UV Piscium – Wikipedia



UV Pisces is a binary famous person device within the constellation of Pisces. With a height obvious visible magnitude of 8.98,[2] it’s too faint to be visual to the bare eye. That is an eclipsing binary device that decreases to magnitude 10.05 right through the principle eclipse, then to magnitude 9.54 with the secondary eclipse. It’s positioned at a distance of 232 mild years from the Solar according to parallax measurements,[1] and is receding with a radial pace of 6.5 km/s.[5] The location of this famous person close to the ecliptic manner it’s topic to lunar occultation.[9]

This famous person was once discovered to be variable via H. Huth in 1959.[10] He decided it to be an eclipsing binary and revealed the morning time curve with a era of 20.67 hours. R. B. Carr in 1969 proposed this to be an Algol-type variable with a minor tidal distortion of the elements, plus a big, anomalous asymmetry within the mild curve.[11]D. S. Corridor in 1976 grouped it a few of the elegance of short-period RS CVn binaries.[12] The next 12 months, variable, non-thermal radio emission was once detected coming from the program, the primary such came upon for a short-period binary.[13]

Daniel M. Popper in 1969 discovered a double-lined, G-type spectrum with each elements appearing emission within the H and Okay traces.[14] In 1979, A. R. Sadik deduced the device is a indifferent binary and recommended a shiny, sizzling spot might produce the seen asymmetry within the mild curve. He discovered stellar classifications of G2V and K0IV for the principle and secondary elements, respectively.[11] With stepped forward spectra, Popper discovered leading collection categories of G5 and K3 for the 2 stars.[3] The presence of a prominence was once deduced in 1992, and a flare of hydrogen alpha was once seen the next 12 months.[15]

It is a shut binary device with an orbital era of 0.86 days. The orbit is round and the elements are spinning swiftly in-sync with their orbital era. This rotation price is making each stars magnetically energetic, with reasonable magnetic box strengths of 137 G and 88 G for the principle and secondary, respectively. Magnetic process cycles seem to be inflicting the orbital era to oscillate with a 61 12 months era.[16] The main is a G-type main-sequence famous person of about the similar dimension and mass because the Solar, whilst the secondary is a smaller Okay-type main-sequence famous person. They’re estimated to be about 4.6 billion years previous.[6]


  1. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). “Gaia Early Information Free up 3: Abstract of the contents and survey houses”. 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 document for this supply at VizieR.
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  3. ^ a b c d e f g Popper, Daniel M. (September 1997), “Orbits of indifferent main-sequence eclipsing binaries of varieties past due F to Okay. II. UV Leonis, UV Piscium, and BH Virginis”, The Astronomical Magazine, 114: 1195, Bibcode:1997AJ….114.1195P, doi:10.1086/118552.
  4. ^ Samus, N. N.; et al. (2017), “Common Catalogue of Variable Stars”, Astronomy Studies, 5.1, 61 (1): 80–88, Bibcode:2017ARep…61…80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  5. ^ a b Karataș, Yüksel; et al. (2004), “Kinematics of chromospherically energetic binaries and proof of an orbital era lower in binary evolution”, Per thirty days 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.
  6. ^ a b c Hahlin, A.; et al. (June 2021), “Magnetic box of the eclipsing binary UV Piscium”, Astronomy & Astrophysics, 650: 17, arXiv:2105.02542, Bibcode:2021A&A…650A.197H, doi:10.1051/0004-6361/202140832, A197.
  7. ^ Qian, S. -B.; et al. (March 2018), “Bodily Homes and Evolutionary States of EA-type Eclipsing Binaries Noticed via LAMOST”, The Astrophysical Magazine Complement Sequence, 235 (1): 12, arXiv:1712.09026, Bibcode:2018ApJS..235….5Q, doi:10.3847/1538-4365/aaa601, 5.
  8. ^ “UV Psc”. SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2022-07-08.
  9. ^ Herr, Richard B. (April 1969), “Identity Listing of Spectroscopic and Eclipsing Binaries Matter to Occultations via the Moon”, Publications of the Astronomical Society of the Pacific, 81 (479): 105, Bibcode:1969PASP…81..105H, doi:10.1086/128748.
  10. ^ Huth, H. (1959), Mitteilungen über Veränderliche Sterne, 424.
  11. ^ a b Sadik, A. R. (July 1979), “Mild and Color Curve Observations and Research of the Quick Length Eclipsing Binary Gadget UV Psc”, Astrophysics and House Science, 63 (2): 319–349, Bibcode:1979Ap&SS..63..319S, doi:10.1007/BF00638905.
  12. ^ Corridor, D. S. (1976), Fitch, W. S. (ed.), “The RS CVn Binaries and Binaries with Equivalent Homes”, A couple of Periodic Variable Stars, Complaints of IAU Colloq. 29, held in Budapest, Hungary, 1-5 September, 1975, D. Reidel Publishers, p. 287, Bibcode:1976ASSL…60..287H, doi:10.1007/978-94-010-1175-4_15.
  13. ^ Spangler, S. R.; et al. (December 1977), “Radio survey of shut binary stars”, Astronomical Magazine, 82: 989–997, Bibcode:1977AJ…..82..989S, doi:10.1086/112161.
  14. ^ Popper, Daniel M. (June 1969), “Twelve Eclipsing Binaries with Double-Covered Spectra”, Bulletin of the American Astronomical Society, 1: 257, Bibcode:1969BAAS….1R.257P.
  15. ^ Liu, Quingyao; et al. (April 1996), “A H-alpha Flare on UV Piscium”, Knowledge Bulletin on Variable Stars, 4326: 1, Bibcode:1996IBVS.4326….1L.
  16. ^ Qian, Shengbang; et al. (1999), “Orbital era research of the RS CVn-type binaries. II. UV Piscium”, Astrophysics and House Science, 266: 529–538, Bibcode:1999Ap&SS.266..529Q, doi:10.1023/A:1002030722350.

