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Iota Persei

Coordinates: Sky map 03h 09m 04s, +49° 36′ 48″
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Iota Persei
Location of ι Persei (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 03h 09m 04.019s[1]
Declination +49° 36′ 47.802″[1]
Apparent magnitude (V) 4.062[2]
Characteristics
Evolutionary stage Main sequence
Spectral type G0V[3] or F9.5 V[4]
U−B color index +0.119[2]
B−V color index +0.595[2]
Astrometry
Radial velocity (Rv)49.47±0.12[1] km/s
Proper motion (μ) RA: +1,265.475 mas/yr[1]
Dec.: −91.50 mas/yr[1]
Parallax (π)94.5412 ± 0.1448 mas[1]
Distance34.50 ± 0.05 ly
(10.58 ± 0.02 pc)[1]
Absolute magnitude (MV)3.94[5]
Details[6]
Mass1.08 – 1.1 M☉
Radius1.417 R☉
Luminosity2.22 L☉
Surface gravity (log g)4.17 cgs
Temperature5,921 K
Metallicity [Fe/H]+0.09 dex
Rotational velocity (v sin i)4.1[7] km/s
Age3.2–4.1[7][8] Gyr
Other designations
ι Per, BD+49°857, FK5 112, GC 3740, HD 19373, HIP 14632, HR 937, SAO 38597, PPM 45875, CCDM J03091+4936A, WDS J03091+4937A[9]
Database references
SIMBADdata

ι Persei, Latinized as Iota Persei, is a single[10] star in the northern constellation Perseus. This object is visible to the naked eye as a faint, yellow-white hued point of light with an apparent visual magnitude of 4.1.[2] It is located 34.5 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +49 km/s.[1] Iota Persei has a relatively high proper motion across the sky.[9]

ι Persei in optical light

This is a late F- or early G-type main-sequence star with a stellar classification of around G0V.[3] It is about 3–4[7][8] billion years old and is spinning slowly with a projected rotational velocity of 4 km/s.[7] The star has 1.1 times the mass of the Sun and 1.4 times the Sun's radius. It is radiating more than double the luminosity of the Sun from its photosphere at an effective 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] This object is located at an angular separation of 154.4″ from the primary along a position angle of 125°, as of 2014.[11]

Naming

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In Chinese, 大陵 (Dà Líng), meaning Mausoleum, refers to an asterism consisting of ι Persei, 9 Persei, τ Persei, κ Persei, β Persei, ρ Persei, 16 Persei and 12 Persei. Consequently, the Chinese name for ι Persei itself is 大陵三 (Dà Líng sān, English: the Third Star of Mausoleum).[12]

References

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  1. ^ 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 at VizieR.
  2. ^ 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.
  3. ^ 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
  4. ^ 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.
  5. ^ 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.
  6. ^ 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. Bibcode:2024A&A...682A.145S. doi:10.1051/0004-6361/202347136. ISSN 0004-6361. Iota Persei's database entry at VizieR.
  7. ^ 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 catalogie J/ApJS/159/141 Archived 2016-08-06 at the Wayback Machine.
  8. ^ 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.
  9. ^ a b "iot Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-08-06.
  10. ^ 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.
  11. ^ Mason, B. D.; et al. (2014), The Washington Visual Double Star Catalog, Bibcode:2001AJ....122.3466M, doi:10.1086/323920
  12. ^ (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 the Wayback Machine
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