7845, SAO 163665 | |
Database references | |
SIMBAD | data |
ARICNS | data |
HD 195564 is the Henry Draper Catalogue designation for a star in the southern constellation of Capricornus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.65. Parallax measurements give us an estimate of its distance as 81 light years. This is a candidate wide binary system as a faint companion star shares a common proper motion with the brighter primary component.
Based upon the spectrum of light emitted by the primary, it has a stellar classification of G2 V. This indicates that it is a G-type main sequence star that is generating energy through the process of thermonuclear fusion in its core region. It has an estimated mass of 1.097 times the mass of the Sun, but a measured radius that is 1.867 times as large. As a result, it shines with 2.705 times the luminosity of the Sun. The abundance of elements in this star is similar to that in the Sun, although it is an older star with an age of around 8.2 billion years. The effective temperature of the stellar atmosphere is 5,421 K, giving it the yellow-hued glow of an ordinary K-type star.
The secondary companion has an apparent magnitude of 11.30, and a mass just 55% that of the Sun. As measured in 1965, it had an angular separation of 3.20″ from the primary, along a position angle of 27° The pair orbit each other with an estimated period of around 510 years.
In a paper published in April 2017, a candidate planet was found orbiting HD 195564 with a period of 5,404 days (14.80 yr).
Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
---|---|---|---|---|---|---|
b (unconfirmed) | — | — | 5403.77251±164.1426 | — | — | — |
References
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
- ^ Gray, R. O.; et al. (2003), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I", The Astronomical Journal, 126 (4): 2048–2059, arXiv:astro-ph/0308182, Bibcode:2003AJ....126.2048G, doi:10.1086/378365, S2CID 119417105.
- Nidever, David L.; et al. (August 2002), "Radial Velocities for 889 Late-Type Stars", The Astrophysical Journal Supplement Series, 141 (2): 503–522, arXiv:astro-ph/0112477, Bibcode:2002ApJS..141..503N, doi:10.1086/340570, S2CID 51814894.
- ^ Boyajian, Tabetha S.; et al. (July 2013), "Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations", The Astrophysical Journal, 771 (1): 31, arXiv:1306.2974, Bibcode:2013ApJ...771...40B, doi:10.1088/0004-637X/771/1/40, S2CID 14911430, 40. See Table 3.
- Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
- ^ Tokovinin, Andrei (April 2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal, 147 (4): 14, arXiv:1401.6827, Bibcode:2014AJ....147...87T, doi:10.1088/0004-6256/147/4/87, S2CID 56066740, 87.
- "HD 195564". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved March 15, 2016.
- "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16.
- ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920, retrieved 2015-07-22.
- ^ Butler, R. Paul; et al. (13 April 2017). "The LCES HIRES/Keck Precision Radial Velocity Exoplanet Survey". The Astronomical Journal. 153 (5): 208. arXiv:1702.03571. Bibcode:2017AJ....153..208B. doi:10.3847/1538-3881/aa66ca. hdl:2299/18220. S2CID 14954371. Planet candidate is in Table 2; full table available here.
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