UV Piscium

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UV Piscium
UVPscLightCurve.png
A light curve for UV Piscium plotted from TESS data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Pisces
Right ascension 01h 16m 55.119s [2]
Declination +06° 48′ 42.13″ [2]
Apparent magnitude  (V)8.98 [3]
Characteristics
Primary
Evolutionary stage Main sequence
Spectral type G5V [4]
B−V color index 0.65±0.02 [4]
Variable type Detached Algol + RS CVn [5]
Secondary
Evolutionary stage Main sequence
Spectral type K3V [4]
B−V color index 1.04±0.07 [4]
Astrometry
Radial velocity (Rv)6.45±0.40 [6]  km/s
Proper motion (μ)RA: +85.250  mas/yr [2]
Dec.: +20.946  mas/yr [2]
Parallax (π)14.0593 ± 0.0236  mas [2]
Distance 232.0 ± 0.4  ly
(71.1 ± 0.1  pc)
Absolute magnitude  (MV)4.48±0.05 [4]
Orbit [7]
Period (P)0.86104716 d
Eccentricity (e)0.0 (assumed)
Inclination (i)88.9±2.0 [4] °
Periastron epoch (T)2,448,897.4226±0.0003  HJD
Semi-amplitude (K1)
(primary)		117.20±0.18 km/s
Semi-amplitude (K2)
(secondary)		154.81±0.37 km/s
Details [7]
Primary
Mass 1.0225±0.0058  M☉
Radius 1.096  R☉
Surface gravity (log g)4.340±0.018  cgs
Temperature 5,780±100  K
Metallicity [Fe/H]0.025±0.066 [8]   dex
Rotation 0.86 d
Rotational velocity (v sin i)71.01+0.37
−0.36 km/s
Age 4.7  Gyr
Secondary
Mass 0.7741±0.0034  M☉
Radius 0.829  R☉
Surface gravity (log g)4.478±0.019  cgs
Temperature 4,750±80  K
Rotation 0.86 d
Rotational velocity (v sin i)51.66+1.25
−1.20 km/s
Other designations
UV Psc, BD+06°189, HD  7700, HIP  5980, SAO  109778 [9]
Database references
SIMBAD data

UV Piscium is a binary star system in the constellation of Pisces. With a peak apparent visual magnitude of 8.98, [3] it is too faint to be visible to the naked eye. This is an eclipsing binary system that decreases to magnitude 10.05 during the primary eclipse, then to magnitude 9.54 with the secondary eclipse. It is located at a distance of 232  light years from the Sun based on parallax measurements, [2] and is receding with a radial velocity of 6.5 km/s. [6] The position of this star near the ecliptic means it is subject to lunar occultation. [10]

This star was found to be variable by H. Huth in 1959. [11] He determined it to be an eclipsing binary and published the first light curve with a period of 20.67 hours. R. B. Carr in 1969 proposed this to be an Algol-type variable with a minor tidal distortion of the components, plus a large, anomalous asymmetry in the light curve. [12] D. S. Hall in 1976 grouped it among the class of short-period RS CVn binaries. [13] The following year, variable, non-thermal radio emission was detected coming from this system, the first such discovered for a short-period binary. [14]

Daniel M. Popper in 1969 found a double-lined, G-type spectrum with both components showing emission in the H and K lines. [15] In 1979, A. R. Sadik deduced the system is a detached binary and suggested a bright, hot spot may produce the observed asymmetry in the light curve. He found stellar classifications of G2V and K0IV for the primary and secondary components, respectively. [12] With improved spectra, Popper found main sequence classes of G5 and K3 for the two stars. [4] The presence of a prominence was deduced in 1992, and a flare of hydrogen alpha was observed the following year. [16]

This is a close binary system with an orbital period of 0.86 days. The orbit is circular and the components are spinning rapidly in-sync with their orbital period. This rotation rate is making both stars magnetically active, with average magnetic field strengths of 137  G and 88 G for the primary and secondary, respectively. Magnetic activity cycles appear to be causing the orbital period to oscillate with a 61 year period. [17] The primary is a G-type main-sequence star of about the same size and mass as the Sun, while the secondary is a smaller K-type main-sequence star. They are estimated to be about 4.6 billion years old. [7]

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<span class="mw-page-title-main">ER Vulpeculae</span> Variable star in the constellation Vulpecula

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<span class="mw-page-title-main">VV Ursae Majoris</span> Variable star system in the constellation Ursa Major

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<span class="mw-page-title-main">AW Ursae Majoris</span> Variable star in the constellation Ursa Major

AW Ursae Majoris is a binary star system in the northern circumpolar constellation of Ursa Major, abbreviated AW UMa. It is an A-type W Ursae Majoris variable with an apparent visual magnitude of 6.83, which is near the lower limit of visibility to the naked eye. This is an eclipsing binary with the brightness dropping to magnitude 7.13 during the primary eclipse and to 7.08 with the secondary eclipse. Parallax measurements give a distance estimate of 221 light years from the Sun. It is drifting closer to the Sun with a radial velocity of approximately −17 km/s. The system has a high proper motion, traversing the celestial sphere at the rate of 0.216 arc second per annum.

