Main sequence star in the constellation Perseus
Iota Persei Location of ι Persei (circled)
Observation dataEpoch J2000 Equinox J2000 Constellation Perseus Right ascension 03h 09m 04.019s [ 1] Declination +49° 36′ 47.80″[ 1] Apparent magnitude (V)4.062[ 2] Characteristics Evolutionary stage Main sequence Spectral type G0V[ 3] [ 4] U−Bcolor index +0.119[ 2] B−Vcolor index +0.595[ 2] Astrometry Radial velocity (Rv )± 0.12[ 1] km/s Proper motion (μ)RA: +1,265.475mas /yr [ 1] Dec.: −91.50mas /yr [ 1] Parallax (π)94.5412± 0.1448 mas [ 1] Distance 34.50 ± 0.05 ly pc )[ 1] Absolute magnitude (MV )3.94[ 5] Details[ 6] Mass 1.08 – 1.1 M ☉ Radius 1.417 R ☉ Luminosity 2.22 L ☉ Surface gravity (log g )4.17 cgs Temperature 5,921 K Metallicity [Fe/H] +0.09 dex Rotational velocity (v sin i )4.1[ 7] Age 3.2–4.1[ 7] [ 8] Gyr Other designations ι Per ,BD +49°857FK5 112GC 3740GJ 124HD 19373HIP 14632HR 937SAO 38597PPM 45875CCDM J03091+4936AWDS J03091+4937A[ 9] Database references SIMBAD data
ι Persei ,Latinized asIota Persei , is a single[ 10] star in the northernconstellation Perseus . This object is visible to the naked eye as a faint, yellow-white hued point of light with anapparent visual magnitude of 4.1.[ 2] light years from the Sun based onparallax , and is drifting further away with aradial velocity of +49 km/s.[ 1] proper motion across the sky.[ 9]
ι Persei in optical light This is alate F- orearly G-type main-sequence star with astellar classification of around G0V.[ 3] [ 7] [ 8] projected rotational velocity of 4 km/s.[ 7] mass of the Sun and 1.4 times theSun's radius . It is radiating more than double theluminosity of the Sun from itsphotosphere at aneffective temperature of 5,921 K.[ 6]
There is a 12.4-magnitude line-of-sight companion star that is not believed to be gravitationally associated with Iota Persei.[ 10] angular separation of″ position angle of 125°, as of 2014.[ 11]
InChinese ,大陵 Dà Líng Mausoleum 9 Persei ,τ Persei ,κ Persei ,β Persei ,ρ Persei ,16 Persei and12 Persei . Consequently, theChinese name for ι Persei itself is大陵三 Dà Líng sān the Third Star of Mausoleum ).[ 12]
^a b c d e f g 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 atVizieR .^a b c d Jennens, P. A.; Helfer, H. L. (September 1975), "A new photometric metal abundance and luminosity calibration for field G and K giants",Monthly Notices of the Royal Astronomical Society 172 (3):667– 679,Bibcode :1975MNRAS.172..667J ,doi :10.1093/mnras/172.3.667 ^a b Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars",The Astrophysical Journal Supplement Series ,71 : 245,Bibcode :1989ApJS...71..245K ,doi :10.1086/191373 ^ Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample",The Astronomical Journal 132 (1):161– 170,arXiv :astro-ph/0603770 Bibcode :2006AJ....132..161G ,doi :10.1086/504637 ,S2CID 119476992 . ^ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics",Astronomy and Astrophysics ,501 (3):941– 947,arXiv :0811.3982 Bibcode :2009A&A...501..941H ,doi :10.1051/0004-6361/200811191 ,S2CID 118577511 . ^a b Soubiran, C.; Creevey, O. L.; Lagarde, N.; Brouillet, N.; Jofré, P.; Casamiquela, L.; Heiter, U.; Aguilera-Gómez, C.; Vitali, S.; Worley, C.; de Brito Silva, D. (2024-02-01)."Gaia FGK benchmark stars: Fundamental Teff and log g of the third version" .Astronomy and Astrophysics .682 : A145.arXiv :2310.11302 Bibcode :2024A&A...682A.145S .doi :10.1051/0004-6361/202347136 .ISSN 0004-6361 . Iota Persei's database entry atVizieR .^a b c d Valenti, Jeff A.; Fischer, Debra A. (July 2005)."Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs" .The Astrophysical Journal Supplement Series .159 (1):141– 166.Bibcode :2005ApJS..159..141V .doi :10.1086/430500 Note: see VizieR catalogieJ/ApJS/159/141 Archived 2016-08-06 at theWayback Machine .^a b Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics".The Astrophysical Journal .687 (2):1264– 1293.arXiv :0807.1686 Bibcode :2008ApJ...687.1264M .doi :10.1086/591785 .S2CID 27151456 . ^a b "iot Per" .SIMBAD Centre de données astronomiques de Strasbourg . Retrieved2019-08-06 .^a b 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 . ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog",The Astronomical Journal ,122 (6): 3466,Bibcode :2001AJ....122.3466M ,doi :10.1086/323920 ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日 Archived 2012-02-04 at theWayback Machine
