Iota Piscium
| |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| 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 |
| Distance | 44.73 ± 0.09 ly (13.71 ± 0.03 pc) |
| Absolute magnitude (MV) | 3.43[6] |
| Details | |
| Radius | 1.595±0.014[7] R☉ |
| Luminosity | 3.555±0.058[7] L☉ |
| Surface gravity (log g) | 4.11[8] cgs |
| Temperature | 6,288±37[7] K |
| Metallicity [Fe/H] | −0.12[8] dex |
| Rotational velocity (v sin i) | 6.67[9] km/s |
| Other designations | |
Iota Piscium (Iota Psc, ι Piscium, ι Psc) is an F-type main-sequence star 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 a suspected to be a variable star, and was once thought to have one or two stellar companions, but both are line-of-sight coincidences.[10]
Naming
In Chinese, 霹靂 (Pī Lì), meaning Thunderbolt, refers to an asterism consisting of refers to an asterism consisting of ι Piscium, β Piscium, γ Piscium, θ Piscium, and ω Piscium. Consequently, ι Piscium itself is known as 霹靂四 (Pī Lì sì, English: the Fourth Star of Thunderbolt.)[11]
References
- 1 2 "Simbad Query Result", Simbad Astronomical Object Database, retrieved April 4, 2007
- 1 2 3 4 5 6 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752
, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357 Vizier catalog entry - 1 2 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, Bibcode:2001AJ....121.2148G, doi:10.1086/319956.
- 1 2 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data (PDF), Bibcode:1986EgUBV........0M
- ↑ 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, Bibcode:2004PASA...21..129N, doi:10.1071/AS04013.
- ↑ Paunzen, E.; et al. (July 2014), "Investigating the possible connection between λ Bootis stars and intermediate Population II type stars", Astronomy & Astrophysics, 567: 8, arXiv:1406.3936, Bibcode:2014A&A...567A..67P, doi:10.1051/0004-6361/201423817, A67.
- 1 2 3 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, arXiv:1112.3316, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101. See Table 10.
- 1 2 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, arXiv:1301.1582, Bibcode:2013ApJ...764...78R, doi:10.1088/0004-637X/764/1/78
- ↑ 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, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725
- ↑ Kaler, James B., "Iota Piscium", Stars, University of Illinois, retrieved September 27, 2007
- ↑ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 8 日