<span class="mw-page-title-main">DM Ursae Majoris</span> Variable star in the constellation Ursa Major

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<span class="mw-page-title-main">DW Ursae Majoris</span> Variable star in the constellation Ursa Major

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<span class="mw-page-title-main">RT Persei</span> Star system in the constellation Perseus

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<span class="mw-page-title-main">DV Piscium</span> Multiple star system in the constellation Pisces

DV Piscium is a triple star system in the equatorial constellation of Pisces, abbreviated DV Psc. It is an eclipsing binary variable of the RS Canum Venaticorum class. The pair have a combined apparent visual magnitude of 10.59, which is too faint to be visible with the naked eye. Based on parallax measurements, DV Piscium is located at a distance of 137.5 light years from the Sun. It is drifting closer with a radial velocity of −28 km/s.

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. 1 2 3 4 5 6 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.
  3. 1 2 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  4. 1 2 3 4 5 6 7 Popper, Daniel M. (September 1997), "Orbits of detached main-sequence eclipsing binaries of types late F to K. II. UV Leonis, UV Piscium, and BH Virginis", The Astronomical Journal, 114: 1195, Bibcode:1997AJ....114.1195P, doi:10.1086/118552.
  5. ↑ Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports , 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  6. 1 2 Karataș, Yüksel; 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, arXiv: astro-ph/0404219 , Bibcode:2004MNRAS.349.1069K, doi:10.1111/j.1365-2966.2004.07588.x, S2CID   15290475.
  7. 1 2 3 Hahlin, A.; et al. (June 2021), "Magnetic field of the eclipsing binary UV Piscium", Astronomy & Astrophysics, 650: 17, arXiv: 2105.02542 , Bibcode:2021A&A...650A.197H, doi:10.1051/0004-6361/202140832, S2CID   233864794, A197.
  8. ↑ Qian, S. -B.; et al. (March 2018), "Physical Properties and Evolutionary States of EA-type Eclipsing Binaries Observed by LAMOST", The Astrophysical Journal Supplement Series, 235 (1): 12, arXiv: 1712.09026 , Bibcode:2018ApJS..235....5Q, doi:10.3847/1538-4365/aaa601, S2CID   119102391, 5.
  9. ↑ "UV Psc". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 8 July 2022.
  10. ↑ Herr, Richard B. (April 1969), "Identification List of Spectroscopic and Eclipsing Binaries Subject to Occultations by the Moon", Publications of the Astronomical Society of the Pacific, 81 (479): 105, Bibcode:1969PASP...81..105H, doi:10.1086/128748, S2CID   123513287.
  11. ↑ Huth, H. (1959), Mitteilungen über Veränderliche Sterne, 424.
  12. 1 2 Sadik, A. R. (July 1979), "Light and Colour Curve Observations and Analysis of the Short Period Eclipsing Binary System UV Psc", Astrophysics and Space Science, 63 (2): 319–349, Bibcode:1979Ap&SS..63..319S, doi:10.1007/BF00638905, S2CID   122684321.
  13. ↑ Hall, D. S. (1976), Fitch, W. S. (ed.), "The RS CVn Binaries and Binaries with Similar Properties", Multiple Periodic Variable Stars, Proceedings of IAU Colloq. 29, held in Budapest, Hungary, 1–5 September 1975, Astrophysics and Space Science Library, D. Reidel Publishers, vol. 60, p. 287, Bibcode:1976ASSL...60..287H, doi:10.1007/978-94-010-1175-4_15, ISBN   978-94-010-1177-8, S2CID   120775716.
  14. ↑ Spangler, S. R.; et al. (December 1977), "Radio survey of close binary stars", Astronomical Journal, 82: 989–997, Bibcode:1977AJ.....82..989S, doi:10.1086/112161.
  15. ↑ Popper, Daniel M. (June 1969), "Twelve Eclipsing Binaries with Double-Lined Spectra", Bulletin of the American Astronomical Society, 1: 257, Bibcode:1969BAAS....1R.257P.
  16. ↑ Liu, Quingyao; et al. (April 1996), "A H-alpha Flare on UV Piscium", Information Bulletin on Variable Stars, 4326: 1, Bibcode:1996IBVS.4326....1L.
  17. ↑ Qian, Shengbang; et al. (1999), "Orbital period studies of the RS CVn-type binaries. II. UV Piscium", Astrophysics and Space Science, 266 (4): 529–538, Bibcode:1999Ap&SS.266..529Q, doi:10.1023/A:1002030722350.

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