Iota Persei

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Iota Persei
Perseus constellation map visualization.PNG
Stars of Perseus
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 03h 09m 04.02s[1]
Declination +49° 36′ 47.8″[1]
Apparent magnitude (V) 4.05
Characteristics
Spectral type G0 V
U−B color index 0.12
B−V color index 0.60
Variable type None
Astrometry
Radial velocity (Rv) +50.0 km/s
Proper motion (μ) RA: +1262.41[1] mas/yr
Dec.: –91.50[1] mas/yr
Parallax (π) 94.87 ± 0.23[1] mas
Distance 34.38 ± 0.08 ly
(10.54 ± 0.03 pc)
Absolute magnitude (MV) 3.94
Details
Mass 1.35 ± 0.08[2] M
Radius 1.412 ± 0.009[3] R
Luminosity 2.181 ± 0.032[3] L
Surface gravity (log g) 4.31[2] cgs
Temperature 5,963 ± 5.1[4] K
Metallicity [Fe/H] +0.09[5] dex
Rotational velocity (v sin i) 4.1[2] km/s
Age 3.2–4.1[2][5] Gyr
Other designations
ι Persei, ι Per, Iota Per, BD+49°857, CCDM J03091+4936A, FK5 112, GC 3740, HD 19373, HIP 14632, HR 937, IDS 03018+4914 A, PPM 45875, SAO 38597, WDS J03091+4937A

Iota Persei (Iota Per, ι Persei, ι Per) is a main sequence dwarf star in the constellation Perseus. It is somewhat larger and greater in mass than the Sun, and is located about 34 light years distant. Iota Persei has a relatively high proper motion across the sky, and moves at a net velocity of 92 km/s, relative to the Sun.

No sub-stellar companions to this star have yet been found. There is a 12th-magnitude line-of-sight companion star that is not believed to be gravitationally associated with Iota Persei.

Naming[edit]

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, ι Persei itself is known as 大陵三 (Dà Líng sān, English: the Third Star of Mausoleum.).[6]

Cultural references[edit]

References[edit]

  1. ^ a b c d e 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
  2. ^ 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.
  3. ^ a b 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.
  4. ^ Kovtyukh, V. V. et al. (2003). "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios". Astronomy and Astrophysics 411 (3): 559–564. arXiv:astro-ph/0308429. Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378. 
  5. ^ 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. 
  6. ^ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日

External links[edit]