ZZ Boötis
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Boötes |
| Right ascension | 13h 56m 09.5178s[1] |
| Declination | +25° 55′ 07.3547″[1] |
| Apparent magnitude (V) | 6.79 - 7.44[2] |
| Characteristics | |
| Spectral type | F2 IV-V + F2 IV-V[3] |
| B−V color index | +0.36[4] |
| Variable type | Algol[2] |
| Astrometry | |
| Radial velocity (Rv) | -29.50[5] km/s |
| Proper motion (μ) | RA: −97.004±0.057[1] mas/yr Dec.: −6.164±0.061[1] mas/yr |
| Parallax (π) | 9.3114 ± 0.0381 mas[1] |
| Distance | 350 ± 1 ly (107.4 ± 0.4 pc) |
| Absolute bolometric magnitude (Mbol) | 2.17 / 2.30[3] |
| Orbit[3] | |
| Period (P) | 4.991744 d |
| Inclination (i) | 88.6 ± 0.1° |
| Semi-amplitude (K1) (primary) | 93.7 ± 2.1 km/s |
| Semi-amplitude (K2) (secondary) | 94.0 ± 2.1 km/s |
| Details | |
| ZZ Boo A | |
| Mass | 1.71 ± 0.06[3] M☉ |
| Radius | 2.28 ± 0.06[3] R☉ |
| Luminosity | 10.7[3] L☉ |
| Surface gravity (log g) | 3.72 ± 0.10[6] cgs |
| Temperature | 6860 ± 20[6] K |
| Metallicity [Fe/H] | −0.10 ± 0.08[6] dex |
| Rotational velocity (v sin i) | 11.9 ± 0.4[6] km/s |
| ZZ Boo B | |
| Mass | 1.70 ± 0.06[3] M☉ |
| Radius | 2.15 ± 0.06[3] R☉ |
| Luminosity | 9.95[3] L☉ |
| Surface gravity (log g) | 3.84 ± 0.10[6] cgs |
| Temperature | 6930 ± 20[6] K |
| Metallicity [Fe/H] | −0.03 ± 0.10[6] dex |
| Rotational velocity (v sin i) | 19.3 ± 0.8[6] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
ZZ Boötis is a star system in the constellation Boötes. It varies from magnitude 6.79 to 7.44 over 5 days.[8] Based on its parallax, measured by the Gaia spacecraft, it is about 350 light-years (107 parsecs) away.[1]
Observational history
In 1950 Grigory Shajn determined that this star is a double lined spectroscopic binary with, with an approximate period of 4.96 days. Sergei Gaposchkin found from an examination of photographic plates, in 1951, that it was an Algol type eclipsing binary system.[9] The primary and secondary eclipses are of equal depth, 0.65 magnitudes, meaning the brightness drops by nearly half.[2] The eclipses make up only 6% of the orbital period.[8]
ZZ Boötis is a binary star system, specifically an eclipsing binary.[8] The component stars appear to be of almost equal mass, differing by only 3%.[4]
References
- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
- ^ a b c d e f g h i Cester, B.; Giuricin, G.; Mardirossian, F.; Mezzetti, M. (1978). "Revised spectrographic and photometric elements of ZZ Boo". Astronomy and Astrophysics Supplement Series. 32: 347–350. Bibcode:1978A&AS...32..347C.
- ^ a b Popper, D. M. (1983). "The F-type eclipsing binaries ZZ Bootis, CW Eridani, and BK Pegasi". Astronomical Journal. 88: 1242–56. Bibcode:1983AJ.....88.1242P. doi:10.1086/113415. ISSN 0004-6256.
- ^ Pourbaix, D.; Tokovinin, A. A.; Batten, A. H.; Fekel, F. C.; Hartkopf, W. I.; Levato, H.; Morrell, N. I.; Torres, G.; Udry, S. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213.
- ^ a b c d e f g h Kang, Young-Woon; Yushchenko, Alexander; Hong, Kyengsoo; Kim, Sungeun; Yushchenko, Volodymyr (2012). "Chemical Composition of the Components of Eclipsing Binary Star ZZ Bootis". The Astronomical Journal. 144 (2): 35–45. Bibcode:2012AJ....144...35K. doi:10.1088/0004-6256/144/2/35.
- ^ "ZZ Boo". SIMBAD. Centre de données astronomiques de Strasbourg.
- ^ a b c Watson, Christopher (4 January 2010). "ZZ Boötis". AAVSO Website. American Association of Variable Star Observers. Retrieved 5 August 2014.
- ^ Gaposchkin, S. (1951). "The system of RZ Eridani and a new bright eclipsing variable with double-lined spectrum". The Astronomical Journal. 56: 125. Bibcode:1951AJ.....56..125G. doi:10.1086/106546.
