Astronomy:Iota Piscium

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Short description: F-type main sequence star in the constellation Pisces
Iota Piscium[1]
Diagram showing star positions and boundaries of the Pisces constellation and its surroundings
Cercle rouge 100%.svg
Location of ι Piscium(circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Pisces
Right ascension  23h 39m 57.04138s[2]
Declination +05° 37′ 34.6475″[2]
Apparent magnitude (V) 4.13[3]
Characteristics
Spectral type F7 V[3]
U−B color index −0.01[4]
B−V color index +0.50[4]
Astrometry
Radial velocity (Rv)+5.4[5] km/s
Proper motion (μ) RA: 377.15±0.19[2] mas/yr
Dec.: −437.43±0.15[2] mas/yr
Parallax (π)72.92 ± 0.15[2] mas
Distance44.73 ± 0.09 ly
(13.71 ± 0.03 pc)
Absolute magnitude (MV)3.43[6]
Details
Radius1.595±0.014[7] R☉
Luminosity3.555±0.058[7] L☉
Surface gravity (log g)4.11[8] cgs
Temperature6,288±37[7] K
Metallicity [Fe/H]−0.12[8] dex
Rotational velocity (v sin i)6.67[9] km/s
Age5.2[10] Gyr
Other designations
ι Piscium, ι Psc, Iota Psc, 17 Piscium, BD+04°5035, CCDM J23399+0538A, FK5 892, GC 32879, HD 222368, HIP 116771, HR 8969, IDS 23348+0505 A, PPM 174312, SAO 128310, WDS J23399+0538A[1]
Database references
SIMBADdata

Iota Piscium (Iota Psc, ι Piscium, ι Psc) is single,[10] F-type main-sequence star located 45 light years from Earth,[2] in the constellation Pisces. Its spectral type is F7V, which means that it is somewhat larger and brighter than the Sun, but still within the range considered to have the potential for Earth-like planets. It has a surface temperature of about 6,000 to 7,500 K. Iota Piscium is suspected to be a variable star, and was once thought to have one or two stellar companions, but both are line-of-sight coincidences.[11] It displays a far-infrared excess at a wavelength of 70μm, suggesting it is being orbited by a cold debris disk.[10]

Naming

In Chinese, 霹靂 (Pī Lì), meaning Thunderbolt, refers to an asterism consisting of ι Piscium, β Piscium, γ Piscium, θ Piscium, and ω Piscium. Consequently, the Chinese name for ι Piscium itself is 霹靂四 (Pī Lì sì, English: the Fourth Star of Thunderbolt.)[12]

References

  1. ↑ 1.0 1.1 "* iot Psc". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+iot+Psc. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V  Vizier catalog entry
  3. ↑ 3.0 3.1 Gray, R. O.; Napier, M. G.; Winkler, L. I. (April 2001), "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars", The Astronomical Journal 121 (4): 2148–2158, doi:10.1086/319956, Bibcode: 2001AJ....121.2148G. 
  4. ↑ 4.0 4.1 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, Bibcode: 1986EgUBV........0M 
  5. ↑ Nordström, Andersen et al. (2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14000 F and G dwarfs", Publications of the Astronomical Society of Australia 21 (2): 129–133, doi:10.1071/AS04013, Bibcode: 2004PASA...21..129N. 
  6. ↑ Paunzen, E. et al. (July 2014), "Investigating the possible connection between λ Bootis stars and intermediate Population II type stars", Astronomy & Astrophysics 567: 8, doi:10.1051/0004-6361/201423817, A67, Bibcode: 2014A&A...567A..67P. 
  7. ↑ 7.0 7.1 7.2 Boyajian, Tabetha S. et al. (February 2012), "Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars", The Astrophysical Journal 746 (1): 101, doi:10.1088/0004-637X/746/1/101, Bibcode: 2012ApJ...746..101B . See Table 10.
  8. ↑ 8.0 8.1 Ramírez, I. et al. (February 2013), "Oxygen abundances in nearby FGK stars and the galactic chemical evolution of the local disk and halo", The Astrophysical Journal 764 (1): 78, doi:10.1088/0004-637X/764/1/78, Bibcode: 2013ApJ...764...78R 
  9. ↑ 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", Astronomy and Astrophysics 520: A79, doi:10.1051/0004-6361/200913725, Bibcode: 2010A&A...520A..79M, http://eprints.ucm.es/37826/1/davidmontes17libre.pdf, retrieved 2018-11-04 
  10. ↑ 10.0 10.1 10.2 Nuñez, Paul D. et al. (September 2017). "A near-infrared interferometric survey of debris-disk stars. VI. Extending the exozodiacal light survey with CHARA/JouFLU". Astronomy & Astrophysics 608 (113): A113. doi:10.1051/0004-6361/201730859. Bibcode: 2017A&A...608A.113N. 
  11. ↑ Kaler, James B., "Iota Piscium", Stars (University of Illinois), http://www.astro.uiuc.edu/~kaler/sow/iotapsc.html, retrieved September 27, 2007 
  12. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 8 日



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