Nothing Special   »   [go: up one dir, main page]
Jump to content

30 Piscium

Coordinates: Sky map 00h 01m 57.6s, −06° 50′ 50.7″
From Wikipedia, the free encyclopedia
30 Piscium
Location of 30 (also called YY) Piscium (circled). It presents in a narrow triangle with two other stars of similar brightness, 27 and 33 Piscium.
Observation data
Epoch J2000      Equinox J2000
Constellation Pisces
Right ascension 00h 01m 57.61947s[1]
Declination −06° 00′ 50.6540″[1]
Apparent magnitude (V) 4.31 – 4.41[2]
Characteristics
Spectral type M3 III[3]
B−V color index 1.631±0.011[4]
Variable type LPV,[5] LB?[2]
Astrometry
Radial velocity (Rv)−11.7±0.5[6] km/s
Proper motion (μ) RA: 46.941 mas/yr[1]
Dec.: −40.471 mas/yr[1]
Parallax (π)7.8758 ± 0.4105 mas[1]
Distance410 ± 20 ly
(127 ± 7 pc)
Absolute magnitude (MV)−1.20[5]
Details
Radius109.2+5.46
−6.05[7] R☉
Luminosity1,597±177[7] L☉
Surface gravity (log g)2[8] cgs
Temperature3,490±35[7] K
Other designations
30 Psc, YY Psc, BD−06° 6345, FK5 1630, HD 224935, HIP 154, HR 9089, SAO 147042[9]
Database references
SIMBADdata

30 Piscium (HIP 154) is a solitary[10] variable star in the zodiac constellation of Pisces. It is visible to the naked eye with an apparent visual magnitude of 4.37.[8] Its calculated mid-value of antiposed parallax shift as the Earth moves around the Sun of very roughly 7.88 mas, makes it around 410 light years away.[1] Its net movement in the present epoch is one of moving closer – radial velocity (speed away from our star system) is −12 km/s.[6]

A visual band light curve for YY Piscium, plotted from data published by Tabur et al. (2009)[11]

This is an aging red giant star with a stellar classification of M3 III,[3] indicating it has exhausted the hydrogen at its core and evolved off the main sequence. It is a candidate long-period variable star[5] and has been given the designation YY Psc.[12] It varies in brightness between magnitudes 4.31 and 4.41 with no clear period. Possible periods of 23.1, 32.0, 53.6, and 167.8 days have been identified.[11] The star has 109 times the Sun's radius and is radiating 1,600 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 3,490 K.[7]

References

[edit]
  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b 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.
  3. ^ a b Keenan, P.; McNeil, R. (October 1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245–266, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
  4. ^ 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.
  5. ^ a b c Rimoldini, L.; et al. (December 2012), "Automated classification of Hipparcos unsolved variables", Monthly Notices of the Royal Astronomical Society, 427 (4): 2917–2937, arXiv:1301.1545, Bibcode:2012MNRAS.427.2917R, doi:10.1111/j.1365-2966.2012.21752.x, S2CID 119191320.
  6. ^ a b de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  7. ^ a b c d Baines, Ellyn K.; Thomas Armstrong, J.; Clark, James H.; Gorney, Jim; Hutter, Donald J.; Jorgensen, Anders M.; Kyte, Casey; Mozurkewich, David; Nisley, Ishara; Sanborn, Jason; Schmitt, Henrique R.; Van Belle, Gerard T. (2021). "Angular Diameters and Fundamental Parameters of Forty-four Stars from the Navy Precision Optical Interferometer". The Astronomical Journal. 162 (5): 198. arXiv:2211.09030. Bibcode:2021AJ....162..198B. doi:10.3847/1538-3881/ac2431.
  8. ^ a b Pérez Martínez, M. I.; et al. (November 2014), "The non-active stellar chromosphere: Ca II basal flux", Monthly Notices of the Royal Astronomical Society, 445 (1): 270–279, Bibcode:2014MNRAS.445..270P, doi:10.1093/mnras/stu1706.
  9. ^ "30 Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-03-10.
  10. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  11. ^ a b Tabur, V; Bedding, T. R; Kiss, L. L; Moon, T. T; Szeidl, B; Kjeldsen, H (2009). "Long-term photometry and periods for 261 nearby pulsating M giants". Monthly Notices of the Royal Astronomical Society. 400 (4): 1945. arXiv:0908.3228. Bibcode:2009MNRAS.400.1945T. doi:10.1111/j.1365-2966.2009.15588.x. S2CID 15358380.
  12. ^ Kukarkin, B. V.; et al. (January 1975), "60th Name-List of Variable Stars", Information Bulletin on Variable Stars, 961: 1, Bibcode:1975IBVS..961....1K.
Retrieved from "https://en.wikipedia.org/w/index.php?title=30_Piscium&oldid=1241650990"