Iota Piscium
(Redirected from 17 Psc)
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| 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 | |
| Evolutionary stage | Main sequence |
| 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 mas[2] |
| 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 |
| Age | 5.2[10] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Iota Piscium (Iota Psc, ι Piscium, ι Psc) is a 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
[edit]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
[edit]- ^ a b "* iot Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved April 4, 2007.
- ^ a b c d e f 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, S2CID 18759600 Vizier catalog entry
- ^ a b 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.
- ^ a b Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, 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, arXiv:0811.3982, Bibcode:2004PASA...21..129N, doi:10.1071/AS04013, S2CID 123457673.
- ^ 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, S2CID 56332289, A67.
- ^ a b c 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, S2CID 18993744. See Table 10.
- ^ a b 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, S2CID 118751608
- ^ 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" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04
- ^ a b c 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, arXiv:1709.01655, Bibcode:2017A&A...608A.113N, doi:10.1051/0004-6361/201730859, S2CID 44229077
- ^ Kaler, James B., "Iota Piscium", Stars, University of Illinois, archived from the original on January 25, 2007, retrieved September 27, 2007
- ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 8 日 Archived 2012-04-15 at the Wayback Machine