Additional studying[edit]

  • Kjurkchieva, Diana P.; et al. (February 2005), “Spectroscopic and Photometric Observations of the Quick-Length RS CVn-Kind Celebrity UV Piscium”, The Astronomical Magazine, 129 (2): 1084–1095, Bibcode:2005AJ….129.1084K, doi:10.1086/427396.
  • Lastennet, E.; et al. (October 2003), “Disentangling discrepancies between stellar evolution principle and sub-solar mass stars. The affect of the blending duration parameter for the UV Psc binary”, Astronomy and Astrophysics, 409: 611–618, arXiv:astro-ph/0307360, Bibcode:2003A&A…409..611L, doi:10.1051/0004-6361:20031114.
  • Vivekananda Rao, P.; Radhika, P. (2002), “Lengthy-Time period Find out about of the Starspot Process at the Eclipsing Quick-Length RS Canum Venaticorum Celebrity UV Piscium”, Astrophysics and House Science, 282 (1): 103–120, Bibcode:2002Ap&SS.282..103V, doi:10.1023/A:1021194218533.
  • Sowell, James R.; et al. (October 2001), “Length Adjustments in 4 Quick-Length Noticed Binaries: UV Piscium, YY Geminorum, CG Cygni, and XY Ursae Majoris”, The Astronomical Magazine, 122 (4): 1965–1973, Bibcode:2001AJ….122.1965S, doi:10.1086/323091.
  • Radhika, P.; Vivekananda Rao, P. (September 2001), “Lengthy-term find out about of the starspot process at the eclipsing short-period RS Canum Venaticorum binary UV Piscium”, Bulletin of the Astronomical Society of India, 29: 317–322, Bibcode:2001BASI…29..317R.
  • Qian, S. B. (2001), Brekke, Pål; et al. (eds.), “Imaginable Magnetic Process Cycles of 4 Chromospherically Energetic Binaries: ER Vul, UV Psc, AR Lac and BH Vir”, Contemporary Insights into the Physics of the Solar and Heliosphere: Highlights from SOHO and Different House Missions, Complaints of IAU Symposium 203, Astronomical Society of the Pacific, p. 437, Bibcode:2001IAUS..203..437Q, ISBN 1-58381-069-2.
  • Hughes, S. B.; et al. (December 2000), “An Investigation of Length Adjustments for 4 RS CVn Stars: UV Psc, YY Gem, CG Cyg, and XY UMa”, American Astronomical Society, 197th AAS Assembly, identification.46.17; Bulletin of the American Astronomical Society, vol. 32, p. 1479, Bibcode:2000AAS…197.4617H.
  • Heckert, Paul A. (November 1999), “1998 Photometry of UV Piscium”, Knowledge Bulletin on Variable Stars, 4806: 1, Bibcode:1999IBVS.4806….1H.
  • Frederik, Marina C.; Etzel, Paul B. (Might 1996), “A Photometric Research and SPOT Fashion of the Indifferent Eclipsing Binary UV Leonis”, Astronomical Magazine, 111: 2081, Bibcode:1996AJ….111.2081F, doi:10.1086/117944.
  • Jassur, D. M. Z.; Kermani, M. H. (September 1994), “1992 UBV Observations of UV PISCIUM and Mild Curve Research”, Astrophysics and House Science, 219 (1): 35–47, Bibcode:1994Ap&SS.219…35J, doi:10.1007/BF00657858.
  • Jassur, D. M. Z.; Kermani, M. H. (June 1993), “UBV Photoelectric Observations of UV Piscium”, Knowledge Bulletin on Variable Stars, 3896: 1, Bibcode:1993IBVS.3896….1J.
  • Popper, Daniel M. (August 1991), “Orbits of Shut Binaries With CA II H and Okay in Emission. V. the Primary-Collection Gadget UV Piscium”, Astronomical Magazine, 102: 699, Bibcode:1991AJ….102..699P, doi:10.1086/115904.
