Main sequence star in the constellation Perseus
Iota Persei
Location of ι Persei (circled)
Observation dataEpoch J2000 Equinox J2000
Constellation
Perseus
Right ascension
03 09 04.019
Declination
+49° 36′ 47.802″
Apparent magnitude (V)
4.062
Characteristics
Evolutionary stage
Main sequence
Spectral type
G0V or F9.5 V
U−B color index
+0.119
B−V color index
+0.595
Astrometry Radial velocity (Rv )49.47±0.12 km/s Proper motion (μ) RA: +1,265.475 mas /yr Dec.: −91.50 mas /yr Parallax (π)94.5412 ± 0.1448 mas Distance 34.50 ± 0.05 ly (10.58 ± 0.02 pc ) Absolute magnitude (MV )3.94
Details 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 +0.09 dex Rotational velocity (v sin i )4.1 km/s Age 3.2–4.1 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
Database references SIMBAD data
ι Persei , Latinized as Iota Persei , is a single 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. 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. Iota Persei has a relatively high proper motion across the sky.
ι Persei in optical light
This is a late F- or early G-type main-sequence star with a stellar classification of around G0V. It is about 3–4 billion years old and is spinning slowly with a projected rotational velocity of 4 km/s. 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.
There is a 12.4-magnitude line-of-sight companion star that is not believed to be gravitationally associated with Iota Persei. This object is located at an angular separation of 154.4″ from the primary along a position angle of 125°, as of 2014.
Naming
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).
References
^ 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 .
^ 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 .
^ 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 .
^ 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 at VizieR .
^ 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 .
^ 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 .
^ "iot Per" . SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-08-06.
^ 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 the Wayback Machine
External links
Categories :
Text is available under the Creative Commons Attribution-ShareAlike License. Additional terms may apply.
**DISCLAIMER** We are not affiliated with Wikipedia, and Cloudflare.
The information presented on this site is for general informational purposes only and does not constitute medical advice.
You should always have a personal consultation with a healthcare professional before making changes to your diet, medication, or exercise routine.
AI helps with the correspondence in our chat.
We participate in an affiliate program. If you buy something through a link, we may earn a commission 💕
↑