  • Han, Gained-Yong; Kim, Tu-Hwan (August 1988), “A Photometric Find out about of UV Piscium”, Publications of the Astronomical Society of the Pacific, 100: 964, Bibcode:1988PASP..100..964H, doi:10.1086/132258.
  • Akan, M. Can (April 1988), “Two-colour photoelectric photometry of UV PISCIUM and Fourier research of its out-of-eclipse mild diversifications”, Astrophysics and House Science, 143: 367–376, Bibcode:1988Ap&SS.143..367A.
  • Ibanoglu, C. (December 1987), “The sunshine curve diversifications in UV Piscium”, Astrophysics and House Science, 139 (1): 139–147, Bibcode:1987Ap&SS.139..139I, doi:10.1007/BF00643819.
  • Busso, M.; et al. (September 1987), “A seek for non-stellar contributions to the optical and near-IR flux of RS CVn binaries. I. The circumstances of TY Pyx, UV Psc, RU CNC and VV Mon”, Astronomy and Astrophysics, 183: 83–90, Bibcode:1987A&A…183…83B.
  • Keskin, V.; et al. (August 1987), “The 1986 Mild Curves of UV Piscium”, Knowledge Bulletin on Variable Stars, 3060: 1, Bibcode:1987IBVS.3060….1K.
  • Antonopoulou, E. (July 1987), “Infrared Photometry of UV-Piscium”, Astrophysics and House Science, 135 (2): 335–345, Bibcode:1987Ap&SS.135..335A, doi:10.1007/BF00641569.
  • Busso, M.; et al. (February 1986), “Differential rotation and process cycles in RS CVn binaries. III. UV Piscium and UX Arietis”, Astronomy and Astrophysics, 156, : 106–110, Bibcode:1986A&A…156..106B.{{quotation}}: CS1 maint: additional punctuation (hyperlink)
  • Barden, S. C. (March 1984), “The Hα Nature of the Quick Length RS CVn Techniques HD86590, σ2Cr B, ER Vul and UV Psc”, Bulletin of the American Astronomical Society, 16: 473, Bibcode:1984BAAS…16..473B.
  • Vivekananda Rao, P.; Sarma, B. Okay. (February 1984), Hidayat, Bambang; et al. (eds.), “Photometry of the RS-Canum Kind Eclipsing Binary UV-Piscium”, Double Stars, Bodily Homes and Generic Family members. Complaints of IAU Colloquium No. 80, held at Lembang, Java, June 3-7, 1983, Dordrecht, Holland; Boston: D. Reidel Publishing Corporate, p. 239, Bibcode:1984Ap&SS..99..239V, doi:10.1007/BF00650248.{{quotation}}: CS1 maint: date and 12 months (hyperlink)
  • Rao, P. V.; Sarma, M. B. Okay. (September 1983), “The distortion wave at the mild curve of the RS CVn binary UV Piscium.”, Magazine of Astrophysics and Astronomy, 4: 161–169, Bibcode:1983JApA….4..161R, doi:10.1007/BF02714902.
  • Antonopoulou, E. (September 1983), “Infrared photometry of the RS CVn binaries. III. JHK mild curves of UV Psc”, Astronomy and Astrophysics, Complement Sequence, 53: 347–349, Bibcode:1983A&AS…53..347A.
  • Zeilik, M.; et al. (February 1982), “1981 UBVR Photometry of UV Psc”, Knowledge Bulletin on Variable Stars, 2089: 1, Bibcode:1982IBVS.2089….1Z.
  • Aslan, Z. (December 1978), “Photoelectric Occasions of Minima and the Length of UV Psc”, Knowledge Bulletin on Variable Stars, 1511: 1, Bibcode:1978IBVS.1511….1A.
  • Al-Naimiy, H.; et al. (April 1978), “Observations of UV Psc and XY Cet”, Knowledge Bulletin on Variable Stars, 1415: 1, Bibcode:1978IBVS.1415….1A.
  • Sadik, A. R. (January 1978), “UV Psc – a Quick Length RS CVn Celebrity”, Knowledge Bulletin on Variable Stars, 1381: 1, Bibcode:1978IBVS.1381….1S.


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